Index: /Backup NB/Talks/MEMPHYSetal/BENE2005AnnualReport/MEMPHYS.tex
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--- /Backup NB/Talks/MEMPHYSetal/BENE2005AnnualReport/MEMPHYS.tex	(revision 385)
+++ /Backup NB/Talks/MEMPHYSetal/BENE2005AnnualReport/MEMPHYS.tex	(revision 385)
@@ -0,0 +1,14 @@
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{The MEMPHYS detector}
+%to describe the signal efficiency/background/systematics
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+The MEMPHYS (MEgaton Mass Physiscs) detector is a Megaton-class water \{C}erenkov in the straight extrapolation of the well known and robust technique used for the SuperKamiokande detector. It is located at Fréjus, so 130~km from CERN and it is an alternative design of the UNO \cite{UNO} and HyperKamiokande \cite{HyperK} detectors and shares the same physics case both from Non Accelerator domain (Nucleon Decay, Super Novae Neutrino from burst event or from Relic explosion, Solar \& Atmospheric Neutrinos) and from Accelerator (Super Beam, Beta Beam) domain. For the physics part not covered by this document, this kind of megaton Water detector can push the Nucleon decay search up to $10^{35}$~yrs in the $e^+\pi^0$ channel  and up to few $10^{34}$~yrs in the $K^+\bar{nu}$ channel, just to cite these benchmark channels. MEMPHYS can register as many as 150,000 events from a SN at 10~kpc from our galaxy and 50~events or so form Andromeda. To detect Relic Neutrinos from past Super Novae explosion one can use pure water and get a flux of 250~evts/10~y/500kT or increase this number by a factor 10 by adding Gadolinium salt.
+
+A recent civil engineering pre-study to envisage the possibly of large cavity excavation located under the Fréjus mountain (4800~m.e.w) near the present Modane Underground Laboratory has been undertaken. The main result of this pre-study is that MEMPHYS may be build with present techniques as 3 or 4 shafts modular detector, $250,000~\mathrm{m}^3$ each with 65~m in diameter, 65~m in height for the total water containment. Each of these shafts correspond to about $5$ times the present SuperKamiokande cavity. For the present physical study, we have chosen on a fiducial volume of 440~kT which means 3 shafts and an Inner Detector (ID) of 57~m in diameter and 57~m in height. Each ID may be equipped with photodetectors (PMT, HPD,...) with a surface coverage at least 30\%. The Fréjus site 4800~m.w.e offers a natural protection against cosmic rays by a factor $10^6$.
+\begin{figure}
+\centering
+\includegraphics[width=0.45\textwidth]{MEMPHYS.eps}
+\caption{\label{fig:MEMPHYS}Sketch of the MEMPHYS detector under the Fréjus mountain.}	
+\end{figure}
+
+The decision for cavity digging is fixed at 2010 after an intense Detector Design Study (eg. cavity excavation, vephotodetector R\&D) performed in parallel of the digging of at least a Safety Galery in the Fréjus road tunnel. One may notes that this key date may also decisive for SPL construction as well as the choice of the EURISOL site. After that, the excavation and PMT production are envisaged to take seven years or so, and the Non accelerator program can start before the rise up of the accelerator program (Super Beam and Beta Beam) which may start before 2020.     
Index: /Backup NB/Talks/MEMPHYSetal/BENE2005AnnualReport/SPL.tex
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--- /Backup NB/Talks/MEMPHYSetal/BENE2005AnnualReport/SPL.tex	(revision 385)
+++ /Backup NB/Talks/MEMPHYSetal/BENE2005AnnualReport/SPL.tex	(revision 385)
@@ -0,0 +1,138 @@
+% --------------------------
+\subsection{SPL SuperBeam}
+% --------------------------
+%In  the CERN-SPL SuperBeam project  \cite{SPL,SPL-Physics,nufact1}
+% the planned 4MW SPL (Superconducting Proton Linac)  would deliver a 2.2  GeV/c
+% proton beam,  on a Hg target to generate
+% an intense $\pi^+$ ($\pi^-$) beam focused by a suitable
+% magnetic horn in a short decay tunnel. As a result   an intense
+% $\nu_{\mu}$ beam, will be produced
+% mainly via the $\pi$-decay,  $\pi^+ \rightarrow \nu_{\mu} \; \mu^+$ providing a
+% flux $\phi \sim 3.6 {\cdot} 10^{11} \nu_{\mu}$/year/m$^2$  at 130 Km
+% of distance, and an average energy of 0.27 GeV.
+% The $\nu_e$ contamination from $K$ will be suppressed by threshold effects
+% and the resulting $\nu_e/\nu_{\mu}$ ratio ($ \sim 0.4 \%$) 
+%  will be known within  $2\%$ error.
+% The use of a near and far detector (the latter at $L = 130$ Km of distance
+% in the Frejus area \cite{Mosca})
+% will allow for both $\nu_{\mu}$-disappearance and
+% $\nu_{\mu} \rightarrow \nu_e$ appearance studies.
+% The physics potential of the 2.2 GeV SPL SuperBeam (SPL-SB)
+% with a water Cerenkov far detector fiducial mass of 440 Kt \cite{UNO}  has been extensively
+% studied \cite{SPL-Physics}. \\
+%
+% New developments show that the potential of the SPL-SB potential could be
+% improved by rising the SPL energy to 3.5 GeV \cite{Cazes},
+% to produce   more copious secondary mesons
+% and to focus them more efficiently. This seems feasible if
+% status of the art RF cavities would be used in place of the old foreseen LEP cavities
+% \cite{Garoby-SPL}.
+% In this upgraded configuration neutrino flux could be increased by a factor 3 with
+% with respect to the 2.2 GeV configuration, reaching
+% a sensitivity to $\sin^2{2 \thetaot}$ 8 times better than T2K and allowing
+% to discovery CP violation (at 3 $\sigma$ level) if
+% $\delCP \geq 25^\circ$  and
+% $\theta_{13} \geq 1.4^\circ$ \cite{MMNufact04}. The expected
+% performances are shown in Fig.~\ref{fig:th13}.
+%
+% \begin{figure}
+%  \centerline{\epsfig{file=show_fluxes_new.eps,width=0.5\textwidth}}
+%  \mycaption{Neutrino flux of $\beta$-Beam ($\gamma=100$)
+%   and CERN-SPL SuperBeam, 3.5 GeV, at 130 Km of distance.}
+%  \label{fig:fluxes}
+% \end{figure}
+
+An optimization of the energy as well as the secondary particle focusing and decay tunnel has been undertaken in the context of a Super Beam of 4~MW \cite{JECACLAL} using the CERN-SPL \cite{SPL} and searching for $\nu_\mu \rightarrow \nu_e$ ($\bar{\nu}_\mu \rightarrow \bar{\nu}_e$) appearance channels in an 500~kT  fiducial volume water Cerenkov detector, called MEMPHYS, and located in an possible new underground laboratory at the Fréjus tunnel, 130~km from the CERN complex. The use of a near detector will also enable the use of the disappearance channels. 
+
+The secondary particles from the interaction of proton beam impinging a 30~cm long 1.5~cm diameter mercury target, have been obtained with the FLUKA generator (see Tab.~\ref{tab:nbPart}). At kinetic energy of 3.5 (2.2)~GeV, the number of p.o.t per year is 0.69 (1.10) $10^{23}$ while the numbers of $\pi^+/\pi^-/K^+/K^o$ per p.o.t are $0.41/0.37/35 10^{-4}/30 10^{-4}$ ($0.24/0.18/7 10^{-4}/6 10^{-4}$). At higher beam energy, the kaon rates grow rapidly compared to the pion rates, and needless to emphasize the need of an experimental confirmation \cite{HARP,MINERVA} of such numbers.
+
+The focusing system (magnetic horns) optimized in the context of a Neutrino Factory \cite{SIMONE1,DONEGA} has been redesigned considering the specific requirements of a Super Beam. The most important points are the phase spaces that are covered by the two types of horns are different, and that for a Super Beam the pions to be focused should have an energy of the order of $p_\pi (\mathrm{MeV})/3 \approx E_\nu \gtrsim  2L(\mathrm{km})$ to obtain a maximum oscillation probability. In practice, this means that one should collect $800$~MeV/c pions to get a mean neutrino energy of $300$~MeV.
+
+\begin{table}
+\centering
+\caption{\label{tab:nbPart}Average numbers of the most relevant secondary particles exiting the $30$~cm long, $1.5$~cm diameter mercury target per incident proton (FLUKA).}
+\begin{tabular}{@{}l*{15}{l}}
+\hline\noalign{\smallskip}
+$E_k$ (GeV) &     p.o.t/y        & $\pi^+$ & $\pi^-$ & $K^+$ & $K^0$ \\
+            & $\times 10^{23}$ &         &         & \multicolumn{2}{c}{$\times 10^{-4}$} \\
+\noalign{\smallskip}\hline\noalign{\smallskip}
+$2.2$ & $1.10$  &  $0.24$   &  $0.18$ &   $7$ &   $6$ \\
+$3.5$ & $0.69$  &  $0.41$   &  $0.37$ &  $35$ &  $30$ \\
+$4.5$ & $0.54$  &  $0.57$   &  $0.39$ &  $93$ &  $68$ \\
+$8.0$ & $0.30$  &  $1.00$   &  $0.85$ & $413$ & $340$ \\
+ \noalign{\smallskip}\hline
+\end{tabular}
+\end{table}
+
+The resulting fluxes for the positive ($\nu_\mu$ beam) and the negative focusing ($\bar{\nu}_\mu$ beam) are show on figure \ref{fig:fluxComparison}. The total number of $\nu_\mu$ ($\bar{\nu}_\mu$) in positive (negative) focusing is about $1.18 (0.97) 10^{12}/\mathrm{m}^2/\mathrm{yr}$ with an average energy of $300$~MeV. The $\nu_e$ ($\bar{\nu}_\mu$) contamination in the $\nu_\mu$ beam is around $0.7\%$ ($6.0\%$) 
+  and will be known within  $2\%$ error. Compared to  the fluxes used in references \cite{MEZZETTONF02,DONINI04} the gain is at least a factor $2.5$. Using neutrino cross-sections on water \cite{LIPARIxsec}, the number of expected $\nu_\mu$ charged current is about $95$ per kT.yr.
+%
+\begin{figure}
+\centering
+\includegraphics[height=60mm]{OptiVsOldFlux.eps}
+\caption{\label{fig:fluxComparison}The $\nu_\mu$ and the $\bar{\nu}_\mu$ fluxes obtained by optimizing the SPL for a Super Beam case ("SB Opt.") are compared to those obtained with a focusing system designed for a Neutrino Factory ("NF Opt.").}
+\end{figure}
+
+The physics potential of the new optimized SPL may be determined using GLoBES software \cite{GLOBES}. Both the appearance and the disappearance channels have been used, and also five bins of 200~MeV each have been introduced. The $\pi^o$ background have been rejected using a tighter PID cut compared to standard SuperK analysis \cite{MEZZETTONF02}. The Michel electron has been required for the $\mu$ identification. As ultimate goal suggested by \cite{T2K} a 2\% systematical error is used both for signal and background.
+
+The $90\%$ CL sensitivity contour in the ($\Delta m^2_{31}$,$\sin^22\theta_{13}$) plane after 5 years running with a positive focusing is shown on figure \ref{fig:SPLDmTheta13Comparison}. With the new optimized setup, one expects to reach a limit on $\theta_{13}$ of $0.7^o$.
+%
+\begin{figure}
+\centering
+\includegraphics[height=60mm]{compareOldNewthetaDm.eps}
+\caption{\label{fig:SPLDmTheta13Comparison}Comparison of the sensitivity contours with the new optimized setup and the original SPL design after 5 years of running with positive focusing.}
+\end{figure}
+%
+One may also appreciate on figure \ref{fig:SPLCPSensi} the improvement on the combined sensitivity of $\sin^22\theta_{13}$ and $\delta_{CP}$ with the new optimization compared for instance to the T2K project \cite{T2K}. 
+%  
+\begin{figure}
+\centering
+\includegraphics[height=60mm]{deltaThetaSens5yOldNew.eps}
+\caption{\label{fig:SPLCPSensi}Comparison of the sensitivity on combined $\theta_{13}$ and $\delta_{CP}$ after 5 years of positive focusing. The T2K sensitivity contour has been derived from  reference \cite{T2K}. No mass hierarchy nor octant hierarchy ambiguity has been considered.}
+\end{figure}
+%
+
+So, the optimized SPL beam line operating a Super Beam towards a megaton scale detector (called MEMPHYS) at the Fréjus tunnel has a great potential.
+
+
+%%%%%%%%%%%%%%%%%%%% SPL Bibliography %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\bibitem{JECACLAL}
+J.E Campagne and A. Cazes, LAL-04-102, arXiv:hep-ex/405002 submitted to \EJP
+
+\bibitem{SPL}
+SPL Conceptual Design, CERN 2000-012
+
+\bibitem{HARP}
+C. Catanesi \etal, CERN-SPSC 2002/019
+
+\bibitem{MINERVA} 
+D. Drakoulakos \etal, Fermilab P-938, arXiv:hep-ex/405002
+
+\bibitem{SIMONE1}
+S.~Gilardoni \etal, AIP Conf.\ Proc.\  {\bf 721} (2004) 334.
+
+\bibitem{DONEGA}
+A. Blondel \etal, CERN-NUFACT-Note-78 (2001)
+ 
+\bibitem{MEZZETTONF02}
+M. Mezzetto,  \jpg {\bf 29}, 1781-1784 (2003), arXiv:hep-ex/0302005
+
+\bibitem{DONINI04}
+A. Donini \etal, IFT-UAM/CSIC-04-30  (2004), arXiv:hep-ph/0406132
+ 
+\bibitem{LIPARIxsec}
+P.~Lipari, M.~Lusignoli and F.~Sartogo,
+  %``The Neutrino cross-section and upward going muons,''
+  \PRL {\bf 74} (1995) 4384, arXiv:hep-ph/9411341
+
+\bibitem{GLOBES}
+P. Hubert, M. Lindner and W. Winter, arXiv:hep-ph/0407333,
+Comput.Phys.Commun. 167 (2005) 195. 
+
+\bibitem{T2K}
+T. Kobayashi, \NP B  143  (Proc. Supp.) (2005) 303
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
Index: /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-13mar07/tt.tar/referee.txt
===================================================================
--- /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-13mar07/tt.tar/referee.txt	(revision 385)
+++ /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-13mar07/tt.tar/referee.txt	(revision 385)
@@ -0,0 +1,176 @@
+
+Authors: J.E.Campagne,M.Maltoni,M.Mezzetto,T.Schwetz 
+
+Title: Physics potential of the CERN-MEMPHYS neutrino oscillation project 
+
+
+We thank the referee for his/her positive evaluation or our work, the
+detailed reading of the manuscript, and the critical comments. Below
+we answer to the criticisms, and list the corresponding changes in the
+text. We hope that with these changes our work is suitable for
+publication.
+
+
+REFEREE: (1) One of the most surprising feature of the results
+obtained in this paper is that the mass hierarchy can be resolved up
+to sin22theta13 =0.03 just by combining SPL and
+betabeam(Fig.16). However, the authors seem to fail to place enough
+emphasis on this unexpected result. I understood that some explanation
+is already offered by the authors in page 25. What are the key
+experimental features which enable the resolution?
+
+ANSWER: As we explain on p. 26 (previously p. 25), this interesting
+effect appears because of a delicate interplay of the (tiny) matter
+effect in all four CP and T conjugate channels. This can also be seen
+from Fig. 5, where the solutions with the wrong hierarchy appear at
+slightly different locations for BB and SPL. We belief that the
+explanation given on p. 26 is clear enough. A more detailed
+investigation of this effect goes beyond the scope of the paper.
+
+
+
+REFEREE: (2)The authors view of the current status of the ideas for
+future projects seems to be a bit outdated. Now another option of T2K
+upgrade, which is called as T2KK, is available. In this option people
+claimed that all the eight-fold parameter degeneracy can be lifted in
+situ without relying on combination with atmospheric neutrinos,
+thereby reserving the latter as a redundant cross check. Also they use
+superbeam only, avoiding a costly beta beam construction. From
+outsiders view it looks like the better option within the scope of
+megaton class water Cherenkov than CERN-MEMPHYS. Even though the
+authors do not fully treat the T2KK setting in their analysis, it
+would be nice if the authors comments on comparison between these two
+strategies.
+
+ANSWER: In our work we have confined ourselves to the standard T2HK
+setup, since the porpose of our work is not a T2K optimization study
+investigating various configurations for that experiment. In contrast,
+here T2HK mainly serves as a point of reference to which we compare
+the CERN--MEMPHYS experiments. For this aim we prefer to stick to the
+``minimal'' one-detector configuration at a relatively short baseline,
+since two-detector setups with very long baselines clearly represent a
+different class of experiments whose consideration goes beyond the
+scope of the present work. We have added a paragraph to say this
+explicitly on p. 4. 
+
+Moreover, we have added at several places in the text comments on the
+sensitivities of T2KK obtained in Refs. [34,35], which are the
+previous Ref. [60] and the more recent T2KK publication which we have
+added to the references. Specifically, we comment on T2KK on p. 22
+(CPV), on p. 26 (mass hierarchy) and on p. 27 (octant degeneracy). In
+addition we mention also the the wide band beam idea in relation to
+the mass hierarchy deterimation, referring to the analysis [74].
+
+
+
+REFEREE: (3)The most serious problem in appearance neutrino experiment
+with water Cherenkov detector is the background issue, in particular
+pi0 rejection.  While the authors refer Ref. [51] for 'tighter cut'
+the reference is not informative at all. Also, one of the advantage of
+the present analysis, as compared to theprevious SPL studies, is that the
+authors take into account the spectrum informations. But, at such low
+energies it is highly nontrivial to reconstruct neutrino energy
+because of Fermi motion. The authors description of the procedure is
+too brief to allow understanding such high performance of the
+method. The reasonably informative description should be provided
+for both aspects.
+
+ANSWER: We quoted reference [53] (previous [51]) because it's the only
+paper where the SPL analysis has been described. It had been performed
+by D. Casper from the SuperKamiokande collaboration. We don't have
+today all the details of this analysis, but the pi0 background can be
+understood from general principles. We have added the following text
+in sec. 3.3:
+
+"Following Ref. [53], the $\pi^o$ background is reduced using a tighter
+PID cut compared to the standard Super-Kamiokande analysis used in
+K2K, but the cuts are looser than for T2K. Indeed, at SPL energies the
+$\pi^o$ background is less severe than for T2HK. This is because the
+resonant cross section is suppressed, and the produced pions have an
+energy where the angle between the two gammas is very wide, leading to
+a small probability that the two gamma rings overlap. This results in
+a higher signal efficiency of SPL compared to T2HK (60\% against 40\%)
+and a smaller rate of $\pi^o$ background."
+
+
+Regarding the energy reconstruction, we think to have fully
+illustrated the problem with Figure 2 and the related discussion in
+sec. 3.2. We are using the same lepton momentum smearing function as
+SK and we are using the most updated version of the Nuance neutrino
+generator, that is worldwide considered the reference for neutrino
+generators, and Fermi motion is taken into account. In ref. [34]
+(previous [60]) the authors quote an energy resolution of 80 MeV for
+QE events. By applying our methods we have 77 MeV resolution in their
+energy range.
+
+
+
+REFEREE: (4)The Dm2 sensitivity of T2HK as presented in Table 4
+appears too good to be true. It is strongly believed that it cannot be
+less than 2
+
+ANSWER: We have added the following text to the discussion of Tab. 4:
+
+"In the interpretation of the numbers given in Tab. 4 one should
+consider that at accuracies below 1\% systematics might become
+important, which are not accounted for here. We do include the most
+relevant systematics (see Secs. 2 and 3), however, at that level
+additional uncertainties related to, for example, the spectral shapes
+of signal and/or background, or the energy calibration might
+eventually limit the accuracy."
+
+
+
+REFEREE: (5) CP sensitivity of T2HK obtained by the authors is
+significantly different from that estimated by T2KK people. With the
+same 5% error the former is up to sin22theta13 =2x10-3,but the latter
+extends to much smaller theta13 region, as shown in one of T2KK paper,
+Fig.7 in Ref.[60]. The authors of the paper include SK
+experimentalists and hence their treatment of the errors might be more
+appropriate than the present analysis. Therefore, at least some
+comments must be made on this discrepancy.
+
+ANSWER: In Ref. [34] (previously Ref. [60]) the systematical errors
+are taken to be correlated between neutrino and antineutrino data (see
+eqs. 3 and 4 of [34]), whereas in our calculation they are assumed to
+be uncorrelated. We have verified that this has a notable impact on
+the CPV sensitivity and can explain the different results.  We added a
+corresponding remark in the text on p. 22. Note that also for the
+CERN-MEMPHYS experiment we assume the errors to be uncorrelated, so we
+compare all experiments on equal footing.
+
+
+REFEREE: (6)It is not obvious which figure is nu only and which
+combines nu and anti-nu. A comment in each caption might be helpful to
+the readers.
+
+ANSWER: We added nu and anti-nu running times in all figure captions.
+
+REFEREE: (7)The fact that the spectral information solves the
+intrinsic degeneracy is noticed for T2K I about 2 years ago in
+Ref. [60].
+
+ANSWER: We do not claim to have discovered this here for the first
+time. We add references to [30,32,34] in the discussion of Fig. 6.
+
+
+REFEREE: (8) The authors do not explain the reason why theta13
+sensitivity has a sharp minimum at delta = pi, as seen in Fig.9; It is
+unusually abrupt drop of more than an order of magnitude.
+
+ANSWER: We add the following paragraph to the discussion of Fig. 9:
+
+"The peak of the sensitivity curves around $\delCP \approx \pi$
+appears due to the interplay of neutrino and antineutrino data. For
+the Super Beams neutrino (antineutrino) data are most sensitive in the
+region $\pi \lesssim \delCP \lesssim 2\pi$ ($0 \lesssim \delCP
+\lesssim \pi$), and opposite for the \BB, compare also Fig. 14 in
+Sec. 6.1. The particular shape of the sensitivity curves emerges from
+the relative location of the corresponding curves for neutrino and
+antineutrino data, which is controlled by the $L/E_\nu$ value where
+the experiment is operated and the value of $|\Delta m^2_{31}|$. The
+fact that the peak is most pronounced for the \BB\ follows from the
+somewhat smaler $L/E_\nu$ of the \BB\ compared to the Super Beams,
+whereas the shapes for SPL and T2HK are similar because of the similar
+$L/E_\nu$ values.
+
Index: /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-29sept06/CERN-MEMPHYS.aux
===================================================================
--- /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-29sept06/CERN-MEMPHYS.aux	(revision 385)
+++ /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-29sept06/CERN-MEMPHYS.aux	(revision 385)
@@ -0,0 +1,303 @@
+\relax 
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+\newlabel{fig:QE-Energy}{{2}{7}}
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+\newlabel{sec:degeneracies}{{4}{12}}
+\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Allowed regions in $\qopname  \relax o{sin}^22\theta _{13}$ and $\delta _\mathrm  {CP}$ for LBL data alone (contour lines) and LBL+ATM data combined (colored regions). $\mathrm  {H^{tr/wr} (O^{tr/wr})}$ refers to solutions with the true/wrong mass hierarchy (octant of $\theta _{23}$). The true parameter values are $\delta _\mathrm  {CP} = -0.85 \pi $, $\qopname  \relax o{sin}^22\theta _{13} = 0.03$, $\qopname  \relax o{sin}^2\theta _{23} = 0.6$, and the values from Eq.\nobreakspace  {}(\G@refundefinedtrue \text  {\normalfont  \bfseries  ??}\GenericWarning  {               }{LaTeX Warning: Reference `eq:default-params' on page 13 undefined}) for the other parameters.}}{13}}
+\newlabel{fig:degeneracies}{{5}{13}}
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+\newlabel{fig:degeneracies_SPL}{{6}{13}}
+\citation{Minakata:2001qm}
+\citation{Donini:2004hu}
+\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces Allowed regions in $\qopname  \relax o{sin}^22\theta _{13}$ and $\delta _\mathrm  {CP}$ for 5\nobreakspace  {}years data (neutrinos only) from $\beta $B, SPL, and the combination. $\mathrm  {H^{tr/wr} (O^{tr/wr})}$ refers to solutions with the true/wrong mass hierarchy (octant of $\theta _{23}$). For the colored regions in the left panel also 5\nobreakspace  {}years of atmospheric data are included; the solution with the wrong hierarchy has $\Delta \chi ^2 = 4$. The true parameter values are $\delta _\mathrm  {CP} = -0.85 \pi $, $\qopname  \relax o{sin}^22\theta _{13} = 0.03$, $\qopname  \relax o{sin}^2\theta _{23} = 0.6$, and the values from Eq.\nobreakspace  {}(\G@refundefinedtrue \text  {\normalfont  \bfseries  ??}\GenericWarning  {               }{LaTeX Warning: Reference `eq:default-params' on page 14 undefined}) for the other parameters. For the $\beta $B\ only analysis (middle panel) an external accuracy of 2\% (3\%) for $|\Delta m^2_{31}|$ ($\theta _{23}$) has been assumed, whereas for the left and right panel the default value of 10\% has been used.}}{14}}
+\newlabel{fig:degeneracies_5yrs}{{7}{14}}
+\citation{Antusch:2004yx}
+\citation{Minakata:2004pg}
+\citation{Donini:2005db}
+\citation{T2K}
+\citation{Maltoni:2004ei}
+\citation{Maltoni:2004ei}
+\citation{Donini:2005db}
+\@writefile{lot}{\contentsline {table}{\numberline {4}{\ignorespaces Accuracies at $3\sigma $ on the atmospheric parameters $|\Delta m^2_{31}|$ and $\qopname  \relax o{sin}^2\theta _{23}$ for 5 years of neutrino data from T2K-I, SPL, and T2HK for the two test points shown in Fig.\nobreakspace  {}\G@refundefinedtrue \text  {\normalfont  \bfseries  ??}\GenericWarning  {               }{LaTeX Warning: Reference `fig:atm-params' on page 15 undefined} ($\theta ^\mathrm  {true}_{13} = 0$). The accuracy for a parameter $x$ is defined as $(x^\mathrm  {upper} - x^\mathrm  {lower})/(2 x^\mathrm  {true})$, where $x^\mathrm  {upper}$ ($x^\mathrm  {lower}$) is the upper (lower) bound at 3$\sigma $ for 1\nobreakspace  {}d.o.f.\ obtained by projecting the contour $\Delta \chi ^2 = 9$ onto the $x$-axis. For the accuracies for test point\nobreakspace  {}2 the octant degenerate solution is neglected.}}{15}}
+\newlabel{tab:atm-params}{{4}{15}}
+\@writefile{toc}{\contentsline {section}{\numberline {5}Physics potential}{15}}
+\newlabel{sec:sensitivities}{{5}{15}}
+\@writefile{toc}{\contentsline {subsection}{\numberline {5.1}Sensitivity to the atmospheric parameters}{15}}
+\newlabel{sec:atm}{{5.1}{15}}
+\citation{Minakata:2004pg}
+\citation{Peres:2003wd}
+\citation{Gonzalez-Garcia:2004cu}
+\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces  Allowed regions of $\Delta m^2_{31}$ and $\qopname  \relax o{sin}^2\theta _{23}$ at 99\%\nobreakspace  {}CL (2 d.o.f.) after 5\nobreakspace  {}yrs of neutrino data taking for SPL, T2K phase\nobreakspace  {}I, T2HK, and the combination of SPL with 5\nobreakspace  {}yrs of atmospheric neutrino data in the MEMPHYS detector. For the true parameter values we use $\Delta m^2_{31} = 2.2\tmspace  +\thinmuskip {.1667em} (2.6) \times 10^{-3}\nobreakspace  {}\mathrm  {eV}^2$ and $\qopname  \relax o{sin}^2\theta _{23} = 0.5 \tmspace  +\thinmuskip {.1667em} (0.37)$ for the test point 1 (2), and $\theta _{13} = 0$ and the solar parameters as given in Eq.\nobreakspace  {}(\G@refundefinedtrue \text  {\normalfont  \bfseries  ??}\GenericWarning  {               }{LaTeX Warning: Reference `eq:default-params' on page 16 undefined}). The shaded region corresponds to the 99\%\nobreakspace  {}CL region from present SK and K2K data\nobreakspace  {}\cite  {Maltoni:2004ei}.}}{16}}
+\newlabel{fig:atm-params}{{8}{16}}
+\@writefile{toc}{\contentsline {subsection}{\numberline {5.2}The $\theta _{13}$ discovery potential}{16}}
+\newlabel{sec:th13}{{5.2}{16}}
+\@writefile{lof}{\contentsline {figure}{\numberline {9}{\ignorespaces $3\sigma $ discovery sensitivity to $\ensuremath  {\qopname  \relax o{sin}^22\theta _{13}}$ for $\beta $B, SPL, and T2HK as a function of the true value of \ensuremath  {\delta _{\rm  CP}}\ (left panel) and as a function of the fraction of all possible values of \ensuremath  {\delta _{\rm  CP}}\ (right panel). The width of the bands corresponds to values for the systematical errors between 2\% and 5\%. The black curves correspond to the combination of $\beta $B\ and SPL with 10\nobreakspace  {}yrs of total data taking each for a systematical error of 2\%, and the dashed curves show the sensitivity of the $\beta $B\ when the number of ion decays/yr are reduced by a factor of two with respect to the values given in Tab.\nobreakspace  {}\G@refundefinedtrue \text  {\normalfont  \bfseries  ??}\GenericWarning  {               }{LaTeX Warning: Reference `tab:setups' on page 17 undefined}.}}{17}}
+\newlabel{fig:th13}{{9}{17}}
+\@writefile{lof}{\contentsline {figure}{\numberline {10}{\ignorespaces  $3\sigma $ discovery sensitivity to $\ensuremath  {\qopname  \relax o{sin}^22\theta _{13}}$ for the SPL as a function of the true value of \ensuremath  {\delta _{\rm  CP}}\ for $\qopname  \relax o{sin}^2\theta _{23}^\mathrm  {true} = 0.6$ and true values for the other parameters as given in Eq.\nobreakspace  {}(\G@refundefinedtrue \text  {\normalfont  \bfseries  ??}\GenericWarning  {               }{LaTeX Warning: Reference `eq:default-params' on page 18 undefined}).}}{18}}
+\newlabel{fig:SPLTheta13Disco}{{10}{18}}
+\@writefile{toc}{\contentsline {subsection}{\numberline {5.3}Sensitivity to CP violation}{18}}
+\newlabel{sec:CPV}{{5.3}{18}}
+\@writefile{lof}{\contentsline {figure}{\numberline {11}{\ignorespaces CPV discovery potential for $\beta $B, SPL, and T2HK: For parameter values inside the ellipse-shaped curves CP conserving values of \ensuremath  {\delta _{\rm  CP}}\ can be excluded at $3\sigma $ $(\Delta \chi ^2>9)$. The width of the bands corresponds to values for the systematical errors from 2\% to 5\%. The dashed curves show the sensitivity of the $\beta $B\ when the number of ion decays/yr are reduced by a factor of two with respect to the values given in Tab.\nobreakspace  {}\G@refundefinedtrue \text  {\normalfont  \bfseries  ??}\GenericWarning  {               }{LaTeX Warning: Reference `tab:setups' on page 19 undefined} for 2\% systematics.}}{19}}
+\newlabel{fig:CPV}{{11}{19}}
+\@writefile{lof}{\contentsline {figure}{\numberline {12}{\ignorespaces Impact of total exposure and systematical errors on the CPV discovery potential of $\beta $B, SPL, and T2HK. We show the smallest true value of $\ensuremath  {\qopname  \relax o{sin}^22\theta _{13}}$ for which $\ensuremath  {\delta _{\rm  CP}}= \pi /2$ can be distinguished from $\ensuremath  {\delta _{\rm  CP}}= 0$ or $\ensuremath  {\delta _{\rm  CP}}= \pi $ at $3\sigma $ $(\Delta \chi ^2>9)$ as a function of the exposure in kt\nobreakspace  {}yrs (left) and as a function of the systematical error on the background $\sigma _\mathrm  {bkgr}$ (right). The widths of the curves in the left panel corresponds to values of $\sigma _\mathrm  {bkgr}$ from 2\% to 5\%. The thin solid curves in the left panel corresponds to no systematical errors. The right plot is calculated for the standard exposure of 4400\nobreakspace  {}kt\nobreakspace  {}yrs. No systematical error on the signal has been assumed. }}{20}}
+\newlabel{fig:systematics}{{12}{20}}
+\citation{Ishitsuka:2005qi}
+\@writefile{lof}{\contentsline {figure}{\numberline {13}{\ignorespaces Impact of degeneracies on the CPV discovery potential for the $\beta $B. We show the sensitivity to CPV at $3\sigma $ $(\Delta \chi ^2>9)$ computed for 4 different combinations of the true values of the hierarchy (NH or IH) and $\theta _{23}$ ($\qopname  \relax o{sin}^2\theta _{23} = 0.4$ or $0.6$). Dashed curves are computed neglecting degeneracies in the fit.}}{21}}
+\newlabel{fig:deltacp}{{13}{21}}
+\citation{Huber:2005ep}
+\citation{Huber:2005ep}
+\citation{Petcov:1998su}
+\citation{Akhmedov:1998ui}
+\citation{Bernabeu:2003yp}
+\citation{Kim:1998bv}
+\citation{Peres:2003wd}
+\citation{Gonzalez-Garcia:2004cu}
+\citation{Kajita}
+\citation{Huber:2005ep}
+\@writefile{toc}{\contentsline {section}{\numberline {6}Synergies provided by the CERN--MEMPHYS facilities}{22}}
+\newlabel{sec:synergies}{{6}{22}}
+\@writefile{toc}{\contentsline {subsection}{\numberline {6.1}Combining Beta Beam and Super Beam}{22}}
+\newlabel{sec:synergies-beams}{{6.1}{22}}
+\@writefile{toc}{\contentsline {subsection}{\numberline {6.2}Resolving degeneracies with atmospheric neutrinos}{22}}
+\newlabel{sec:atmospherics}{{6.2}{22}}
+\@writefile{lof}{\contentsline {figure}{\numberline {14}{\ignorespaces Discovery potential of a finite value of $\ensuremath  {\qopname  \relax o{sin}^22\theta _{13}}$ at $3\sigma $ $(\Delta \chi ^2>9)$ for 5\nobreakspace  {}yrs neutrino data from $\beta $B, SPL, and the combination of $\beta $B\ + SPL compared to 10\nobreakspace  {}yrs data from T2HK (2\nobreakspace  {}yrs neutrinos + 8\nobreakspace  {}yrs antineutrinos). }}{23}}
+\newlabel{fig:th13-5yrs}{{14}{23}}
+\@writefile{lof}{\contentsline {figure}{\numberline {15}{\ignorespaces Sensitivity to CPV at $3\sigma $ $(\Delta \chi ^2>9)$ for combining 5\nobreakspace  {}yrs neutrino data from $\beta $B\ and SPL compared to 10\nobreakspace  {}yrs data from T2HK (2\nobreakspace  {}yrs neutrinos + 8\nobreakspace  {}yrs antineutrinos). }}{23}}
+\newlabel{fig:CP-5yrs}{{15}{23}}
+\citation{Huber:2005ep}
+\citation{Ayres:2004js}
+\citation{Ayres:2004js}
+\citation{Ayres:2004js}
+\citation{Ayres:2004js}
+\citation{Huber:2005ep}
+\@writefile{lof}{\contentsline {figure}{\numberline {16}{\ignorespaces Sensitivity to the mass hierarchy at $2\sigma $ $(\Delta \chi ^2 = 4)$ as a function of the true values of $\qopname  \relax o{sin}^22\theta _{13}$ and $\delta _\mathrm  {CP}$ (left), and the fraction of true values of $\ensuremath  {\delta _{\rm  CP}}$ (right). The solid curves are the sensitivities from the combination of long-baseline and atmospheric neutrino data, the dashed curves correspond to long-baseline data only. For comparison we show in the right panel also the sensitivities of NO$\nu $A and NO$\nu $A+T2K extracted from Fig.\nobreakspace  {}13.14 of Ref.\nobreakspace  {}\cite  {Ayres:2004js}. For the curve labeled ``NO$\nu $A (p.dr.)+T2K@4\nobreakspace  {}MW'' a proton driver has been assumed for NO$\nu $A and the T2K beam has been up-graded to 4\nobreakspace  {}MW, see Ref.\nobreakspace  {}\cite  {Ayres:2004js} for details.}}{24}}
+\newlabel{fig:hierarchy}{{16}{24}}
+\citation{Huber:2005ep}
+\citation{Petcov:2005rv}
+\citation{Ayres:2004js}
+\citation{Ayres:2004js}
+\citation{Ishitsuka:2005qi}
+\citation{MenaRequejo:2005hn}
+\citation{Hagiwara:2005pe}
+\citation{Kachelriess:2004vs}
+\citation{Huber:2005ep}
+\citation{Huber:2005ep}
+\citation{Gonzalez-Garcia:2004cu}
+\citation{Ishitsuka:2005qi}
+\@writefile{lof}{\contentsline {figure}{\numberline {17}{\ignorespaces $\Delta \chi ^2$ of the solution with the wrong octant of $\theta _{23}$ as a function of the true value of $\qopname  \relax o{sin}^2\theta _{23}$. We have assumed a true value of $\theta _{13} = 0$.}}{26}}
+\newlabel{fig:octant}{{17}{26}}
+\@writefile{toc}{\contentsline {section}{\numberline {7}Summary}{26}}
+\newlabel{sec:conclusions}{{7}{26}}
+\citation{ISSpage}
+\bibcite{solar}{1}
+\bibcite{Fukuda:1998mi}{2}
+\bibcite{Ashie:2005ik}{3}
+\bibcite{Araki:2004mb}{4}
+\bibcite{Aliu:2004sq}{5}
+\bibcite{MINOS}{6}
+\bibcite{OPERA}{7}
+\bibcite{CNGS}{8}
+\bibcite{LSND}{9}
+\bibcite{MINIBOONE}{10}
+\bibcite{FOGLILISI05}{11}
+\bibcite{Maltoni:2004ei}{12}
+\bibcite{PMNS}{13}
+\bibcite{CHOOZ}{14}
+\bibcite{Wpaper}{15}
+\bibcite{T2K}{16}
+\bibcite{Ayres:2004js}{17}
+\bibcite{Huber:2003pm}{18}
+\bibcite{Albrow:2005kw}{19}
+\bibcite{SPL}{20}
+\bibcite{BNLHS}{21}
+\bibcite{zucchelli}{22}
+\bibcite{Albright:2004iw}{23}
+\bibcite{Blondel:2004ae}{24}
+\bibcite{Campagne:2004wt}{25}
+\bibcite{Mezzetto:2003ub}{26}
+\bibcite{memphys}{27}
+\bibcite{UNO}{28}
+\bibcite{Nakamura:2003hk}{29}
+\bibcite{Huber:2005ep}{30}
+\bibcite{Globes}{31}
+\bibcite{Huber:2002mx}{32}
+\bibcite{Nuance}{33}
+\bibcite{ISSpage}{34}
+\bibcite{MyNufact04}{35}
+\bibcite{Donini:2004hu}{36}
+\bibcite{JJHigh2}{37}
+\bibcite{LindnerBB}{38}
+\bibcite{JJHigh1}{39}
+\bibcite{Terranova}{40}
+\bibcite{BB-Reviews}{41}
+\bibcite{Volpe}{42}
+\bibcite{Lindroos}{43}
+\bibcite{Eurisol}{44}
+\bibcite{Lindroos-Optimization}{45}
+\bibcite{MezzettoNuFact05}{46}
+\bibcite{Neugen}{47}
+\bibcite{FLUKA}{48}
+\bibcite{GEANT}{49}
+\bibcite{HARP-MINERVA}{50}
+\bibcite{Mezzetto:2003mm}{51}
+\bibcite{Honda:2004yz}{52}
+\bibcite{Lipari:1991ut}{53}
+\bibcite{Gonzalez-Garcia:2004wg}{54}
+\bibcite{Burguet-Castell:2001ez}{55}
+\bibcite{Minakata:2001qm}{56}
+\bibcite{Fogli:1996pv}{57}
+\bibcite{Barger:2001yr}{58}
+\bibcite{Yasuda:2004gu}{59}
+\bibcite{Ishitsuka:2005qi}{60}
+\bibcite{Antusch:2004yx}{61}
+\bibcite{Minakata:2004pg}{62}
+\bibcite{Donini:2005db}{63}
+\bibcite{Peres:2003wd}{64}
+\bibcite{Gonzalez-Garcia:2004cu}{65}
+\bibcite{Petcov:1998su}{66}
+\bibcite{Akhmedov:1998ui}{67}
+\bibcite{Bernabeu:2003yp}{68}
+\bibcite{Kim:1998bv}{69}
+\bibcite{Kajita}{70}
+\bibcite{Petcov:2005rv}{71}
+\bibcite{MenaRequejo:2005hn}{72}
+\bibcite{Hagiwara:2005pe}{73}
+\bibcite{Kachelriess:2004vs}{74}
Index: /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-29sept06/CERN-MEMPHYS.blg
===================================================================
--- /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-29sept06/CERN-MEMPHYS.blg	(revision 385)
+++ /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-29sept06/CERN-MEMPHYS.blg	(revision 385)
@@ -0,0 +1,4 @@
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+I found no \bibstyle command---while reading file C:\Presentation\NuFactSB\CERN-Frejus\TS-29sept06\CERN-MEMPHYS.aux
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Index: /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-29sept06/CERN-MEMPHYS.log
===================================================================
--- /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-29sept06/CERN-MEMPHYS.log	(revision 385)
+++ /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-29sept06/CERN-MEMPHYS.log	(revision 385)
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+[][]\OT1/cmr/m/n/12 B. Autin \OT1/cmr/m/it/12 et al.\OT1/cmr/m/n/12 , J. Phys. 
+G \OT1/cmr/bx/n/12 29\OT1/cmr/m/n/12 , 1785 (2003) [physics/0306106];
+ []
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+C, 2004,
+ []
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+[]\OT1/cmtt/m/n/12 http://accelconf.web.cern.ch/AccelConf/e04\OT1/cmr/m/n/12 ; 
+M. Lin-droos, EU-RISOL
+ []
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+[][]\OT1/cmr/m/n/12 The NEU-GEN neu-trino event gen-er-a-tor, []\OT1/cmtt/m/n/1
+2 http://minos.phy.tufts.edu/gallag/neugen/\OT1/cmr/m/n/12 . 
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+%%%%%%%%%%%%%%%%%%%%%%%%
+% definitions
+%%%%%%%%%%%%%%%%%%%%%%%%
+\newcommand{\centre}[2]{\multispan{#1}{\hfill #2\hfill}}
+\newcommand{\etal}{\textit{et al.}}
+\newcommand{\stheta}{\ensuremath{\sin^22\theta_{13}}}
+\newcommand{\BB}{$\beta$B}
+\newcommand{\sigdm}{\ensuremath{{\rm sign}(\Delta m^2_{31})}}
+\newcommand{\delCP}{\ensuremath{\delta_{\rm CP}}}
+\newcommand{\thetatt}{\ensuremath{\theta_{23}}}
+
+\def\nubar{$\overline{\nu}\ $}
+\def\nue{\ensuremath{\nu_{e}}}
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+\def\numu{\ensuremath{\nu_{\mu}\ }}
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+\def\nutau{\ensuremath{\nu_{\tau}\ }}
+\def\nubartau{\ensuremath{\overline{\nu}_{\tau}}}
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+\newcommand{\nubarmunubare}{\ensuremath{\overline{\nu}_\mu \rightarrow \overline{\nu}_e\,}}
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+
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+\def\anumu{\overline{{\mathrm\nu}}_{\mathrm \mu}}
+\newcommand{\thetaot}{\ensuremath{\theta_{13}}\,}
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+\newcommand{\nueovernumu}{\ensuremath{\nue/\numu}}
+
+\newcommand{\Efin}{E^\text{fin}}
+\newcommand{\Emin}{E_\text{min}}
+
+
+\begin{document}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+%%%%                     Title-page                              %%%%
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+%\begin{titlepage}
+
+% the footnote symbols are only redefined for the title page !
+\renewcommand{\thefootnote}{\alph{footnote}}
+
+\begin{flushright}
+LAL-06-35\\
+IC/2006/011\\
+SISSA 16/2006/EP\\
+\end{flushright}
+
+\vspace*{1cm}
+
+\renewcommand{\thefootnote}{\fnsymbol{footnote}}
+\setcounter{footnote}{-1}
+
+{\begin{center} 
+{\Large\textbf{
+Physics potential of the CERN--MEMPHYS\\[2mm] 
+neutrino oscillation project}
+}
+\end{center}}
+
+\vspace*{.8cm}
+
+\begin{center} {\bf
+J.-E.\ Campagne$^a$, 
+M.\ Maltoni$^b$,
+M.\ Mezzetto$^c$, and 
+T.\ Schwetz$^d$}
+\end{center}
+
+{\it
+\begin{center}
+  $^a$Laboratoire de l'Acc\'el\'erateur Lin\'eaire, 
+  IN2P3-CNRS and Universit\'e PARIS-SUD 11\\
+  Centre Scientifique d'Orsay-B\^at.\ 200-B.P.\ 34, 
+  91898 Orsay Cedex, France\\[2mm]
+%  
+  $^b$International Centre for Theoretical Physics, 
+  Strada Costiera 11, 31014 Trieste, Italy\\[2mm]
+%  
+  $^c$Istituto Nazionale Fisica Nucleare, Sezione di Padova,
+  Via Marzolo 8, 35100 Padova, Italy\\[2mm]
+%
+  $^d$Scuola Internazionale Superiore di Studi Avanzati, 
+  Via Beirut 2--4, 34014 Trieste, Italy
+\end{center}}
+
+\vspace*{0.5cm}
+
+
+\begin{abstract}
+We consider the physics potential of CERN based neutrino oscillation
+experiments consisting of a Beta Beam (\BB) and a Super Beam (SPL)
+sending neutrinos to MEMPHYS, a 440~kt water \v{C}erenkov detector at
+Fr\'ejus, at a distance of 130~km from CERN. The $\theta_{13}$
+discovery reach and the sensitivity to CP violation are investigated,
+including a detailed discussion of parameter degeneracies and
+systematical errors. For SPL sensitivities similar to the ones of the
+phase~II of the T2K experiment (T2HK) are obtained, whereas the \BB\
+may reach significantly better sensitivities, depending on the
+achieved number of total ion decays.  The results for the
+CERN--MEMPHYS experiments are less affected by systematical
+uncertainties than T2HK.
+%
+We point out that by a combination of data from \BB\ and SPL a
+measurement with antineutrinos is not necessary and hence the same
+physics results can be obtained within about half of the measurement time
+compared to one single experiment.
+%
+Furthermore, it is shown how including data from atmospheric neutrinos in
+the MEMPHYS detector allows to resolve parameter degeneracies and, in
+particular, provides sensitivity to the neutrino mass hierarchy and
+the octant of $\theta_{23}$.
+%\pacs{14.60.Pq, 14.60.Lm}
+\end{abstract}
+
+\renewcommand{\thefootnote}{\arabic{footnote}}
+\setcounter{footnote}{0}
+
+\newpage
+%\tableofcontents
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Introduction}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+In recent years strong evidence for neutrino oscillations has been
+obtained in solar~\cite{solar},
+atmospheric~\cite{Fukuda:1998mi,Ashie:2005ik},
+reactor~\cite{Araki:2004mb}, and accelerator~\cite{Aliu:2004sq}
+neutrino experiments. The very near future of long-baseline (LBL)
+neutrino experiments is devoted to the study of the oscillation
+mechanism in the range of $\Delta m^2_{31} \approx 2.4\times10^{-3} \:
+\mathrm{eV}^2$ indicated by atmospheric neutrinos using conventional
+$\nu_\mu$ beams.  Similar as in the K2K experiment in
+Japan~\cite{Aliu:2004sq}, the presently running MINOS experiment in
+the USA~\cite{MINOS} uses a low energy beam to measure $\Delta
+m^2_{31}$ by observing the $\nu_\mu\rightarrow\nu_\mu$ disappearance
+probability, while the OPERA~\cite{OPERA} experiment will be able to
+detect $\nu_\tau$ appearance within the high energy CERN--Gran Sasso
+beam~\cite{CNGS}.
+%
+If we do not consider the LSND anomaly~\cite{LSND} that will be
+further studied soon by the MiniBooNE experiment~\cite{MINIBOONE}, all
+data can be accommodated within the three flavor scenario (see
+Refs.~\cite{FOGLILISI05,Maltoni:2004ei} for recent global analyses),
+and neutrino oscillations are described by two neutrino mass-squared
+differences ($\Delta m^2_{21}$ and $\Delta m^2_{31}$) and the $3\times
+3$ unitary Pontecorvo-Maki-Nakagawa-Sakata (PMNS) lepton mixing
+matrix~\cite{PMNS} with three angles
+($\theta_{12}$,$\theta_{13}$,$\theta_{23}$) and one Dirac CP phase
+$\delCP$.
+
+Future tasks of neutrino physics are an improved sensitivity to the
+last unknown mixing angle, $\theta_{13}$, to explore the CP violation
+mechanism in the leptonic sector, and to determine the sign of $\Delta
+m^2_{31}$ which describes the type of the neutrino mass hierarchy
+(normal, $\Delta m^2_{31} > 0$ or inverted, $\Delta m^2_{31} < 0$).
+%
+The present upper bound on $\theta_{13}$ is dominated by the
+constraint from the Chooz reactor experiment~\cite{CHOOZ}. A global
+analysis of all data yields $\sin^22\theta_{13}<0.082$ at
+90\%~CL~\cite{Maltoni:2004ei}. A main purpose of upcoming reactor and
+accelerator experiments is to improve this bound or to reveal a finite
+value of $\theta_{13}$. In reactor experiments, one uses $\bar{\nu}_e$
+in disappearance mode and the sensitivity is increased with respect to
+present experiments by the use of a near detector close to the
+reactor~\cite{Wpaper}. In accelerator experiments, the first
+generation of so-called Super Beams with sub-mega watt proton drivers
+such as T2K (phase-I)~\cite{T2K} and NO$\nu$A~\cite{Ayres:2004js}, the
+appearance channel $\nu_\mu\to\nu_e$ is explored. This next generation
+of reactor and Super Beam experiments will reach sensitivities of the
+order of $\sin^22\theta_{13} \lesssim 0.01$ ($90\%$~CL) within a time
+scale of several years~\cite{Huber:2003pm}.
+%
+Beyond this medium term program, there are several projects on how to
+enter the high precision age in neutrino oscillations and to attack
+the ultimate goals like the discovery of leptonic CP violation or the
+determination of the neutrino mass hierarchy. In accelerator
+experiments, one can extend the Super Beam concept by moving to
+multi-mega watt proton drivers~\cite{T2K,Albrow:2005kw,SPL,BNLHS} or
+apply novel technologies, such as neutrino beams from decaying ions
+(so-called Beta Beams)~\cite{zucchelli,Albright:2004iw} or from
+decaying muons (so-called Neutrino
+Factories)~\cite{Albright:2004iw,Blondel:2004ae}.
+
+In this work we focus on possible future neutrino oscillation
+facilities hosted at CERN, namely a multi-mega watt Super Beam
+experiment based on a Super Proton Linac (SPL)~\cite{Campagne:2004wt}
+and a $\gamma = 100$ Beta Beam
+(\BB)~\cite{Mezzetto:2003ub}. These experiments will search for
+$\stackrel{\scriptscriptstyle (-)}{\nu}_\mu \to
+\stackrel{\scriptscriptstyle(-)}{\nu}_e$ and
+$\stackrel{\scriptscriptstyle (-)}{\nu}_e \to
+\stackrel{\scriptscriptstyle(-)}{\nu}_\mu$ appearance, respectively,
+by sending the neutrinos to a mega ton scale water \v{C}erenkov
+detector (MEMPHYS)~\cite{memphys}, located at a distance of 130~km from
+CERN under the Fr\'ejus mountain. Similar detectors are under
+consideration also in the US (UNO~\cite{UNO}) and in Japan
+(Hyper-K~\cite{T2K,Nakamura:2003hk}).
+%
+We perform a detailed analysis of the SPL and \BB\ physics
+potential, discussing the discovery reach for $\theta_{13}$ and
+leptonic CP violation. In addition we consider the possibility to
+resolve parameter degeneracies in the LBL data by using the
+atmospheric neutrinos available in the mega ton
+detector~\cite{Huber:2005ep}. This leads to a sensitivity to the
+neutrino mass hierarchy of the CERN--MEMPHYS experiments, despite the
+rather short baseline.
+%
+The physics performances of \BB\ and SPL are compared to the ones
+obtainable at the second phase of the T2K experiment in Japan, which
+is based on an upgraded version of the original T2K beam and the
+Hyper-K detector (T2HK)~\cite{T2K}.
+
+The outline of the paper is as follows.  In Sec.~\ref{sec:analysis} we
+summarize the main characteristics of the \BB, SPL, and T2HK
+experiments and give general details of the physics analysis methods,
+whereas in Sec.~\ref{sec:experiments} we describe in some detail the
+MEMPHYS detector, the \BB, the SPL Super Beam, and our atmospheric
+neutrino analysis. In Sec.~\ref{sec:degeneracies} we review the
+problem of parameter degeneracies and discuss its implications for the
+experiments under consideration. In Sec.~\ref{sec:sensitivities} we
+present the sensitivities to the ``atmospheric parameters''
+$\theta_{23}$ and $\Delta m^2_{31}$, the $\theta_{13}$ discovery
+potential, and the sensitivity to CP violation. We also investigate in
+some detail the impact of systematical errors. In
+Sec.~\ref{sec:synergies} we discuss synergies which are offered by the
+CERN--MEMPHYS facilities.  We point out advantages of the case when
+\BB\ and SPL are available simultaneously, and we consider the use of
+atmospheric neutrino data in MEMPHYS in combination with the LBL
+experiments. Our results are summarized in Sec.~\ref{sec:conclusions}.
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Experiments overview and analysis methods}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:analysis}
+
+In this section we give the most important experimental parameters
+which we adopt for the simulation of the CERN--MEMPHYS experiments
+\BB\ and SPL, as well as for the T2HK experiment in Japan. These
+parameters are summarized in Tab.~\ref{tab:setups}. For all
+experiments the detector mass is 440~kt, and the running time is 10
+years, with a division in neutrino and antineutrino running time in
+such a way that roughly an equal number of events is obtained. We
+always use the total available information from appearance as well as
+disappearance channels including the energy spectrum. For all three
+experiments we adopt rather optimistic values for the systematical
+uncertainties of 2\% as default values, but we also consider the case
+when systematics are increased to 5\%. These errors are uncorrelated
+between the various signal channels (neutrinos and antineutrinos), and
+between signals and backgrounds.
+
+\begin{table}
+  \centering
+  \begin{tabular}{lcc@{\qquad\qquad}c}
+  \hline\noalign{\smallskip}
+       & \BB & SPL & T2HK \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  Detector mass & 440~kt & 440~kt & 440~kt\\
+  Baseline      & 130 km & 130 km & 295 km \\
+  Running time ($\nu + \bar\nu$) 
+                & 5 + 5 yr & 2 + 8 yr & 2 + 8 yr \\
+  Beam intensity  & $5.8\,(2.2) \cdot 10^{18}$ He (Ne) dcys/yr & 4 MW & 4 MW\\
+  Systematics on signal  & 2\% & 2\% & 2\%\\
+  Systematics on backgr. & 2\% & 2\% & 2\%\\
+  \noalign{\smallskip}\hline
+  \end{tabular}
+  \mycaption{Summary of default parameters used for the simulation of the
+  \BB, SPL, and T2HK experiments.\label{tab:setups}}
+\end{table}
+
+A more detailed description of the CERN--MEMPHYS experiments is given
+in Sec.~\ref{sec:experiments}. For the T2HK simulation we use the
+setup provided by GLoBES~\cite{Globes} based on
+Ref.~\cite{Huber:2002mx}, which follows closely the LOI~\cite{T2K}. In
+order to allow a fair comparison we introduce the following changes
+with respect to the configuration used in Ref.~\cite{Huber:2002mx}:
+The fiducial mass is set to 440~kt, the systematical errors on the
+background and on the $\nu_e$ and $\bar\nu_e$ appearance signals is
+set to 2\%, and we use a total running time of 10 years, divided into
+2 years of data taking with neutrinos and 8 years with
+antineutrinos. We include an additional background from the
+$\bar\nu_\mu \to \bar\nu_e$ ($\nu_\mu \to \nu_e$) channel in the
+neutrino (antineutrino) mode. Furthermore, we use
+the same CC detection cross section as for the \BB/SPL
+analysis~\cite{Nuance}. For more details see
+Refs.~\cite{T2K,Huber:2002mx}.
+
+\begin{table}
+  \centering
+  \begin{tabular}{lcccccc}
+  \hline\noalign{\smallskip}
+       & \centre{2}{\BB} & \centre{2}{SPL} & \centre{2}{T2HK} \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  & $\delCP=0$ & $\delCP=\pi/2$ & $\delCP=0$ & $\delCP=\pi/2$ & $\delCP=0$ & $\delCP=\pi/2$\\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+%
+  appearance $\nu$ & & & & & & \\
+  background       & \centre{2}{143} &\centre{2}{622} &\centre{2}{898}\\
+  $\stheta=0$      & \centre{2}{28}  &\centre{2}{51}  &\centre{2}{83}  \\
+  $\stheta=10^{-3}$&    76  &   88   &   105  &   14  &   178 &    17  \\ 
+  $\stheta=10^{-2}$&   326  &  365   &   423  &  137  &   746 &   238  \\
+%  
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+%
+  appearance $\bar\nu$ & & & & & & \\
+  background       & \centre{2}{157} &\centre{2}{640} &\centre{2}{1510}\\
+  $\stheta=0$      & \centre{2}{31}  &\centre{2}{57}  &\centre{2}{93}  \\
+  $\stheta=10^{-3}$&    83  &   12   &   102  &  146  &   192 &   269  \\ 
+  $\stheta=10^{-2}$&   351  &  126   &   376  &  516  &   762 &  1007  \\
+%  
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+%
+  disapp. $\nu$ &\centre{2}{100315}&\centre{2}{21653}&\centre{2}{24949}\\
+  background    & \centre{2}{6}   &\centre{2}{1}    &\centre{2}{444}\\
+  disapp. $\bar\nu$&\centre{2}{84125}&\centre{2}{18321}&\centre{2}{34650}\\
+  background       &\centre{2}{5}    &\centre{2}{1}    &\centre{2}{725}\\
+  \noalign{\smallskip}\hline
+%  
+  \end{tabular}
+  \mycaption{Number of events for appearance and disappearance signals
+  and backgrounds for the \BB, SPL, and T2HK experiments as
+  defined in Tab.~\ref{tab:setups}. For the appearance signals the
+  event numbers are given for several values of $\stheta$ and $\delCP
+  = 0$ and $\pi/2$. The background as well as the disappearance event
+  numbers correspond to $\theta_{13}=0$. For the other oscillation
+  parameters the values of Eq.~(\ref{eq:default-params}) are
+  used.\label{tab:events}}
+\end{table}
+
+In Tab.~\ref{tab:events} we give the number of signal and background
+events for the experiment setups as defined in Tab.~\ref{tab:setups}.
+For the appearance channels ($\stackrel{\scriptscriptstyle (-)}{\nu}_e
+\to \stackrel{\scriptscriptstyle(-)}{\nu}_\mu$ for the \BB\ and
+$\stackrel{\scriptscriptstyle (-)}{\nu}_\mu \to
+\stackrel{\scriptscriptstyle(-)}{\nu}_e$ for SPL and T2HK) we give the
+signal events for various values of $\theta_{13}$ and $\delCP$. The
+``signal'' events for $\theta_{13} = 0$ are appearance events induced by
+the oscillations with $\Delta m^2_{21}$. The value $\stheta = 10^{-3}$
+corresponds roughly to the sensitivity limit for the considered
+experiments, whereas $\stheta = 10^{-2}$ gives a good sensitivity
+to CP violation. This can be appreciated by comparing the values of
+$\nu$ and $\bar\nu$ appearance events for $\delCP = 0$ and $\pi/2$. In
+the table the background to the appearance signal is given for
+$\theta_{13} = 0$. Note that in general the number of background
+events depends also on the oscillation parameters, since also the
+background neutrinos in the beam oscillate. This effect is
+consistently taken into account in the analysis, however, for the
+parameter values in the table the change in the background events due
+to oscillations is only of the order of a few events.
+
+The physics analysis is performed with the GLoBES open source
+software~\cite{Globes}, which provides a convenient tool to simulate
+long-baseline experiments and compare different facilities in a
+unified framework. The experiment definition (AEDL) files for the \BB\
+and SPL simulation with GLoBES are available at Ref.~\cite{ISSpage}.
+In the analysis parameter degeneracies and correlations are fully
+taken into account and in general all oscillation parameters are
+varied in the fit.
+%
+To simulate the ``data'' we adopt the following
+set of ``true values'' for the oscillation parameters:
+%
+\begin{equation}\label{eq:default-params}
+\begin{array}{l@{\qquad}l}
+  \Delta m^2_{31} = +2.4 \times 10^{-3}~\mathrm{eV}^2\,, & 
+  \sin^2\theta_{23} = 0.5\,,\\ 
+  \Delta m^2_{21} = 7.9 \times 10^{-5}~\mathrm{eV}^2 \,,&
+  \sin^2\theta_{12} = 0.3 \,,
+\end{array}
+\end{equation} 
+%
+and we include a prior knowledge of these values with an accuracy of
+10\% for $\theta_{12}$, $\theta_{23}$, $\Delta m^2_{31}$, and 4\% for
+$\Delta m^2_{21}$ at 1$\sigma$. These values and accuracies are
+motivated by recent global fits to neutrino oscillation
+data~\cite{FOGLILISI05,Maltoni:2004ei}, and they are always used
+except where explicitly stated otherwise.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{The CERN--MEMPHYS experiments}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:experiments}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The MEMPHYS detector}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+MEMPHYS (MEgaton Mass PHYSics)~\cite{memphys} is a mega ton class
+water \v{C}erenkov detector in the straight extrapolation of
+Super-Kamiokande, located at Fr\'ejus, at a distance of 130~km from
+CERN. It is an alternative design of the UNO~\cite{UNO} and
+Hyper-Kamiokande~\cite{Nakamura:2003hk} detectors and shares the same
+physics case, both from the non-accelerator domain (nucleon decay,
+super nova neutrino detection, solar neutrinos, atmospheric neutrinos)
+and from the accelerator domain which is the subject of this paper. A
+recent civil engineering pre-study to envisage the possibly of large
+cavity excavation located under the Fr\'ejus mountain (4800~m.e.w.)
+near the present Modane underground laboratory has been undertaken.
+The main result of this pre-study is that MEMPHYS may be built with
+present techniques as a modular detector consisting of several shafts,
+each with 65~m in diameter, 65~m in height for the total water
+containment. A schematic view of the layout is shown in
+Fig.~\ref{fig:MEMPHYS}. For the present study we have chosen a
+fiducial mass of 440~kt which means 3 shafts and an inner detector of
+57~m in diameter and 57~m in height.  Each inner detector may be
+equipped with photo detectors (81000 per shaft) with a 30\%
+geometrical coverage and the same photo-statistics as Super-Kamiokande
+(with a 40\% coverage). In principle up to 5 shafts are possible,
+corresponding to a fiducial mass of 730~kt.
+%
+The Fr\'ejus site offers a natural protection against cosmic rays by a
+factor $10^6$. If not mentioned otherwise, the event selection and
+particle identification are the Super-Kamiokande algorithms results.
+
+\begin{figure}
+\centering
+\includegraphics[width=0.65\textwidth]{./fig1.eps}
+\mycaption{\label{fig:MEMPHYS}Sketch of the MEMPHYS detector under the
+Fr\'ejus mountain.}	
+\end{figure}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The $\gamma = 100\times100$ baseline Beta Beam}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+The concept of a Beta Beam (\BB) has been introduced by P.~Zucchelli
+in Ref.~\cite{zucchelli}. Neutrinos are produced by the decay of
+radioactive isotopes which are stored in a decay ring. An important
+parameter is the relativistic gamma factor of the ions, which
+determines the energy of the emitted neutrinos. \BB\ performances have
+been computed previously for $\gamma(\He)= 66$~\cite{Mezzetto:2003ub},
+100~\cite{MyNufact04,Donini:2004hu,JJHigh2}, 150~\cite{JJHigh2},
+200~\cite{LindnerBB}, 350~\cite{JJHigh2},
+500~\cite{JJHigh1,LindnerBB}, 1000~\cite{LindnerBB},
+2000~\cite{JJHigh1}, 2488~\cite{Terranova}. Reviews can be found in
+Ref.~\cite{BB-Reviews}, the physics potential of a very low gamma \BB\
+has been studied in Ref.~\cite{Volpe}. Performances of a \BB\ with
+$\gamma > 150$ are extremely promising, however, they are neither
+based on an existing accelerator complex nor on detailed calculations
+of the ion decay rates. For a CERN based \BB, fluxes have been
+estimated in Ref.~\cite{Lindroos} and a design study is in progress
+for the facility \cite{Eurisol}. In this work we assume an integrated
+flux of neutrinos in 10 years corresponding to $2.9\cdot 10^{19}$
+useful \He\ decays and $1.1 \cdot 10^{19}$ useful \Ne\ decays. These
+fluxes have been assumed in all the physics papers quoted above, and
+they are two times higher than the baseline fluxes computed in
+Ref.~\cite{Lindroos}. These latter fluxes suffer for the known
+limitations of the PS and SPS synchrotrons at CERN, ways to improve
+them have been delineated in Ref.~\cite{Lindroos-Optimization}.
+
+The infrastructure available at CERN as well as the MEMPHYS
+location at a distance of 130~km suggest a $\gamma$-factor of about
+$100$. Such a value implies a mean neutrino energy of 400~MeV, which
+leads to the oscillation maximum at about 200~km for $\Delta m^2_{31}
+= 2.4\times 10^{-3}$~eV$^2$.  We have checked that the performance at
+the somewhat shorter baseline of 130~km is rather similar to the one
+at the oscillation maximum. Moreover, the purpose of this paper is to
+estimate the physics potential for a realistic set-up and not to study
+the optimization of the \BB\ regardless of any logistic consideration
+(see, e.g., Refs.~\cite{LindnerBB,JJHigh2} for such optimization
+studies).
+
+The signal events from the $\nu_e \to \nu_\mu$ neutrino and
+antineutrino appearance channels in the \BB\ are \numu charged current
+(CC) events. The Nuance v3r503 Monte Carlo code~\cite{Nuance} is used
+to generate signal events. The selection for these events is based on
+standard Super-Kamiokande particle identification algorithms.  The
+muon identification is reinforced by asking for the detection of the
+Michel decay electron. 
+%
+The neutrino energy is reconstructed by smearing momentum and
+direction of the charged lepton with the Super-Kamiokande resolution
+functions, and applying quasi-elastic (QE) kinematics assuming the
+known incoming neutrino direction. Energy reconstruction in the \BB\
+energy range is remarkably powerful, and the contamination of non-QE
+events very small, as shown in Fig.~\ref{fig:QE-Energy}.
+%
+As pointed out in Ref.~\cite{JJHigh2}, it is necessary to use a
+migration matrix for the neutrino energy reconstruction to properly
+handle Fermi motion smearing and the non-QE event contamination.  We
+use 100~MeV bins for the reconstructed energy and 40~MeV bins for the
+true neutrino energy.  Four migration matrices (for
+$\nu_e,\bar\nu_e,\nu_\mu,\bar\nu_\mu$) are applied to signal events as
+well as backgrounds. As suggested from Fig.~\ref{fig:QE-Energy} the 
+results using migration matrices are very similar to a Gaussian
+energy resolution.
+
+\begin{figure}[!t]
+  \centering
+  \includegraphics[width=0.65\textwidth]{./fig2.eps}
+  \mycaption{\label{fig:QE-Energy} Energy resolution for \nue\
+  interactions in the 200--300~MeV energy range. The quantity
+  displayed is the difference between the reconstructed and the true
+  neutrino energy.}
+\end{figure}
+
+Backgrounds from charged pions and atmospheric neutrinos are computed
+with the identical analysis chain as signal events.
+Charged pions generated in NC events (or in NC-like events where the
+leading electron goes undetected) are the main source of background for
+the experiment. To compute this background inclusive NC and CC events
+have been generated with the \BB\ spectrum. Events have been selected
+where the only visible track is a charged pion above the \v{C}erenkov
+threshold. Particle identification efficiencies have been applied to
+those particles. The probability for a pion to survive in water until
+its decay has been computed with Geant~3.21 and cross-checked with a
+Fluka~2003 simulation. This probability is different for positive and
+negative pions, the latter having a higher probability to be absorbed
+before decaying. The surviving events are background, and the
+reconstructed neutrino energy is computed misidentifying these pions
+as muons. Event rates are reported in Tab.~\ref{tab:sigbck}. From
+these numbers it becomes evident that requiring the detection of the
+Michel electron provides an efficient cut to eliminate the pion
+background.
+%
+These background rates are significantly smaller than quoted in
+Ref.~\cite{MyNufact04}, where pion decays were computed with the
+same probabilities as for muons and they are slightly different
+from those quoted in Ref.~\cite{ MezzettoNuFact05}, where an
+older version of Nuance had been used.
+%
+The numbers of Tab.~\ref{tab:sigbck} have been cross-checked by
+comparing the Nuance and Neugen~\cite{Neugen} event
+generators, finding a fair agreement in background rates and energy shape.
+
+\begin{table}[t]
+     \centering
+     \begin{tabular}{l@{\qquad}rrr@{\qquad}rrr}
+     \hline\noalign{\smallskip}
+       & \multicolumn{3}{ c }{\Ne} & \multicolumn{3}{c}{\He} \\
+     \hline\noalign{\smallskip}
+       & \numu CC & $\pi^+$ & $\pi^-$ & \nubarmu CC & $\pi^+$ & $\pi^-$ \\
+     \hline\noalign{\smallskip}
+      Generated ev.\ & 115367   &  557   &  341 & 101899 &  674   &  400 \\
+      Particle ID    &  95717   &  204   &  100 & 85285  &  240   &  118 \\
+      Decay          &  61347   &  107   &    8 & 69242  &  120   &    8 \\
+\hline\noalign{\smallskip}
+    \end{tabular}
+    \mycaption{\label{tab:sigbck} Events for the \BB\ in a 4400~kt~yr
+    exposure.  \numu(\nubarmu) CC events are computed assuming full
+    oscillations ($P_{\nu_e\to\nu_\mu} = 1$), and pion backgrounds are
+    computed from \nue(\nubare) CC+NC events. In the rows we give the
+    number events generated within the fiducial volume (``Generated
+    ev.''), after muon particle identification (``Particle ID''), and
+    after applying a further identification requiring the detection of
+    the Michel electron (``Decay''). }
+\end{table}
+
+Also atmospheric neutrinos can constitute an important source of
+background~\cite{zucchelli,JJHigh2,JJHigh1,MezzettoNuFact05}. This
+background can be suppressed only by keeping a very short duty cycle
+($2.2 \cdot 10^{-3}$ is the target value for the \BB\ design study),
+and this in turn is one of the most challenging bounds on the design
+of the Beta Beam complex. Following Ref.~\cite{MezzettoNuFact05} we
+include the atmospheric neutrino background based on a Monte Carlo
+simulation using Nuance. Events are reconstructed as if they were
+signal neutrino events. We estimate that 5 events/year would survive
+the analysis chain in a full solar year (the \BB\ should run for about
+1/3 of this period) and include these events as backgrounds in the
+analysis. Under these circumstances, the present value of the \BB\
+duty cycle seems to be an overkill, it could be reduced by a factor 5
+at least, see also Ref.~\cite{MezzettoNuFact05} for a discussion of
+the effect of a higher duty cycle.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The $3.5$-GeV SPL Super Beam}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
+In the recent Conceptual Design Report 2 (CDR2) the foreseen Super
+Proton Linac (SPL)~\cite{SPL} will provide the protons for the muon
+production in the context of a Neutrino Factory, and at a first stage
+will feed protons to a fixed target experiment to produce an intense
+conventional neutrino beam (``Super Beam''). The parameters of the
+beam line take into account the optimization~\cite{Campagne:2004wt} of
+the beam energy as well as the secondary particle focusing and decay
+to search for $\nu_\mu \rightarrow \nu_e$ and $\bar{\nu}_\mu
+\rightarrow \bar{\nu}_e$ appearance as well as $\nu_\mu$,
+$\bar\nu_\mu$ disappearance in a mega ton scale water \v{C}erenkov
+detector. In particular, a full simulation of the beam line from the
+proton on target interaction up to the secondary particle decay tunnel
+has been performed. The proton on a liquid mercury target (30~cm long,
+$7.5$~mm radius, 13.546 density) has been simulated with
+FLUKA~2002.4~\cite{FLUKA} while the horn focusing system and the decay
+tunnel simulation has been preformed with
+GEANT~3.21~\cite{GEANT}.\footnote{Although there are differences
+between the predicted pion and kaon productions as a function of
+proton kinetic energy with FLUKA~2002.4 and 2005.6, the results are
+consistent for the relevant energy of 3.5~GeV. We emphasize that the
+pion and the kaon production cross-sections are waiting for
+experimental confirmation~\cite{HARP-MINERVA} and a new optimization
+would be required if their is a disagreement with the present
+knowledge.}
+
+\begin{figure}[!t]
+  \centering 
+  \includegraphics[width=0.65\textwidth]{./fig3.eps}
+  \mycaption{\label{fig:fluxSPLContrib} Neutrino fluxes, at $130$~km
+  from the target with the horns focusing the positive particles
+  (top panel) or the negative particles (bottom panel). The fluxes are
+  computed for a SPL proton beam of $3.5$~GeV (4~MW), a decay tunnel
+  with a length of $40$~m and a radius of $2$~m.}
+\end{figure}
+
+Since the optimization requirements for a Neutrino Factory are rather
+different than for a Super Beam the new SPL configuration has a
+significant impact on the physics performance (see
+Ref.~\cite{Campagne:2004wt} for a detailed discussion).  The SPL
+fluxes of the four neutrino species ($\nu_\mu$, $\nu_e$,
+$\bar{\nu}_\mu$, $\bar{\nu}_e$) for the positive ($\nu_\mu$ beam) and
+the negative focusing ($\bar{\nu}_\mu$ beam) are show in
+Fig.~\ref{fig:fluxSPLContrib}.  The total number of $\nu_\mu$
+($\bar{\nu}_\mu$) in positive (negative) focusing is about
+$1.18\,(0.97) \times 10^{12}\:\mathrm{m}^{-2}\mathrm{y}^{-1}$ with an
+average energy of $300$~MeV. The $\nu_e$ ($\bar{\nu}_e$) contamination
+in the $\nu_\mu$ ($\bar\nu_\mu$) beam is around $0.7\%$
+($6.0\%$). Following Ref.~\cite{Mezzetto:2003mm}, the $\pi^o$
+background is reduced using a tighter PID cut compared to standard
+Super-Kamiokande analysis. The Michel electron is required for the
+$\mu$ identification.
+%
+For the $\nu_\mu \rightarrow \nu_e$ channel the background consists
+roughly of 90\% $\nu_e \rightarrow \nu_e$ CC interactions, 6\% $\pi^o$
+from NC interactions, 3\% miss identified muons from $\nu_\mu
+\rightarrow \nu_\mu$ CC, and 1\% $\bar{\nu}_e \rightarrow \bar{\nu}_e$
+CC interactions. For the $\bar{\nu}_\mu \rightarrow \bar{\nu}_e$
+channel the contributions to the background are 45\% $\bar{\nu}_e
+\rightarrow \bar{\nu}_e$ CC interactions, 35\% $\nu_e \rightarrow
+\nu_e$ CC interactions, 18\% $\pi^o$ from NC interactions and 2\% miss
+identified muons from $\bar{\nu}_\mu \rightarrow \bar{\nu}_\mu$ CC.
+In addition we include the events from the contamination of 
+``wrong sign'' muon-neutrinos due to $\bar\nu_\mu \to \bar\nu_e$
+($\nu_\mu \to \nu_e$) oscillations in the neutrino (antineutrino)
+mode. 
+%
+We have checked that with the envisaged duty cycle of $2.4\times
+10^{-4}$ the background from atmospheric neutrinos is negligible for
+the SPL.
+
+\begin{figure}[!t]
+  \centering
+  \includegraphics[width=0.5\textwidth]{./fig4.eps}
+%
+  \mycaption{\label{fig:fluxComparison} 
+  Comparison of the fluxes from SPL and \BB.}
+\end{figure}
+
+Considering the signal over square-root of background
+ratio, the $3.5$~GeV beam energy is more favorable than the original
+$2.2$~GeV option. Compared to the fluxes used in
+Refs.~\cite{Mezzetto:2003mm,Donini:2004hu} the gain is at least a
+factor $2.5$ and this justifies to reconsider in detail the physics
+potential of the SPL Super Beam.
+%
+Both the appearance and the disappearance channels are used. For the
+spectral analysis we use 10 bins of 100~MeV in the interval $0 < E_\nu
+< 1$~GeV, applying the same migration matrices as for the \BB\ to take
+into account properly the neutrino energy reconstruction. As ultimate
+goal suggested in Ref.~\cite{T2K} a 2\% systematical error is used as
+default both for signal and background, this would be achieved by a
+special care of the design of the close position. However, we discuss
+also how a 5\% systematical error affects the sensitivities.
+%
+Using neutrino cross-sections on water from Ref.~\cite{Nuance}, the
+number of expected $\nu_\mu$ charged current is about $98$ per
+kt~yr. In Fig.~\ref{fig:fluxComparison} we compare the fluxes from the
+SPL to the one from the \BB.
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The atmospheric neutrino analysis}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:atm-details}
+
+The simulation of atmospheric neutrino data in MEMPHYS is based on the
+analysis presented in Ref.~\cite{Huber:2005ep}, with the following
+differences:
+%
+\begin{itemize}
+  \item We replace the neutrino fluxes at Kamioka with those at Gran
+    Sasso. We use the Honda calculations~\cite{Honda:2004yz}, which
+    unfortunately are not yet available for the Fr\'ejus
+    site. However, since the fluxes increase with the geomagnetic
+    latitude and Fr\'ejus is northern than Gran Sasso, our choice is
+    conservative.
+    
+  \item We take into account the specific geometry of the MEMPHYS
+    detector. This is particularly important to properly separate
+    fully contained from partially contained events, as well as
+    stopping muon from through-going muon events.
+    
+  \item We divide our total data sample into 420 different bins:
+    fully contained single-ring events, further subdivided according
+    to flavor ($e$-like or $\mu$-like), lepton momentum (8 bins:
+    0.1--0.3, 0.3--0.5, 0.5--1, 1--2, 2--3, 3--5, 5--8,
+    8--$\infty$~GeV) and lepton direction (20 bins in zenith angle);
+%
+    fully contained multi-ring events, further subdivided according to
+    flavor ($e$-like or $\mu$-like), reconstructed neutrino energy (3
+    bins: 0--1.33, 1.33--5, 5--$\infty$~GeV) and lepton direction (10
+    bins in zenith angle);
+%    	
+    partially contained $\mu$-like events, divided into 20 zenith bins;
+%	
+    up-going muons, divided into stopping and through-going events, and in
+    10 zenith bins each.
+
+    \item We include in our calculations the neutral-current
+      contamination of each bin. To this extent we assume that the
+      ratio between neural-current and \emph{unoscillated}
+      charged-current events in MEMPHYS is the same as in
+      Super-Kamiokande, and we take this ratio from
+      Ref.~\cite{Ashie:2005ik}.
+      
+    \item We consider also multi-ring events, which we define
+      as fully contained charged-current events which are \emph{not}
+      tagged as single-ring. Again, we assume that the survival
+      efficiency and the NC contamination are the same as for
+      Super-Kamiokande~\cite{Ashie:2005ik}.
+\end{itemize}
+
+The expected number of contained events is given by:
+%
+\begin{multline} \label{eq:contained}
+    N_b(\vec\omega) = N_b^\text{NC} +
+    n_\text{tgt} T \sum_{\alpha,\beta,\pm}
+    \int_0^\infty dh \int_{-1}^{+1} dc_\nu
+    \int_{\Emin}^\infty dE_\nu \int_{\Emin}^{E_\nu} dE_l
+    \int_{-1}^{+1} dc_a \int_0^{2\pi} d\varphi_a
+    \\
+    \frac{d^3 \Phi_\alpha^\pm}{dE_\nu \, dc_\nu \, dh}(E_\nu, c_\nu, h)
+    \, P_{\alpha\to\beta}^\pm(E_\nu, c_\nu, h \,|\, \vec\omega)
+    \, \frac{d^2\sigma_\beta^\pm}{dE_l \, dc_a}(E_\nu, E_l, c_a)
+    \, \varepsilon_\beta^b(E_l, c_l(c_\nu, c_a, \varphi_a))
+    \,,
+\end{multline}
+%
+where $P_{\alpha\to\beta}^+$ ($P_{\alpha\to\beta}^-$) is the
+$\nu_\alpha \to \nu_\beta$ ($\bar{\nu}_\alpha \to \bar{\nu}_\beta$)
+conversion probability for given values of the neutrino energy
+$E_\nu$, the cosine $c_\nu$ of the angle between the incoming neutrino
+and the vertical direction, the production altitude $h$, and the
+neutrino oscillation parameters $\vec\omega$. We calculate the
+conversion probability numerically in the general three-flavor
+framework taking into account matter effects from a realistic Earth
+density profile. Further, $N_b^\text{NC}$ is the neutral-current
+background for the bin $b$, $n_\text{tgt}$ is the number of targets,
+$T$ is the experiment running time, $\Phi_\alpha^+$ ($\Phi_\alpha^-$)
+is the flux of atmospheric neutrinos (antineutrinos) of type $\alpha$,
+and $\sigma_\beta^+$ ($\sigma_\beta^-$) is the charged-current
+neutrino- (antineutrino-) nucleon interaction cross section.
+%
+The variable $E_l$ is the energy of the final lepton of type $\beta$,
+while $c_a$ and $\varphi_a$ parametrize the opening angle between the
+incoming neutrino and the final lepton directions as determined by the
+kinematics of the neutrino interaction.
+%
+Finally, $\varepsilon_\beta^b$ gives the probability that a charged
+lepton of type $\beta$, energy $E_l$ and direction $c_l$ contributes
+to the bin $b$.
+
+Up-going muon events are calculated as follows:
+%
+\begin{multline} \label{eq:upgoing}
+    N_b(\vec\omega) = \rho_\text{rock} T \sum_{\alpha,\pm} 
+    \int_0^\infty dh \int_{-1}^{+1} dc_\nu
+    \int_{\Emin}^\infty dE_\nu 
+    \int_{\Emin}^{E_\nu} dE^0_\mu \int_{\Emin}^{E^0_\mu} d\Efin_\mu
+    \int_{-1}^{+1} dc_a \int_0^{2\pi} d\varphi_a
+    \\
+    \frac{d^3 \Phi_\alpha^\pm}{dE_\nu \, dc_\nu \, dh}(E_\nu, c_\nu, h)
+    \, P_{\alpha\to\mu}^\pm(E_\nu, c_\nu, h \,|\, \vec\omega)
+    \, \frac{d^2\sigma_\mu^\pm}{dE^0_\mu \, dc_a}(E_\nu, dE^0_\mu, c_a)
+    \\
+    \times R_\text{rock}(E^0_\mu,\Efin_\mu)
+    \, \mathcal{A}_\text{eff}^b(\Efin_\mu,
+    c_l(c_\nu, c_a, \varphi_a)) \,,
+\end{multline}
+%
+where $\rho_\text{rock}$ is the density of targets in standard rock,
+$R_\text{rock}$ is the effective muon range~\cite{Lipari:1991ut} for a
+muon which is produced with energy $E^0_\mu$ and reaches the detector
+with energy $\Efin_\mu$, and $\mathcal{A}_\text{eff}^b$ is the
+effective area for the bin $b$. The other variables and physical
+quantities are the same as for contained events.
+
+The statistical analysis is based on the pull method, as described in
+Ref.~\cite{Gonzalez-Garcia:2004wg}. In our analysis we include three
+different kind of experimental uncertainties:
+%
+Flux uncertainties: total normalization (20\%), tilt factor (5\%),
+zenith angle (5\%), $\nu/\bar\nu$ ratio (5\%), and $\mu/e$ ratio
+(5\%);
+%    
+cross-section uncertainties: total normalization (15\%) and $\mu/e$
+ratio (1\%) for each type of charged-current interaction
+(quasi-elastic, one-pion production, and deep-inelastic scattering),
+and total normalization (15\%) for the neutral-current contributions;
+%    
+systematic uncertainties: same as in previous analyses, details are
+given in the Appendix of Ref.~\cite{Gonzalez-Garcia:2004wg}. In
+addition, we assume independent normalization uncertainties (20\%) for
+$e$-like and $\mu$-like multi-ring events.
+%
+Since we are dividing our data sample into a large number of bins, it
+is important to use Poisson statistics as some of the bins contain
+only a few number of events. We therefore write our $\chi^2$ as:
+%
+\begin{equation} \label{eq:poisson}
+    \chi^2(\vec\omega) = \min_{\vec\xi} \left[ 2 \sum_b \left(
+    N_b^\text{th}(\vec\omega,\, \vec\xi)
+    - N_b^\text{ex} + N_b^\text{ex} \ln\frac{N_b^\text{ex}}
+    {N_b^\text{th}(\vec\omega,\, \vec\xi)} \right) 
+    + \sum_n \xi_n^2 \right] \,,
+\end{equation}
+%
+where the number of events for a given value of the pulls $\vec\xi$ is
+given by:
+%
+\begin{equation} \label{eq:theopulls}
+    N_b^\text{th}(\vec\omega,\, \vec\xi) = N_b^\text{th}(\vec\omega) \,
+    \exp\left( \sum_n \pi_b^n(\vec\omega)\, \xi_n \right) \,.
+\end{equation}
+%
+The use of an exponential dependence on the pulls in
+Eq.~\eqref{eq:theopulls}, rather than the usual linear dependence,
+ensures that the theoretical predictions remain positive for
+\emph{any} value of the pulls, thus avoiding numerical inconsistencies
+during the pull minimization procedure.
+
+ 
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Degeneracies}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:degeneracies}
+
+
+A characteristic feature in the analysis of future LBL experiments is
+the presence of {\it parameter degeneracies}.  Due to the inherent
+three-flavor structure of the oscillation probabilities, for a given
+experiment in general several disconnected regions in the
+multi-dimensional space of oscillation parameters will be
+present. Traditionally these degeneracies are referred to in the
+following way:
+%
+\begin{itemize}
+\item
+The {\it intrinsic} or
+($\delCP,\theta_{13}$)-degeneracy~\cite{Burguet-Castell:2001ez}:
+For a measurement based on the $\nu_\mu \to \nu_e$ oscillation probability for
+neutrinos and antineutrinos two disconnected solutions appear in the
+($\delCP,\theta_{13}$) plane.
+\item
+The {\it hierarchy} or sign($\Delta
+m^2_{31}$)-degeneracy~\cite{Minakata:2001qm}: The two solutions
+corresponding to the two signs of $\Delta m^2_{31}$ appear in general
+at different values of $\delCP$ and $\theta_{13}$.
+\item
+The {\it octant} or $\theta_{23}$-degeneracy~\cite{Fogli:1996pv}:
+Since LBL experiments are sensitive mainly to $\sin^22\theta_{23}$ it
+is difficult to distinguish the two octants $\theta_{23} < \pi/4$ and
+$\theta_{23} > \pi/4$.  Again, the solutions corresponding to
+$\theta_{23}$ and $\pi/2 - \theta_{23}$ appear in general at different
+values of $\delCP$ and $\theta_{13}$.
+\end{itemize}
+%
+This leads to an eight-fold ambiguity in $\theta_{13}$ and
+$\delCP$~\cite{Barger:2001yr}, and hence degeneracies provide a
+serious limitation for the determination of $\theta_{13}$, $\delCP$,
+and the sign of $\Delta m^2_{31}$. Recent discussions of degeneracies
+can be found for example in
+Refs.~\cite{Huber:2002mx,Huber:2005ep,Yasuda:2004gu,Ishitsuka:2005qi};
+degeneracies in the context of CERN--Fr\'ejus \BB\ and SPL have been
+considered previously in Ref.~\cite{Donini:2004hu}.
+%
+In Fig.~\ref{fig:degeneracies} we illustrate the effect of
+degeneracies for the \BB, SPL, and T2HK experiments. Assuming the
+true parameter values $\delta_\mathrm{CP} = -0.85 \pi$,
+$\sin^22\theta_{13} = 0.03$, $\sin^2\theta_{23} = 0.6$ we show the
+allowed regions in the plane of $\stheta$ and $\delCP$ taking into
+account the solutions with the wrong hierarchy and the wrong octant of
+$\theta_{23}$.
+
+\begin{figure}[!t]
+\centering
+\includegraphics[width=0.95\textwidth]{./fig5.eps}
+%
+  \mycaption{Allowed regions in $\sin^22\theta_{13}$ and
+  $\delta_\mathrm{CP}$ for LBL data alone (contour lines) and LBL+ATM
+  data combined (colored regions). $\mathrm{H^{tr/wr} (O^{tr/wr})}$
+  refers to solutions with the true/wrong mass hierarchy (octant of
+  $\theta_{23}$). The true parameter values are $\delta_\mathrm{CP} =
+  -0.85 \pi$, $\sin^22\theta_{13} = 0.03$, $\sin^2\theta_{23} = 0.6$,
+  and the values from Eq.~(\ref{eq:default-params}) for the other
+  parameters.}
+\label{fig:degeneracies}
+\end{figure}
+
+
+\begin{figure}[!t]
+\centering
+\includegraphics[width=0.9\textwidth]{./fig6.eps}
+%
+  \mycaption{Resolving degeneracies in SPL by successively using the
+  appearance rate measurement, disappearance channel rate and
+  spectrum, spectral information in the appearance channel, and
+  atmospheric neutrinos.  Allowed regions in $\sin^22\theta_{13}$ and
+  $\delta_\mathrm{CP}$ are shown at 95\%~CL, and $\mathrm{H^{tr/wr}
+  (O^{tr/wr})}$ refers to solutions with the true/wrong mass hierarchy
+  (octant of $\theta_{23}$). The true parameter values are
+  $\delta_\mathrm{CP} = -0.85 \pi$, $\sin^22\theta_{13} = 0.03$,
+  $\sin^2\theta_{23} = 0.6$, and the values from
+  Eq.~(\ref{eq:default-params}) for the other parameters.}
+\label{fig:degeneracies_SPL}
+\end{figure}
+
+As visible in Fig.~\ref{fig:degeneracies} for the
+Super Beam experiments SPL and T2HK there is only a four-fold
+degeneracy related to sign($\Delta m^2_{31}$) and the octant of
+$\theta_{23}$, whereas the intrinsic degeneracy can be resolved. 
+%
+Several pieces of information contribute to this effect, as we
+illustrate at the example of SPL in Fig.~\ref{fig:degeneracies_SPL}.
+The dashed curves in the left panel of this figure show the allowed
+regions for only the appearance measurement (for neutrinos and
+antineutrinos) without spectral information, i.e., just a counting
+experiment. In this case the eight-fold degeneracy is present in its
+full beauty, and one finds two solutions (corresponding to the
+intrinsic degeneracy) for each choice of sign($\Delta m^2_{31}$) and
+the octant of $\theta_{23}$. Moreover, the allowed regions are
+relatively large. For the thin solid curves the information from the
+disappearance rate is added. The main effect is to decrease the size
+of the allowed regions in $\stheta$. This is especially pronounced for
+the solutions involving the wrong octant of $\theta_{23}$, since these
+solutions are strongly affected by an uncertainty in $\theta_{23}$
+which gets reduced by the disappearance information. Using in addition
+to the disappearance rate also the spectrum again decreases the size
+of the allowed regions, however, still all eight solutions are present
+(compare dashed curves in the right panel).
+%
+The most relevant effect comes from the inclusion of spectral
+information in the appearance channel, as visible from the comparison
+of the dashed and thick-solid curves in the right panel of
+Fig.~\ref{fig:degeneracies_SPL}. The intrinsic degeneracy gets
+resolved and only four solutions corresponding to the sign and octant
+degeneracies are left.\footnote{The inclusion of spectral information
+might be the source of possible differences to previous studies, see
+e.g.\ Ref.~\cite{Donini:2004hu}.} Note that the thick curves in the
+right panel of Fig.~\ref{fig:degeneracies_SPL} correspond to the
+regions show in Fig.~\ref{fig:degeneracies} for the SPL.
+%
+Finally, by the inclusion of information from atmospheric neutrinos
+all degeneracies can be resolved in this example, and the true
+solution is identified at 95\%~CL (see Sec.~\ref{sec:atmospherics} and
+Ref.~\cite{Huber:2005ep} for further discussions of atmospheric
+neutrinos).
+
+Concerning the \BB\ one observes from Fig.~\ref{fig:degeneracies} that
+in this case the ($\delCP,\theta_{13}$)-degeneracy cannot be resolved
+and one has to deal with eight distinct solutions. One reason for this
+is the absence of precise information on $|\Delta m^2_{31}|$ and
+$\sin^22\theta_{23}$ which is provided by the $\nu_\mu$ disappearance
+in Super Beam experiments but is not available from the \BB. If
+external information on these parameters at the level of 3\% is
+included the allowed regions in Fig.~\ref{fig:degeneracies} are
+significantly reduced. However, still all eight solutions are present,
+which indicates that for the \BB\ spectral information is not
+efficient enough to resolve the ($\delCP,\theta_{13}$)-degeneracy, and
+in this case only the inclusion of atmospheric neutrino data allows a
+nearly complete resolution of the degeneracies.
+
+An important observation from Fig.~\ref{fig:degeneracies} is that
+degeneracies have only a very small impact on the CP violation
+discovery, in the sense that if the true solution is CP violating also
+the fake solutions are located at CP violating values of
+$\delCP$. Indeed, since for the relatively short baselines in the
+experiments under consideration matter effects are very small, the
+sign($\Delta m^2_{31}$)-degenerate solution is located within good
+approximation at $\delCP' \approx \pi -
+\delCP$~\cite{Minakata:2001qm}. Therefore, although degeneracies
+strongly affect the determination of $\theta_{13}$ and $\delCP$ they
+have only a small impact on the CP violation discovery potential.
+Furthermore, as clear from Fig.~\ref{fig:degeneracies} the sign($\Delta
+m^2_{31}$) degeneracy has practically no effect on the $\theta_{13}$
+measurement, whereas the octant degeneracy has very little impact on
+the determination of $\delCP$.
+
+\begin{figure}[!t]
+\centering
+\includegraphics[width=0.9\textwidth]{./fig7.eps}
+%
+  \mycaption{Allowed regions in $\sin^22\theta_{13}$ and
+  $\delta_\mathrm{CP}$ for 5~years data (neutrinos only) from \BB,
+  SPL, and the combination. $\mathrm{H^{tr/wr} (O^{tr/wr})}$ refers to
+  solutions with the true/wrong mass hierarchy (octant of
+  $\theta_{23}$). For the colored regions in the left panel also
+  5~years of atmospheric data are included; the solution with the
+  wrong hierarchy has $\Delta\chi^2 = 4$. The true parameter
+  values are $\delta_\mathrm{CP} = -0.85 \pi$, $\sin^22\theta_{13} =
+  0.03$, $\sin^2\theta_{23} = 0.6$, and the values from
+  Eq.~(\ref{eq:default-params}) for the other parameters. For the \BB\
+  only analysis (middle panel) an external accuracy of 2\% (3\%) for
+  $|\Delta m^2_{31}|$ ($\theta_{23}$) has been assumed, whereas for
+  the left and right panel the default value of 10\% has been used.}
+\label{fig:degeneracies_5yrs}
+\end{figure}
+
+Fig.~\ref{fig:degeneracies} shows also that the fake solutions occur
+at similar locations in the ($\stheta$, $\delCP$) plane for \BB\ and
+SPL. Therefore, as noted in Ref.~\cite{Donini:2004hu}, in this sense
+the two experiments are not complementary, and the combination of
+10~years of \BB\ and SPL data is not very effective in resolving
+degeneracies. This is obvious since the baseline is the same and the
+neutrino energies are similar.
+%
+Note however, that the \BB\ looks for $\nu_e\to\nu_\mu$ appearance,
+whereas in SPL the T-conjugate channel $\nu_\mu\to\nu_e$ is observed.
+Assuming CPT invariance the relation $P_{\nu_\alpha\to\nu_\beta} =
+P_{\bar\nu_\beta\to\bar\nu_\alpha}$ holds, which implies that the
+antineutrino measurement can be replaced by a measurement in the
+T-conjugate channel.  Hence, if \BB\ and SPL experiments are available
+simultaneously the full information can be obtained just from neutrino
+data, and in principle the (time consuming) antineutrino measurement 
+is not necessary. As shown in Fig.~\ref{fig:degeneracies_5yrs} the
+combination of 5~yrs neutrino data from the \BB\ with 5~yrs of
+neutrino data from SPL leads to a result very close to the 10~yrs
+neutrino+antineutrino data from one experiment alone. Hence, if \BB\
+and SPL experiments are available simultaneously the data taking
+period is reduced approximately by a factor of 2 with respect to a
+single experiment. This synergy is discussed later in
+Sec.~\ref{sec:synergies-beams} in the context of the $\theta_{13}$ and
+CP violation discovery potentials.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Physics potential}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:sensitivities}
+
+\subsection{Sensitivity to the atmospheric parameters}
+\label{sec:atm}
+
+The $\nu_\mu$ disappearance channel available in the Super Beam
+experiments SPL and T2HK allows a precise determination of the
+atmospheric parameters $|\Delta m^2_{31}|$ and $\sin^22\theta_{23}$,
+see, e.g., Refs.~\cite{Antusch:2004yx,Minakata:2004pg,Donini:2005db}
+for recent analyses). Fig.~\ref{fig:atm-params} illustrates the
+improvement on these parameters by Super Beam experiments with respect
+to the present knowledge from SK atmospheric and K2K data. We show the
+allowed regions at 99\%~CL for T2K-I, SPL, and T2HK, where in all
+three cases 5~years of neutrino data are assumed. T2K-I corresponds to
+the phase~I of the T2K experiment with a beam power of 0.77~MW and the
+Super-Kamiokande detector as target~\cite{T2K}. In Tab.~\ref{tab:atm-params} we
+give the corresponding relative accuracies at 3$\sigma$ for $|\Delta
+m^2_{31}|$ and $\sin^2\theta_{23}$.
+
+\begin{figure}[!t]
+\centering
+  \includegraphics[width=0.55\textwidth]{./fig8.eps}
+  \mycaption{\label{fig:atm-params} Allowed regions of $\Delta
+  m^2_{31}$ and $\sin^2\theta_{23}$ at 99\%~CL (2 d.o.f.)  after 5~yrs
+  of neutrino data taking for SPL, T2K phase~I, T2HK, and the
+  combination of SPL with 5~yrs of atmospheric neutrino data in the
+  MEMPHYS detector. For the true parameter values we use $\Delta
+  m^2_{31} = 2.2\, (2.6) \times 10^{-3}~\mathrm{eV}^2$ and
+  $\sin^2\theta_{23} = 0.5 \, (0.37)$ for the test point 1 (2), and
+  $\theta_{13} = 0$ and the solar parameters as given in
+  Eq.~(\ref{eq:default-params}). The shaded region corresponds to the
+  99\%~CL region from present SK and K2K data~\cite{Maltoni:2004ei}.}
+\end{figure}
+
+
+\begin{table}[!t]
+  \centering
+  \begin{tabular}{lcrrr}
+  \hline\noalign{\smallskip}
+    & True values  & T2K-I & SPL & T2HK \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  $\Delta m^2_{31}$   & $2.2\cdot 10^{-3}$ eV$^2$ & 4.7\% & 3.2\% & 1.1\% \\
+  $\sin^2\theta_{23}$ & $0.5$                     & 20\%  & 20\%  & 6\%   \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  $\Delta m^2_{31}$   & $2.6\cdot 10^{-3}$ eV$^2$ & 4.4\% & 2.5\% & 0.7\% \\
+  $\sin^2\theta_{23}$ & $0.37$                    & 8.9\% & 3.1\% & 0.8\% \\
+  \noalign{\smallskip}\hline
+  \end{tabular}
+  \mycaption{Accuracies at $3\sigma$ on the atmospheric parameters
+  $|\Delta m^2_{31}|$ and $\sin^2\theta_{23}$ for 5 years of neutrino
+  data from T2K-I, SPL, and T2HK for the two test points shown in
+  Fig.~\ref{fig:atm-params} ($\theta^\mathrm{true}_{13} = 0$). The
+  accuracy for a parameter $x$ is defined as $(x^\mathrm{upper} -
+  x^\mathrm{lower})/(2 x^\mathrm{true})$, where $x^\mathrm{upper}$
+  ($x^\mathrm{lower}$) is the upper (lower) bound at 3$\sigma$ for
+  1~d.o.f.\ obtained by projecting the contour $\Delta \chi^2 = 9$
+  onto the $x$-axis. For the accuracies for test point~2 the octant
+  degenerate solution is neglected.\label{tab:atm-params}}
+\end{table}
+
+From the figure and the table it becomes evident that the T2K setups
+are very good in measuring the atmospheric parameters, and only a
+modest improvement is possible with SPL with respect to T2K phase~I.
+T2HK provides an excellent sensitivity for these parameters, and for
+the example of the test point~2 sub-percent accuracies are obtained at
+3$\sigma$. The disadvantage of SPL with respect to T2HK is the
+limited spectral information. Because of the lower beam energy
+nuclear Fermi motion is a severe limitation for energy reconstruction
+in SPL, whereas in T2K the somewhat higher energy allows an efficient
+use of spectral information of quasi-elastic events. Indeed, due to
+the large number of events in the disappearance channel (cf.\
+Tab.~\ref{tab:events}) the measurement is completely dominated by the
+spectrum, and even increasing the normalization uncertainty up to
+100\% has very little impact on the allowed regions. The effect of
+spectral information on the disappearance measurement is
+discussed in some detail in Ref.~\cite{Donini:2005db}.
+
+For the test point~1, with maximal mixing for $\theta_{23}$, rather
+poor accuracies of $\sim20\%$ for T2K-I and SPL, and $6\%$ for T2HK
+are obtained for $\sin^2\theta_{23}$. The reason is that in the
+disappearance channel $\sin^22\theta_{23}$ is measured with high
+precision, which translates to rather large errors for
+$\sin^2\theta_{23}$ if $\theta_{23} = \pi/4$~\cite{Minakata:2004pg}.
+%
+For the same reason it is difficult to resolve the octant degeneracy,
+and for the test point~2, with a non-maximal value of
+$\sin^2\theta_{23} = 0.37$, for all three LBL experiments the
+degenerate solution is present around $\sin^2\theta_{23} = 0.63$.
+%
+As pointed out in Refs.~\cite{Peres:2003wd,Gonzalez-Garcia:2004cu}
+atmospheric neutrino data may allow to distinguish between the two
+octants of $\theta_{23}$. If 5~years of atmospheric neutrino data in
+MEMPHYS are added to the SPL data, the degenerate solution for the
+test point~2 can be excluded at more than $5\sigma$ and hence the
+octant degeneracy is resolved in this example, see
+Sec.~\ref{sec:atmospherics} for a more detailed discussion.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The $\theta_{13}$ discovery potential}
+\label{sec:th13}
+
+If no finite value of $\theta_{13}$ is discovered by the next round of
+experiments an important task of the experiments under consideration
+here is to push further the sensitivity to this parameter. In this
+section we address this problem, where we use to following definition
+of the $\theta_{13}$ discovery potential: Data are simulated for a
+finite true value of $\stheta$ and a given true value for $\delCP$. If
+the $\Delta\chi^2$ of the fit to these data with $\theta_{13} = 0$ is
+larger than 9 the corresponding true value of $\theta_{13}$ ``is
+discovered at 3$\sigma$''. In other words, the $3\sigma$ discovery
+limit as a function of the true $\delCP$ is given by the true value of
+$\stheta$ for which $\Delta\chi^2(\theta_{13}=0) = 9$. In the fitting
+process we minimize the $\Delta\chi^2$ with respect to $\theta_{12}$,
+$\theta_{23}$, $\Delta m^2_{12}$, and $\Delta m^2_{31}$, and in
+general one has to test also for degenerate solutions in sign($\Delta
+m^2_{31}$) and the octant of $\theta_{23}$.
+
+\begin{figure}
+  \centering \includegraphics[width=0.9\textwidth]{./fig9.eps}
+  \mycaption{$3\sigma$ discovery sensitivity to $\stheta$ for \BB,
+  SPL, and T2HK as a function of the true value of \delCP\ (left
+  panel) and as a function of the fraction of all possible values of
+  \delCP\ (right panel). The width of the bands corresponds to values
+  for the systematical errors between 2\% and 5\%. The black curves
+  correspond to the combination of \BB\ and SPL with 10~yrs of total
+  data taking each for a systematical error of 2\%, and the dashed
+  curves show the sensitivity of the \BB\ when the number of ion
+  decays/yr are reduced by a factor of two with respect to the values
+  given in Tab.~\ref{tab:setups}.\label{fig:th13}}
+\end{figure}
+
+The discovery limits are shown for \BB, SPL, and T2HK in
+Fig.~\ref{fig:th13}. One observes that SPL and T2HK are rather similar
+in performance, whereas the \BB\ with our standard fluxes performs
+significantly better. For all three facilities a guaranteed discovery
+reach of $\stheta \simeq 5\times 10^{-3}$ is obtained, irrespective of
+the actual value of \delCP, however, for certain values of \delCP\ the
+sensitivity is significantly improved. For SPL and T2HK discovery
+limits around $\stheta \simeq 10^{-3}$ are possible for a large
+fraction of all possible values of \delCP, whereas for our standard
+\BB\ a sensitivity below $\stheta = 4\times 10^{-4}$ is reached for
+80\% of all possible values of \delCP. If 10~years of data from \BB\
+and SPL are combined the discovery limit is dominated by the \BB.
+%
+Let us stress that the \BB\ performance depends crucially on the
+neutrino flux intensity, as can be seen from the dashed curves in
+Fig.~\ref{fig:th13}, which has been obtained by reducing the number of
+ion decays/yr by a factor of two with respect to our standard values
+given in Tab.~\ref{tab:setups}. In this case the sensitivity decreases
+significantly, but still values slightly better than from the
+Super Beam experiments are reached.
+
+In Fig.~\ref{fig:th13} we illustrate also the effect of systematical
+errors on the $\theta_{13}$ discovery reach. The lower boundary of the
+band for each experiment corresponds to a systematical error of 2\%,
+whereas the upper boundary is obtained for 5\%. These errors include
+the (uncorrelated) normalization uncertainties on the signal as well
+as on the background, where the crucial uncertainty is the error on
+the background. We find that the \BB\ is basically not affected by
+these errors, since the background has a rather different spectral
+shape (strongly peaked at low energies) than the signal. The fact
+that T2HK is relatively strongly affected by the actual value of the
+systematics can by understood by considering the ratio of signal to
+the square-root of the background using the numbers of
+Tab.~\ref{tab:events}. We shall discuss this issue in more detail in
+the next section in the context of the CP violation discovery reach.
+
+Let us remark that the $\theta_{13}$ sensitivities are practically not
+affected by the sign($\Delta m^2_{31}$)-degeneracy. This is easy to
+understand, since the data is fitted with $\theta_{13} = 0$, and in
+this case both mass hierarchies lead to very similar event rates. If
+the inverted hierarchy is used as the true hierarchy, the peak in the
+discovery limit visible in the left panel of Fig.~\ref{fig:th13}
+around $\delCP \sim \pi$ moves to $\delCP \sim 0$. However, the
+characteristic shape of the curves, and in particular, the sensitivity
+as a function of the \delCP-fraction shown in the right panel are
+hardly affected by the sign of the true $\Delta m^2_{31}$.
+%
+In case of a non-maximal value of $\theta_{23}$ the octant-degeneracy
+has a minor impact on the $\theta_{13}$ discovery potential, as
+illustrated in Fig.~\ref{fig:SPLTheta13Disco} for the SPL. We show the
+discovery limit obtained with the true and the fake octant of
+$\theta_{23}$ for a true value of $\sin^2\theta_{23}= 0.6$. Let us
+note that for true values of $\sin^2\theta_{23} > 0.5$ the
+octant-degenerate solution leads to a worse sensitivity to
+$\theta_{13}$ (see figure), whereas for $\sin^2\theta_{23} < 0.5$ the
+fake solution does not affect the $\theta_{13}$ discovery, since in
+this case the sensitivity is increased.
+
+\begin{figure}
+  \centering
+  \includegraphics[width=0.9\textwidth]{./fig10.eps}
+  \mycaption{\label{fig:SPLTheta13Disco} $3\sigma$ discovery
+  sensitivity to $\stheta$ for the SPL as a function of the true value
+  of \delCP\ for $\sin^2\theta_{23}^\mathrm{true} = 0.6$ and true values for
+  the other parameters as given in Eq.~(\ref{eq:default-params}).}
+\end{figure}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{Sensitivity to CP violation}
+\label{sec:CPV}
+
+In case a finite value of $\theta_{13}$ is established it is important
+to quantitatively assess the discovery potential for leptonic CP
+violation (CPV). The CP symmetry is violated if the complex phase
+\delCP\ is different from $0$ and $\pi$. Therefore, CPV is discovered
+if these values for \delCP\ can be excluded. 
+%
+We evaluate the discovery potential for CPV in the following way:
+Data are calculated by scanning the true values of $\stheta$ and
+$\delCP$. Then these data are fitted with the CP conserving values
+$\delCP = 0$ and $\delCP = \pi$, where all parameters except \delCP\
+are varied and the sign and octant degeneracies are taken into
+account. If no fit with $\Delta \chi^2 < 9$ is found CP conserving
+values of \delCP\ can be excluded at $3\sigma$ for the chosen values
+of $\delta_\mathrm{CP}^\mathrm{true}$ and $\stheta^\mathrm{true}$.
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.65\textwidth]{./fig11.eps}
+%   
+   \mycaption{CPV discovery potential for \BB, SPL, and T2HK: For
+   parameter values inside the ellipse-shaped curves CP conserving
+   values of \delCP\ can be excluded at $3\sigma$ $(\Delta\chi^2>9)$.
+   The width of the bands corresponds to values for the systematical
+   errors from 2\% to 5\%. The dashed curves show the sensitivity of
+   the \BB\ when the number of ion decays/yr are reduced by a factor
+   of two with respect to the values given in Tab.~\ref{tab:setups}
+   for 2\% systematics.\label{fig:CPV}}
+\end{figure}
+
+The CPV discovery potential for \BB, SPL, and T2HK is shown in
+Fig.~\ref{fig:CPV}. As in the case of the $\theta_{13}$ sensitivity we
+find that SPL and T2HK perform rather similar, whereas the \BB\ has
+significantly better sensitivity if our adopted numbers of ion decays
+per year can be achieved. For systematical errors of 2\% maximal CPV
+(for $\delCP^\mathrm{true} = \pi/2, \, 3\pi/2$) can be discovered at
+$3\sigma$ down to $\stheta \simeq 8.8 \,(6.6)\times 10^{-4}$ for SPL
+(T2HK), and $\stheta \simeq 2\times 10^{-4}$ for the \BB. This number
+for the \BB\ is increased by a factor 3 if the fluxes are reduced to
+half of our nominal values.  The best sensitivity to CPV is obtained
+for all three facilities around $\stheta \sim 10^{-2}$. For this value
+CPV can be established for 78\%, 73\%, 75\% of all values of \delCP\
+for \BB, SPL, T2HK, respectively (again for systematics of 2\%).
+
+The widths of the bands in Fig.~\ref{fig:CPV} corresponds to different
+values for systematical errors. The curves which give the best
+sensitivities are obtained for systematics of 2\%, the curves
+corresponding to the worst sensitivity have been computed for
+systematics of 5\%. We change the uncertainty on the signal as well as
+on the background, however, it turns out that the most relevant
+uncertainty is the background normalization. We find that the impact
+of systematics is very small for the \BB. The reason for this is that
+the spectral shape of the background in the \BB\ (from pions and
+atmospheric neutrinos) is very different from the signal, and
+therefore they can be disentangled by the fit of the energy spectrum.
+For the Super Beams the background spectrum is more similar to the
+signal, and therefore an uncertainty on the background normalization
+might have a strong impact on the sensitivity, as visible from the SPL
+and T2HK curves in Fig.~\ref{fig:CPV}. In particular T2HK is strongly
+affected, and moving from 2\% to 5\% uncertainy decreases the
+sensitivity to maximal CPV by a factor 3.
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.9\textwidth]{./fig12.eps}
+%   
+   \mycaption{Impact of total exposure and systematical errors on the
+   CPV discovery potential of \BB, SPL, and T2HK. We show the
+   smallest true value of $\stheta$ for which $\delCP = \pi/2$ can be
+   distinguished from $\delCP = 0$ or $\delCP = \pi$ at $3\sigma$
+   $(\Delta\chi^2>9)$ as a function of the exposure in kt~yrs (left)
+   and as a function of the systematical error on the background
+   $\sigma_\mathrm{bkgr}$ (right). The widths of the curves in the
+   left panel corresponds to values of $\sigma_\mathrm{bkgr}$ from 2\%
+   to 5\%. The thin solid curves in the left panel corresponds to no
+   systematical errors. The right plot is calculated for the standard
+   exposure of 4400~kt~yrs. No systematical error on the signal has
+   been assumed. \label{fig:systematics}}
+\end{figure}
+
+This interesting feature can be understood in the following way. A
+rough measure to estimate the sensitivity is given by the signal
+compared to the error on the background. The latter receives
+contributions from the statistical error $\sqrt{B}$ and from the
+systematical uncertainty $\sigma_\mathrm{bkgr}B$, where $B$ is the
+number of background events and $\sigma_\mathrm{bkgr}$ is the
+(relative) systematical error. Hence the importance of the systematics
+can be estimated by the ratio of systematical and statistical errors
+$\sigma_\mathrm{bkgr} B / \sqrt{B} = \sigma_\mathrm{bkgr} \sqrt{B}$.
+Summing the numbers for background events in the neutrino and
+antineutrino channels given in Tab.~\ref{tab:events} one finds that
+systematical errors dominate ($\sigma_\mathrm{bkgr} \sqrt{B} > 1$) if
+$\sigma_\mathrm{bkgr} \gtrsim 6\%,\, 3\%, \, 2\%$ for \BB, SPL, T2HK,
+respectively. 
+%
+In the right panel Fig.~\ref{fig:systematics} we show the sensitivity
+to maximal CPV (as defined in the figure caption) as a function of
+$\sigma_\mathrm{bkgr}$. Indeed, the worsening of the sensitivity due
+to systematics occurs roughly at the values of $\sigma_\mathrm{bkgr}$
+as estimated above. For a more quantitative understanding of these
+curves it is necessary to consider the number of signal and background
+events for neutrinos and antineutrinos separately, as well as to take
+into account spectral information.
+
+
+The left panel of Fig.~\ref{fig:systematics} shows the sensitivity to
+maximal CPV as a function of the exposure\footnote{Note that the CPV
+sensitivity for the \BB\ with reduced fluxes from Fig.~\ref{fig:CPV}
+is worse than the value which follows from Fig.~\ref{fig:systematics}.
+The reason is that in Fig.~\ref{fig:systematics} the total exposure is
+scaled (mass~$\times$~time), i.e., signal and background are scaled in
+the same way, whereas for the dashed curve in Fig.~\ref{fig:CPV} only
+the fluxes are reduced but backgrounds are kept constant.} for values
+of $\sigma_\mathrm{bkgr}$ from 2\% to 5\%. One can observe clearly
+that for the standard exposure of 4400~kt~yrs T2HK is dominated by
+systematics and changing $\sigma_\mathrm{bkgr}$ from 2\% to 5\% has a
+big impact on the sensitivity. In contrast the CERN--MEMPHYS
+experiments (especially the \BB) are rather stable with respect to
+systematics and for the standard exposure they are still statistics
+dominated. We conclude that in T2HK systematics have to be under very
+good control\footnote{As a possible solution to this problem for T2HK
+it has been proposed in Ref.~\cite{Ishitsuka:2005qi} to place one half
+of the Hyper-K detector mass at Kamioka and the second half at the
+same off-axis angle in Korea.}, whereas this issue is less important
+for \BB\ and SPL.
+%
+We have checked explicitly that the systematical error on the signal
+has negligible impact on these results. Therefore, we have set this
+error to zero for calculating Fig.~\ref{fig:systematics} to highlight
+the importance of the background error. In all other calculations also
+the signal error is included, in particular also in Fig.~\ref{fig:CPV}.
+
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.8\textwidth]{./fig13.eps}
+%   
+   \mycaption{Impact of degeneracies on the CPV discovery potential
+   for the \BB. We show the sensitivity to CPV at $3\sigma$
+   $(\Delta\chi^2>9)$ computed for 4 different combinations of the
+   true values of the hierarchy (NH or IH) and $\theta_{23}$
+   ($\sin^2\theta_{23} = 0.4$ or $0.6$). Dashed curves are computed
+   neglecting degeneracies in the fit.\label{fig:deltacp}}
+\end{figure}
+
+Finally, in Fig.~\ref{fig:deltacp} we illustrate the impact of
+degeneracies, as well as the true hierarchy and \thetatt-octant on the
+CPV sensitivity.  Curves of different colors correspond to the four
+different choices for \sigdm\ and the \thetatt-octant of the true
+parameters. For the solid curves the simulated data for each choice of
+true \sigdm\ and \thetatt-octant are fitted by taking into account all
+four degenerate solutions, i.e., also for the fit all four
+combinations of \sigdm\ and \thetatt-octant are used. One observes
+from the figure that the true hierarchy and octant have a rather small
+impact on the \BB\ CPV sensitivity, in particular the sensitivity to
+maximal CPV is completely independent.  The main effect of changing the
+true hierarchy is to exchange the behavior between $0 < \delCP <
+180^\circ$ and $180^\circ < \delCP < 360^\circ$. For $\stheta \lesssim
+10^{-2}$ the sensitivity gets slightly worse if
+$\thetatt^\mathrm{true} > \pi/4$ compared to $\thetatt^\mathrm{true} <
+\pi/4$.
+
+The dashed curves in Fig.~\ref{fig:deltacp} are computed without
+taking into account the degeneracies, i.e., for each choice of true
+\sigdm\ and \thetatt-octant the data are fitted only with this
+particular choice. The effect of the degeneracies becomes visible for
+large values of \thetaot. Note that this is just the region where they
+can be reduced by a combined analysis with atmospheric neutrinos (see
+Sec.~\ref{sec:atmospherics} or Ref.~\cite{Huber:2005ep}).
+ 
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Synergies provided by the CERN--MEMPHYS facilities}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:synergies}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{Combining Beta Beam and Super Beam}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:synergies-beams}
+
+In this section we discuss synergies which emerge if both \BB\ and SPL
+are available. The main difference between these two beams is the
+different initial neutrino flavor,
+$\stackrel{\scriptscriptstyle(-)}{\nu}_e$ for \BB\ and
+$\stackrel{\scriptscriptstyle (-)}{\nu}_\mu$ for SPL. This implies
+that at near detectors all relevant cross sections can be measured. In
+particular, the near detector of the \BB\ will measure the cross
+section for the SPL appearance search, and vice versa.
+%
+If both experiments run with neutrinos and antineutrinos all possible
+transition probabilities are covered: $P_{\nu_e\to\nu_\mu}$,
+$P_{\bar\nu_e\to\bar\nu_\mu}$, $P_{\nu_\mu\to\nu_e}$, and
+$P_{\bar\nu_\mu\to\bar\nu_e}$. Together with the fact that matter
+effects are very small because of the relatively short baseline, this
+means that in addition to CP also direct tests of the T and CPT
+symmetries are possible.
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.9\textwidth]{./fig14.eps}
+%   
+   \mycaption{Discovery potential of a finite value of $\stheta$ at
+   $3\sigma$ $(\Delta\chi^2>9)$ for 5~yrs neutrino data from
+   \BB, SPL, and the combination of \BB\ + SPL compared to
+   10~yrs data from T2HK (2~yrs neutrinos + 8~yrs antineutrinos).
+   \label{fig:th13-5yrs}}
+\end{figure}
+
+However, if the CPT symmetry is assumed in principle all information
+can be obtained just from neutrino data because of the relations
+$P_{\bar\nu_e\to\bar\nu_\mu} = P_{\nu_\mu\to\nu_e}$ and
+$P_{\bar\nu_\mu\to\bar\nu_e} = P_{\nu_e\to\nu_\mu}$. As mentioned
+already in Sec.~\ref{sec:degeneracies} this implies that (time
+consuming) antineutrino running can be avoided. We illustrate this
+synergy in Figs.~\ref{fig:th13-5yrs} and \ref{fig:CP-5yrs}. In
+Fig.~\ref{fig:th13-5yrs} we show the $\theta_{13}$ discovery potential
+of 5 years of neutrino data from \BB\ and SPL. From the left panel the
+complementarity of the two experiments is obvious, since each of them
+is most sensitive in a different region of \delCP. (As expected from
+general properties of the oscillation probabilities the sensitivity
+curves of \BB\ and SPL are approximately related by the transformation
+$\delCP \to 2\pi - \delCP$.) Combining these two data sets results in
+a sensitivity slightly better than from 10 years (2$\nu$+8$\bar\nu$)
+of T2HK data.
+%
+As visible in Fig.~\ref{fig:CP-5yrs} also for the CPV discovery this
+synergy works and 5 years of neutrino data from \BB\ and SPL lead to a
+similar sensitivity as 10 years of T2HK.
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.6\textwidth]{./fig15.eps}
+%   
+   \mycaption{Sensitivity to CPV at $3\sigma$ $(\Delta\chi^2>9)$ for
+   combining 5~yrs neutrino data from \BB\ and SPL compared to
+   10~yrs data from T2HK (2~yrs neutrinos + 8~yrs antineutrinos).
+   \label{fig:CP-5yrs}}
+\end{figure}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{Resolving degeneracies with atmospheric neutrinos}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:atmospherics}
+
+It was pointed out in Ref.~\cite{Huber:2005ep} that for LBL
+experiments based on mega ton scale water \v{C}erenkov detectors data
+from atmospheric neutrinos (ATM) provide an attractive method to
+resolve degeneracies. Atmospheric neutrinos are sensitive to the
+neutrino mass hierarchy if $\theta_{13}$ is sufficiently large due to
+Earth matter effects, mainly in multi-GeV $e$-like
+events~\cite{Petcov:1998su,Akhmedov:1998ui,Bernabeu:2003yp}. Moreover,
+sub-GeV $e$-like events provide sensitivity to the octant of
+$\theta_{23}$~\cite{Kim:1998bv,Peres:2003wd,Gonzalez-Garcia:2004cu}
+due to oscillations with $\Delta m^2_{21}$ (see also
+Ref.~\cite{Kajita} for a discussion of atmospheric neutrinos in the
+context of Hyper-K). 
+%
+Following Ref.~\cite{Huber:2005ep} we investigate here the synergy
+from a combination of LBL data from \BB\ and SPL with ATM data in the
+MEMPHYS detector. Technical details are given in
+Sec.~\ref{sec:atm-details}. 
+ 
+The effect of degeneracies in LBL data has been discussed in
+Sec.~\ref{sec:degeneracies}, see Figs.~\ref{fig:degeneracies} and
+\ref{fig:degeneracies_SPL}. As discussed there, for given true
+parameter values the data can be fitted with the wrong hierarchy
+and/or with the wrong octant of $\theta_{23}$. Hence, from LBL data
+alone the hierarchy and the octant cannot be determined and
+ambiguities exist in the determination of $\theta_{13}$ and
+$\delta_\mathrm{CP}$.
+%
+If the LBL data are combined with ATM data only the colored regions in
+Fig.~\ref{fig:degeneracies} survive, i.e., in this particular example
+for SPL and T2HK the degeneracies are completely lifted at 95\%~CL,
+the mass hierarchy and the octant of $\theta_{23}$ can be identified,
+and the ambiguities in $\theta_{13}$ and $\delta_\mathrm{CP}$ are
+resolved. For the \BB\ an island corresponding to the wrong hierarchy
+does survive at the 95\%~CL for 2~dof. Still, the solution with the
+wrong sign of $\Delta m^2_{31}$ is disfavored with $\Delta\chi^2 =
+5.1$ with respect to the true solution, which corresponds to
+2.4$\sigma$ for 1~dof.
+%
+Let us note that in Fig.~\ref{fig:degeneracies} we have chosen a
+favorable value of $\sin^2\theta_{23} = 0.6$; for values
+$\sin^2\theta_{23} < 0.5$ in general the sensitivity of ATM data is
+weaker~\cite{Huber:2005ep}.
+
+\begin{figure}[!t]
+\centering
+  \includegraphics[width=0.9\textwidth]{./fig16.eps}
+%
+  \mycaption{Sensitivity to the mass hierarchy at $2\sigma$
+  $(\Delta\chi^2 = 4)$ as a function of the true values of
+  $\sin^22\theta_{13}$ and $\delta_\mathrm{CP}$ (left), and the
+  fraction of true values of $\delCP$ (right). The solid curves are
+  the sensitivities from the combination of long-baseline and
+  atmospheric neutrino data, the dashed curves correspond to
+  long-baseline data only. For comparison we show in the right panel
+  also the sensitivities of NO$\nu$A and NO$\nu$A+T2K extracted from
+  Fig.~13.14 of Ref.~\cite{Ayres:2004js}. For the curve labeled
+  ``NO$\nu$A (p.dr.)+T2K@4~MW'' a proton driver has been assumed for
+  NO$\nu$A and the T2K beam has been up-graded to 4~MW, see
+  Ref.~\cite{Ayres:2004js} for details.}
+  \label{fig:hierarchy}
+\end{figure}
+
+In Fig.~\ref{fig:hierarchy} we show how the combination of ATM+LBL
+data leads to a non-trivial sensitivity to the neutrino mass
+hierarchy, i.e.\ to the sign of $\Delta m^2_{31}$. For LBL data alone
+(dashed curves) there is practically no sensitivity for the
+CERN--MEMPHYS experiments (because of the very small matter effects
+due to the relatively short baseline), and the sensitivity of T2HK
+depends strongly on the true value of $\delta_\mathrm{CP}$. However,
+by including data from atmospheric neutrinos (solid curves) the mass
+hierarchy can be identified at $2\sigma$~CL provided
+$\sin^22\theta_{13} \gtrsim 0.02-0.03$. As an example we have chosen
+in that figure a true value of $\theta_{23} = \pi/4$. Generically the
+hierarchy sensitivity increases with increasing $\theta_{23}$, see
+Ref.~\cite{Huber:2005ep} for a detailed discussion.
+
+The sensitivity to the neutrino mass hierarchy shown in
+Fig.~\ref{fig:hierarchy} is significantly improved with respect to our
+previous results obtained in Ref.~\cite{Huber:2005ep}. There are two
+main reasons for this improved performance: First, we use now much
+more bins in charged lepton energy for fully contained single-ring
+events\footnote{The impact of energy binning on the hierarchy
+determination with atmospheric neutrinos has been discussed recently
+in Ref.~\cite{Petcov:2005rv} in the context of magnetized iron
+detectors.}  (compare Sec.~\ref{sec:atm-details}), and second, we
+implemented also information from multi-ring events. This latter point
+is important since the relative contribution of neutrinos and
+antineutrinos is different for single- and multi-ring
+events. Therefore, combining single- and multi-ring data allows to
+obtain a discrimination between neutrino and antineutrino events on a
+statistical basis. This in turn contains crucial information on the
+hierarchy, since the matter enhancement is visible either in neutrinos
+or antineutrinos, depending on the hierarchy.
+
+Although \BB\ and SPL alone have no sensitivity to the hierarchy at
+all, we find that the combination of them does provide rather good
+sensitivity even without atmospheric data. The reason for this
+interesting effect is the following. Because of the rather short
+baseline the matter effect is too small to distinguish between NH and
+IH given only neutrino and antineutrino information in one channel.
+However, the tiny matter effect suffices to move the hierarchy
+degenerate solution to slightly different locations in the ($\stheta$,
+$\delCP$) plane for the $\stackrel{\scriptscriptstyle(-)}{\nu}_e \to
+\stackrel{\scriptscriptstyle (-)}{\nu}_\mu$ (\BB) and
+$\stackrel{\scriptscriptstyle(-)}{\nu}_\mu \to
+\stackrel{\scriptscriptstyle (-)}{\nu}_e$ (SPL) channels (compare
+Fig.~\ref{fig:degeneracies}). Hence, if all four CP and T conjugate
+channels are available (as it is the case for the \BB+SPL combination)
+already the small matter effect picked up along the 130~km
+CERN--MEMPHYS distance provides sensitivity to the mass hierarchy for
+$\sin^22\theta_{13} \gtrsim 0.03$, or $\sin^22\theta_{13} \gtrsim 0.015$
+if also atmospheric neutrino data is included.
+
+For comparison we show in the right panel of Fig.~\ref{fig:hierarchy}
+also the sensitivity of the NO$\nu$A~\cite{Ayres:2004js} experiment,
+and of NO$\nu$A+T2K, where in the second case a beam upgrade by a
+proton driver has been assumed for NO$\nu$A, and for T2K the
+Super-Kamiokande detector has been used but the beam intensity has
+been increased by assuming 4~MW power. More details on these
+sensitivities can be found in Ref.~\cite{Ayres:2004js}.
+%
+Let us note that in general LBL experiments with two detectors (or the
+combination of two different LBL experiments) are a competitive method
+to atmospheric neutrinos for the hierarchy determination, see, e.g.,
+Refs.~\cite{Ishitsuka:2005qi,MenaRequejo:2005hn,Hagiwara:2005pe} for
+recent analyses.
+%
+We mention also the possibility to determine the neutrino mass
+hierarchy by using neutrino events from a galactic Super Nova
+explosion in mega ton \v{C}erenkov detectors such as MEMPHYS, see,
+e.g., Ref.~\cite{Kachelriess:2004vs}.
+
+\begin{figure}[!t]
+\centering
+  \includegraphics[width=0.55\textwidth]{./fig17.eps}
+%
+  \mycaption{$\Delta\chi^2$ of the solution with the wrong octant of
+  $\theta_{23}$ as a function of the true value of
+  $\sin^2\theta_{23}$. We have assumed a true value of $\theta_{13} =
+  0$.}
+  \label{fig:octant}
+\end{figure}
+
+Fig.~\ref{fig:octant} shows the potential of ATM+LBL data to exclude
+the octant degenerate solution. Since this effect is based mainly on
+oscillations with $\Delta m^2_{21}$ there is very good sensitivity
+even for $\theta_{13} = 0$; a finite value of $\theta_{13}$ in general
+improves the sensitivity~\cite{Huber:2005ep}.  From the figure one can
+read off that atmospheric data alone can can resolve the correct
+octant at $3\sigma$ if $|\sin^2\theta_{23} - 0.5| \gtrsim 0.085$. If
+atmospheric data is combined with the LBL data from SPL or T2HK there
+is sensitivity to the octant for $|\sin^2\theta_{23} - 0.5| \gtrsim
+0.05$. The improvement of the octant sensitivity with respect to
+previous analyses~\cite{Huber:2005ep,Gonzalez-Garcia:2004cu} follows
+from changes in the analysis of sub-GeV atmospheric events, where now
+three bins in lepton momentum are used instead of one. Note that since
+in Fig.~\ref{fig:octant} we have assumed a true value of $\theta_{13}
+= 0$, combining the \BB\ with ATM does not improve the sensitivity
+with respect to atmospheric data alone.
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Summary}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:conclusions}
+
+In this work we have studied the physics potential of the
+CERN--MEMPHYS neutrino oscillation project. We consider a Beta Beam
+(\BB) with $\gamma = 100$ for the stored ions, where existing
+facilities at CERN can be used optimally, and a Super Beam based on an
+optimized Super Proton Linac (SPL) with a beam energy of 3.5~GeV and
+4~MW power. As target we assume the MEMPHYS detector, a 440~kt water
+\v{C}erenkov detector at Fr\'ejus, at a distance of 130~km from
+CERN. The main characteristics of the experiments are summarized in
+Tab.~\ref{tab:setups}.
+%
+The adopted neutrino fluxes are based on realistic calculations of ion
+production and storage for the \BB, and a full simulation of the beam
+line (particle production and decay of secondaries) for SPL. Special
+care has be given to the issue of backgrounds, which we include by
+means of detailed event simulations and applying Super-Kamiokande particle
+identification algorithms.
+
+The physics potential of the \BB\ and SPL experiments in terms of
+$\theta_{13}$ discovery reach and sensitivity to CP violation has been
+addressed where parameter degeneracies are fully taken into account.
+The main results on these performance indicators are summarized in
+Figs.~\ref{fig:th13} and \ref{fig:CPV}.
+%
+We obtain a guaranteed discovery reach of $\stheta \simeq 5\times
+10^{-3}$ at $3\sigma$, irrespective of the actual value of \delCP. For
+certain values of \delCP\ the sensitivity is significantly improved,
+and for \BB\ (SPL) discovery limits around $\stheta \simeq 3\,(10)
+\times 10^{-4}$ are possible for a large fraction of all possible
+values of \delCP.
+%
+Maximal CP violation (for $\delCP^\mathrm{true} = \pi/2, \, 3\pi/2$)
+can be discovered at $3\sigma$ down to $\stheta \simeq 2\, (9)\times
+10^{-4}$ for \BB\ (SPL), whereas the best sensitivity to CP violation
+is obtained for $\stheta \sim 10^{-2}$: For $\stheta = 10^{-2}$ CP
+violation can be established at $3\sigma$ for 78\% (73\%) of all
+possible true values of \delCP\ for \BB\ (SPL).
+%
+We stress that the \BB\ performance in general depends crucially on
+the number of ion decays per year.
+%
+The impact of the value of systematical uncertainties on signal and
+background on our results is discussed.
+%
+The \BB\ and SPL sensitivities are compared to the ones of the
+phase~II of the T2K experiment in Japan (T2HK), which is a competing
+proposal of similar size and timescale. In general we obtain rather
+similar sensitivities for T2HK and SPL, and hence the CERN--MEMPHYS
+experiments provide a viable alternative to T2HK. We find that \BB\
+and SPL are less sensitive to systematical errors, whereas the
+sensitivity of T2HK crucially depends on the systematical error on the
+background.\footnote{Let us note that in the present study we have not
+considered the recent ``T2KK'' proposal~\cite{Ishitsuka:2005qi}, where
+one half of the Hyper-K detector mass is at Kamioka and the second
+half in Korea. For such a setup our results do not apply and
+especially the conclusion on systematical errors may be different.}
+
+Assuming that both \BB\ and SPL experiments are available, we point
+out that one can benefit from the different oscillation channels
+$\nu_e\to\nu_\mu$ for \BB\ and $\nu_\mu\to\nu_e$ for SPL, since by the
+combination of these channels the time intensive antineutrino
+measurements can be avoided. We show that 5 years of neutrino data from
+\BB\ and SPL lead to similar results as 2 years of neutrino plus 8
+years of antineutrino data from T2HK.
+%
+Furthermore, we discuss the use of atmospheric neutrinos in the
+MEMPHYS detector to resolve parameter degeneracies in the
+long-baseline data. This effect leads to a sensitivity to the neutrino
+mass hierarchy at $2\sigma$~CL for $\sin^22\theta_{13} \gtrsim
+0.025$ for \BB\ and SPL, although these experiments alone (without
+atmospheric data) have no sensitivity at all. The optimal hierarchy
+sensitivity is obtained from combining \BB+SPL+atmospheric data.
+Furthermore, the combination of atmospheric data with a Super Beam
+provides a possibility to determine the octant of $\theta_{23}$.
+
+To conclude, we have shown that the CERN--MEMPHYS neutrino oscillation
+project based on a Beta Beam and/or a Super Beam plus a mega ton scale
+water \v{C}erenkov detector offers interesting and competitive physics
+possibilities and is worth to be considered as a serious option in
+the worldwide process of identifying future high precision neutrino
+oscillation facilities~\cite{ISSpage}.
+
+\subsection*{Acknowledgment}
+
+We thank J.~Argyriades for communication on the Super-K atmospheric
+neutrino analysis, A.~Cazes for his work on the SPL simulation, and
+P.~Huber for his patience in answering questions concerning the use of
+GLoBES. Furthermore, we thank D.~Casper for the help in installing and
+running Nuance, and E.~Couce for discussions about the \BB\
+backgrounds.  T.S.\ is supported by the $6^\mathrm{th}$~Framework
+Program of the European Community under a Marie Curie Intra-European
+Fellowship.
+
+
+%\newpage
+\begin{thebibliography}{99}
+
+\bibitem{solar}
+  B.~T.~Cleveland {\it et al.},
+  Astrophys.\ J.\  {\bf 496} (1998) 505;
+  %%CITATION = ASJOA,496,505;%%
+%
+  J.N.~Abdurashitov {\it et al.}  [SAGE],
+  J.\ Exp.\ Theor.\ Phys.\  {\bf 95} (2002) 181
+  % [Zh.\ Eksp.\ Teor.\ Fiz.\  {\bf 122} (2002) 211].
+  [astro-ph/0204245];
+  %%CITATION = ASTRO-PH 0204245;%%
+%
+  T. Kirsten {\it et al.} [GALLEX and GNO], 
+  Nucl. Phys. B (Proc. Suppl.)  {\bf 118} (2003) 33;
+%
+  S.~Fukuda {\it et al.} [Super-Kamiokande],
+  %``Determination of solar neutrino 
+  % oscillation parameters using 1496 days  of Super-Kamiokande-I data,''
+  Phys. Lett. {\bf B539} (2002) 179;
+%
+%\bibitem{ahmad:2002ka}
+  Q.R. Ahmad {\em et~al.} [SNO],
+  Phys. Rev. Lett. {\bf 89}, 011302 (2002) 
+  [nucl-ex/0204009];
+  %%CITATION = NUCL-EX 0204009;%%
+%
+%\bibitem{Aharmim:2005gt}
+  B.~Aharmim {\it et al.}  [SNO],
+  %``Electron energy spectra, fluxes, and day-night asymmetries of B-8 solar
+  %neutrinos from the 391-day salt phase SNO data set,''
+  Phys.\ Rev.\ C {\bf 72} (2005) 055502
+  [nucl-ex/0502021].
+  %%CITATION = NUCL-EX 0502021;%%
+
+\bibitem{Fukuda:1998mi}
+  Y.~Fukuda {\it et al.} [Super-Kamiokande Coll.],
+  %``Evidence for oscillation of atmospheric neutrinos,''
+  Phys.\ Rev.\ Lett.\  {\bf 81} (1998) 1562
+  [hep-ex/9807003].
+  %%CITATION = HEP-EX 9807003;%%
+
+\bibitem{Ashie:2005ik}
+  Super-Kamiokande Coll.,
+  Y.~Ashie {\it et al.},  %[Super-Kamiokande Collaboration],
+  %``A measurement of atmospheric neutrino oscillation parameters by
+  %Super-Kamiokande I,''
+  Phys.\ Rev.\ D {\bf 71}, 112005 (2005)
+  [hep-ex/0501064];
+  %%CITATION = HEP-EX 0501064;%%
+%
+%\bibitem{Hosaka:2006zd}
+  J.~Hosaka {\it et al.},% [Super-Kamiokande Collaboration],
+  %``Three flavor neutrino oscillation analysis of atmospheric neutrinos in
+  %Super-Kamiokande,''
+  Phys.\ Rev.\ D {\bf 74}, 032002 (2006)
+  [hep-ex/0604011].
+  %%CITATION = HEP-EX 0604011;%%
+
+
+\bibitem{Araki:2004mb}
+  T.~Araki {\it et al.} [KamLAND Coll.],
+  %``Measurement of neutrino oscillation with KamLAND: Evidence of spectral
+  %distortion,''
+  Phys.\ Rev.\ Lett.\  {\bf 94}, 081801 (2005)
+  [hep-ex/0406035].
+  %%CITATION = HEP-EX 0406035;%%
+
+
+\bibitem{Aliu:2004sq}
+  E.~Aliu {\it et al.}  [K2K Coll.],
+  %``Evidence for muon neutrino oscillation in an accelerator-based
+  %experiment,''
+  Phys.\ Rev.\ Lett.\  {\bf 94}, 081802 (2005)
+  [hep-ex/0411038].
+  %%CITATION = HEP-EX 0411038;%%
+
+\bibitem{MINOS} 
+  D.G.~Micheal {\it et al.} [MINOS Coll.],
+  %''Observation of muon neutrino disappearance with the {MINOS} detectors and
+  %the {NuMI} neutrino beam,''
+  hep-ex/0607088.
+
+\bibitem{OPERA}
+  D. Autiero [OPERA Coll.], 
+  Nucl.\ Phys.\ B (Proc. Suppl.) {\bf 143}, 257 (2005);
+  M. Guler  \etal, \textit{Experiment proposal}, 
+  CERN/SPSC 2000-028 SPSC/P318 LNGS P25/2000.
+
+\bibitem{CNGS}
+  G. Acquistapace \etal, CERN-98-02.
+
+\bibitem{LSND}
+  A. Athanassopoulos \etal, Phys.\ Rev.\ Lett.\ {\bf 81}, 1774  (1998);
+  A. Aguilar \etal, Phys.\ Rev.\ D {\bf 64}, 112007 (2001).
+
+\bibitem{MINIBOONE}
+  I. Stancu \etal, FERMILAB-TM-2207.
+
+\bibitem{FOGLILISI05}
+  G.~L.~Fogli, E.~Lisi, A.~Marrone and A.~Palazzo,
+  %``Global analysis of three-flavor neutrino masses and mixings,''
+  Prog.\ Part.\ Nucl.\ Phys.\  {\bf 57}, 742 (2006)
+  [hep-ph/0506083].
+  %%CITATION = HEP-PH 0506083;%%
+
+\bibitem{Maltoni:2004ei}
+  M.~Maltoni, T.~Schwetz, M.~A.~Tortola and J.~W.~F.~Valle,
+  %``Status of global fits to neutrino oscillations,''
+  New J.\ Phys.\  {\bf 6}, 122 (2004)
+  [hep-ph/0405172];
+  %%CITATION = HEP-PH 0405172;%%
+%
+%\bibitem{Schwetz:2005jr}
+  T.~Schwetz,
+  %``Neutrino oscillations: Current status and prospects,''
+  Acta Phys.\ Polon.\ B {\bf 36}, 3203 (2005)
+  [hep-ph/0510331].
+  %%CITATION = HEP-PH 0510331;%%
+
+\bibitem{PMNS}
+  B.~Pontecorvo, Sov.\ Phys.--JETP {\bf 6}, 429 (1957) 
+  [Zh.\ Eksp.\ Teor.\ Fiz.\ \textbf{33}, 549 (1957)];
+  Z.~Maki, M.~Nakagawa and S.~Sakata, 
+  Prog.\ Theor.\ Phys.\ \textbf{28}, 870 (1962);
+  B.~Pontecorvo, Sov.\ Phys.--JETP \textbf{26}, 984 (1968) 
+  [Zh. Eksp. Teor. Fiz. \textbf{53}, 1717 (1967)];
+  V.~N.~Gribov and B.~Pontecorvo, 
+  Phys.\ Lett.\ B \textbf{28}, 493 (1969). 
+
+\bibitem{CHOOZ}
+  Chooz Collaboration,
+  M. Apollonio \etal, Phys.\ Lett.\ B {\bf 466}, 415 (1999);
+%\bibitem{Apollonio:2002gd}
+  M.~Apollonio {\it et al.},
+  %``Search for neutrino oscillations on a long base-line at the CHOOZ  nuclear
+  %power station,''
+  Eur.\ Phys.\ J.\ C {\bf 27}, 331 (2003)
+  [hep-ex/0301017].
+  %%CITATION = HEP-EX 0301017;%%
+
+\bibitem{Wpaper}
+  K.~Anderson \etal, White paper report on using nuclear 
+  reactors to search for a value of $\theta_{13}$, 
+  hep-ex/0402041;
+%
+  F.~Ardellier \etal, Letter of intent for Double-Chooz, 
+  hep-ex/0405032.
+
+\bibitem{T2K}
+  Y.~Itow {\it et al.},
+  The JHF-Kamioka neutrino project,
+  hep-ex/0106019;
+  %%CITATION = HEP-EX 0106019;%%
+%
+%\bibitem{Kobayashi:2005hu}
+  T.~Kobayashi,
+  %``Super beams,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 143} (2005) 303.
+  %%CITATION = NUPHZ,143,303;%%
+
+\bibitem{Ayres:2004js}
+  D.~S.~Ayres {\it et al.} [NOvA Coll.],
+  %``NOvA proposal to build a 30-kiloton off-axis detector to study neutrino
+  %oscillations in the Fermilab NuMI beamline,''
+  hep-ex/0503053.
+  %%CITATION = HEP-EX 0503053;%%
+
+\bibitem{Huber:2003pm}
+  P.~Huber, M.~Lindner, T.~Schwetz and W.~Winter,
+  %``Reactor neutrino experiments compared to superbeams,''
+  Nucl.\ Phys.\ B {\bf 665} (2003) 487
+  [hep-ph/0303232];
+  %%CITATION = HEP-PH 0303232;%%
+%
+%\bibitem{Huber:2004ug}
+  P.~Huber, M.~Lindner, M.~Rolinec, T.~Schwetz and W.~Winter,
+  %``Prospects of accelerator and reactor neutrino oscillation experiments  for
+  %the coming ten years,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 073014
+  [hep-ph/0403068].
+  %%CITATION = HEP-PH 0403068;%%
+
+\bibitem{Albrow:2005kw}
+  M.~G.~Albrow {\it et al.},
+  Physics at a Fermilab proton driver,
+  hep-ex/0509019.
+  %%CITATION = HEP-EX 0509019;%%
+
+\bibitem{SPL}
+  M.~Baylac {\it et al.},
+  Conceptual design of the SPL II: A high-power superconducting H- linac
+  at CERN, CERN-2006-006.
+
+\bibitem{BNLHS}
+%\bibitem{Diwan:2003bp}
+  M.~V.~Diwan {\it et al.},
+  %``Very long baseline neutrino oscillation experiments for precise
+  %measurements of mixing parameters and CP violating effects,''
+  Phys.\ Rev.\ D {\bf 68} (2003) 012002
+  [hep-ph/0303081].
+  %%CITATION = HEP-PH 0303081;%%
+
+\bibitem{zucchelli}
+%\bibitem{Zucchelli:2002sa}
+  P.~Zucchelli,
+  %``A novel concept for a anti-nu/e / nu/e neutrino factory: The Beta Beam,''
+  Phys.\ Lett.\ B {\bf 532} (2002) 166.
+  %%CITATION = PHLTA,B532,166;%%
+
+\bibitem{Albright:2004iw}
+  C.~Albright {\it et al.}  [Neutrino Factory/Muon Collider Coll.],
+  %``The neutrino factory and Beta Beam experiments and development,''
+  physics/0411123.
+  %%CITATION = PHYS-ICS 0411123;%%
+
+\bibitem{Blondel:2004ae}
+  A.~Blondel {\it et al.},
+  ECFA/CERN studies of a European neutrino factory complex,
+  CERN-2004-002
+
+\bibitem{Campagne:2004wt}
+  J.~E.~Campagne and A.~Cazes,
+  %``The theta(13) and delta(CP) sensitivities of the SPL-Frejus project
+  %revisited,''
+  Eur.\ Phys.\ J.\ C {\bf 45} (2006) 643
+  [hep-ex/0411062].
+  %%CITATION = HEP-EX 0411062;%%
+
+\bibitem{Mezzetto:2003ub}
+  M.~Mezzetto,
+  %``Physics reach of the beta beam,''
+  J.\ Phys.\ G {\bf 29} (2003) 1771
+  [hep-ex/0302007];
+  %%CITATION = HEP-EX 0302007;%%
+%
+  J.~Bouchez, M.~Lindroos, M.~Mezzetto,
+  %``Beta Beams: Present design and expected performances,''
+  AIP Conf.\ Proc.\  {\bf 721} (2004) 37
+  [hep-ex/0310059].
+  %%CITATION = HEP-EX 0310059;%%
+
+\bibitem{memphys}
+  A.~de Bellefon {\it et al.}, 
+  MEMPHYS: A large scale water \v{C}erenkov detector
+  at Fr\'ejus, Contribution to the CERN strategic committee,
+  hep-ex/0607026,\\
+  \verb!http://apc-p7.org/APC_CS/Experiences/MEMPHYS/!
+
+\bibitem{UNO} 
+  C.~K.~Jung,
+  Feasibility of a next generation underground water Cherenkov detector:
+  UNO, hep-ex/0005046.
+  %%CITATION = HEP-EX 0005046;%%
+
+\bibitem{Nakamura:2003hk}
+  K.~Nakamura,
+  %``Hyper-Kamiokande: A next generation water Cherenkov detector,''
+  Int.\ J.\ Mod.\ Phys.\ A {\bf 18} (2003) 4053.
+  %%CITATION = IMPAE,A18,4053;%%
+
+\bibitem{Huber:2005ep}
+  P.~Huber, M.~Maltoni, T.~Schwetz,
+  %``Resolving parameter degeneracies in long-baseline experiments by
+  %atmospheric neutrino data,''
+  Phys.\ Rev.\ D {\bf 71} (2005) 053006
+  [hep-ph/0501037].
+  %%CITATION = HEP-PH 0501037;%%
+
+\bibitem{Globes}
+  P.~Huber, M.~Lindner and W.~Winter,
+  %``Simulation of long-baseline neutrino oscillation experiments with
+  %GLoBES,''
+  Comput.\ Phys.\ Commun.\  {\bf 167} (2005) 195
+  [hep-ph/0407333],
+  \verb!http://www.ph.tum.de/~globes!
+
+\bibitem{Huber:2002mx}
+  P.~Huber, M.~Lindner and W.~Winter,
+  %``Superbeams versus neutrino factories,''
+  Nucl.\ Phys.\ B {\bf 645} (2002) 3
+  [hep-ph/0204352].
+  %%CITATION = HEP-PH 0204352;%%
+
+\bibitem{Nuance}
+  NUANCE event generator (v3), 
+  \verb!http://nuint.ps.uci.edu/nuance/!,
+  D.~Casper,
+  %``The nuance neutrino physics simulation, and the future,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 112} (2002) 161
+  [hep-ph/0208030].
+
+\bibitem{ISSpage}
+  Webpage of the International Scoping Study physics working group:\\
+  \verb!http://www.hep.ph.ic.ac.uk/iss/wg1-phys-phen/index.html!
+
+% BB %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\bibitem{MyNufact04}
+  M.~Mezzetto,
+  %``SPL and Beta Beams to the Frejus,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 149} (2005) 179.
+
+\bibitem{Donini:2004hu}
+  A.~Donini, E.~Fernandez-Martinez, P.~Migliozzi, S.~Rigolin and L.~Scotto Lavina,
+  %``Study of the eightfold degeneracy with a standard beta-beam and a
+  %super-beam facility,''
+  Nucl.\ Phys.\ B {\bf 710}, 402 (2005)
+  [hep-ph/0406132].
+  %%CITATION = HEP-PH 0406132;%%
+
+\bibitem{JJHigh2} 
+%\bibitem{Burguet-Castell:2005pa}
+  J.~Burguet-Castell, D.~Casper, E.~Couce, J.~J.~Gomez-Cadenas and P.~Hernandez,
+  %``Optimal beta-beam at the CERN-SPS,''
+  Nucl.\ Phys.\ B {\bf 725} (2005) 306
+  [hep-ph/0503021].
+  %%CITATION = HEP-PH 0503021;%%
+
+\bibitem{LindnerBB}
+%\bibitem{Huber:2005jk}
+  P.~Huber, M.~Lindner, M.~Rolinec and W.~Winter,
+  %``Physics and optimization of beta-beams: From low to very high gamma,''
+  Phys.\ Rev.\ D {\bf 73}, 053002 (2006)
+  [hep-ph/0506237].
+  %%CITATION = HEP-PH 0506237;%%
+
+\bibitem{JJHigh1}
+ J.~Burguet-Castell, D.~Casper, J.~J.~Gomez-Cadenas, P.~Hernandez and F.~Sanchez,
+ Nucl.\ Phys.\ B {\bf 695} (2004) 217
+ [hep-ph/0312068].
+
+\bibitem{Terranova}
+  F.~Terranova, A.~Marotta, P.~Migliozzi and M.~Spinetti,
+  %``High energy beta beams without massive detectors,''
+  Eur.\ Phys.\ J.\ C {\bf 38}, 69 (2004)
+  [hep-ph/0405081].
+  %%CITATION = HEP-PH 0405081;%%
+
+\bibitem{BB-Reviews}
+  M.~Mezzetto, %``Beta Beams,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 143} (2005) 309
+  [hep-ex/0410083];
+%
+  C.~Volpe,
+  %``Topical review on 'beta-beams',''
+  hep-ph/0605033.
+
+\bibitem{Volpe}
+  C.~Volpe,
+  %``What about a Beta Beam facility for low energy neutrinos?,''
+  J.\ Phys.\ G {\bf 30} (2004) L1
+  [hep-ph/0303222].
+
+\bibitem{Lindroos}
+%\bibitem{Autin:2002ms}
+  B.~Autin {\it et al.},
+  %``The acceleration and storage of radioactive ions for a neutrino  factory,''
+  J.\ Phys.\ G {\bf 29}, 1785 (2003)
+  [physics/0306106];
+  %%CITATION = PHYS-ICS 0306106;%%
+% 
+  M.~Benedikt, S.~Hancock and M.~Lindroos,
+  % ``Baseline Design for a Beta-Beam Neutrino Factory'', 
+  Proceedings of EPAC, 2004,
+  \verb!http://accelconf.web.cern.ch/AccelConf/e04!;
+%
+  M.~Lindroos, EURISOL DS/TASK12/TN-05-02.
+
+\bibitem{Eurisol}
+  Eurisol Beta Beam webpage: \verb!http://beta-beam.web.cern.ch/beta-beam/!.
+
+\bibitem{Lindroos-Optimization}
+  M.~Benedikt, A.~Fabich, S.~Hancock and M.~Lindroos,
+  %``Optimization Of The Beta-Beam Baseline,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 155} (2006) 211.
+
+\bibitem{MezzettoNuFact05}
+  M.~Mezzetto,
+  %``Physics potential of the gamma = 100,100 beta beam,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 155} (2006) 214
+  [hep-ex/0511005].
+
+% SPL %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\bibitem{Neugen}
+  The NEUGEN neutrino event generator,
+  \verb!http://minos.phy.tufts.edu/gallag/neugen/!.
+
+\bibitem{FLUKA}
+A.~Fasso \etal, Proceedings of the MonteCarlo 2000 conference, 
+Lisbon, October 26 2000, 
+A.~Kling \etal\ (eds.), Springer-Verlag Berlin (2001), 159-164 and 955-960. 
+
+\bibitem{GEANT}
+Application Software group, Computing and Network Division \etal, 
+GEANT Description and Simulation Tool, CERN Geneva, Switzerland
+
+\bibitem{HARP-MINERVA}
+  C. Catanesi \etal\ [HARP Coll.], CERN-SPSC 2002/019;
+%
+%\bibitem{Drakoulakos:2004gn}
+  D.~Drakoulakos {\it et al.}  [Minerva Coll.],
+  %``Proposal to perform a high-statistics neutrino scattering experiment  using
+  %a fine-grained detector in the NuMI beam,''
+  hep-ex/0405002.
+  %%CITATION = HEP-EX 0405002;%%
+
+\bibitem{Mezzetto:2003mm}
+  M.~Mezzetto,
+  %``Physics potential of the SPL super beam,''
+  J.\ Phys.\ G {\bf 29}, 1781 (2003)
+  [hep-ex/0302005].
+  %%CITATION = HEP-EX 0302005;%%
+
+% ATM %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\bibitem{Honda:2004yz}
+  M.~Honda, T.~Kajita, K.~Kasahara and S.~Midorikawa,
+  %``A new calculation of the atmospheric neutrino flux in a 3-dimensional
+  %scheme,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 043008
+  [astro-ph/0404457].
+  %%CITATION = ASTRO-PH 0404457;%%
+
+\bibitem{Lipari:1991ut}
+  P.~Lipari and T.~Stanev,
+  %``Propagation of multi - TeV muons,''
+  Phys.\ Rev.\ D {\bf 44} (1991) 3543.
+  %%CITATION = PHRVA,D44,3543;%%
+
+\bibitem{Gonzalez-Garcia:2004wg}
+  M.~C.~Gonzalez-Garcia and M.~Maltoni,
+  %``Atmospheric neutrino oscillations and new physics,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 033010
+  [hep-ph/0404085].
+  %%CITATION = HEP-PH 0404085;%%
+
+% DEGENERACIES %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\bibitem{Burguet-Castell:2001ez}
+  J.~Burguet-Castell, M.~B.~Gavela, J.~J.~Gomez-Cadenas, P.~Hernandez and O.~Mena,
+  %``On the measurement of leptonic CP violation,''
+  Nucl.\ Phys.\ B {\bf 608} (2001) 301
+  [hep-ph/0103258].
+  %%CITATION = HEP-PH 0103258;%%
+
+\bibitem{Minakata:2001qm}
+  H.~Minakata and H.~Nunokawa,
+  %``Exploring neutrino mixing with low energy superbeams,''
+  JHEP {\bf 0110}, 001 (2001)
+  [hep-ph/0108085].
+  %%CITATION = HEP-PH 0108085;%%
+
+\bibitem{Fogli:1996pv}
+  G.~L.~Fogli and E.~Lisi,
+  %``Tests of three-flavor mixing in long-baseline neutrino oscillation
+  %experiments,''
+  Phys.\ Rev.\ D {\bf 54}, 3667 (1996)
+  [hep-ph/9604415].
+  %%CITATION = HEP-PH 9604415;%%
+
+\bibitem{Barger:2001yr}
+  V.~Barger, D.~Marfatia and K.~Whisnant,
+  %``Breaking eight-fold degeneracies in neutrino CP violation, mixing, and
+  %mass hierarchy,''
+  Phys.\ Rev.\ D {\bf 65}, 073023 (2002)
+  [hep-ph/0112119].
+  %%CITATION = HEP-PH 0112119;%%
+
+\bibitem{Yasuda:2004gu}
+  O.~Yasuda,
+  %``New plots and parameter degeneracies in neutrino oscillations,''
+  New J.\ Phys.\  {\bf 6}, 83 (2004)
+  [hep-ph/0405005].
+  %%CITATION = HEP-PH 0405005;%%
+
+\bibitem{Ishitsuka:2005qi}
+  M.~Ishitsuka, T.~Kajita, H.~Minakata and H.~Nunokawa,
+  %``Resolving neutrino mass hierarchy and CP degeneracy by two identical
+  %detectors with different baselines,''
+  Phys.\ Rev.\ D {\bf 72} (2005) 033003
+  [hep-ph/0504026].
+  %%CITATION = HEP-PH 0504026;%%
+
+\bibitem{Antusch:2004yx}
+  S.~Antusch, P.~Huber, J.~Kersten, T.~Schwetz and W.~Winter,
+  %``Is there maximal mixing in the lepton sector?,''
+  Phys.\ Rev.\ D {\bf 70}, 097302 (2004)
+  [hep-ph/0404268].
+  %%CITATION = HEP-PH 0404268;%%
+
+\bibitem{Minakata:2004pg}
+  H.~Minakata, M.~Sonoyama and H.~Sugiyama,
+  %``Determination of theta(23) in long-baseline neutrino oscillation
+  %experiments with three-flavor mixing effects,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 113012
+  [hep-ph/0406073].
+  %%CITATION = HEP-PH 0406073;%%
+
+\bibitem{Donini:2005db}
+  A.~Donini, E.~Fernandez-Martinez, D.~Meloni and S.~Rigolin,
+  %``nu/mu disappearance at the SPL, T2K-I, NOnuA and the neutrino factory,''
+  Nucl.\ Phys.\ B {\bf 743}, 41 (2006)
+  [hep-ph/0512038].
+  %%CITATION = HEP-PH 0512038;%%
+
+\bibitem{Peres:2003wd}
+  O.L.G.~Peres, A.Y.~Smirnov,
+  %``Atmospheric neutrinos: LMA oscillations, U(e3) induced interference and
+  %CP-violation,''
+  Nucl.\ Phys.\ B {\bf 680} (2004) 479
+  [hep-ph/0309312].
+  %%CITATION = HEP-PH 0309312;%%
+
+\bibitem{Gonzalez-Garcia:2004cu}
+  M.C.~Gonzalez-Garcia, M.~Maltoni, A.Y. Smirnov,
+  %``Measuring the deviation of the 2-3 lepton mixing from maximal with
+  %atmospheric neutrinos,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 093005
+  [hep-ph/0408170].
+  %%CITATION = HEP-PH 0408170;%%
+
+\bibitem{Petcov:1998su}
+  S.~T.~Petcov,
+  %``Diffractive-like (or parametric-resonance-like?) enhancement of the  earth
+  %(day-night) effect for solar neutrinos crossing the earth core,''
+  Phys.\ Lett.\ B {\bf 434} (1998) 321
+  [hep-ph/9805262];
+  %%CITATION = HEP-PH 9805262;%%
+%
+%\bibitem{Chizhov:1998ug}
+  M.~Chizhov, M.~Maris and S.~T.~Petcov,
+  %``On the oscillation length resonance in the transitions of solar and
+  %atmospheric neutrinos crossing the earth core,''
+  hep-ph/9810501;
+  %%CITATION = HEP-PH 9810501;%%
+%
+%\bibitem{Chizhov:1999az}
+  M.~V.~Chizhov and S.~T.~Petcov,
+  %``New conditions for a total neutrino conversion in a medium,''
+  Phys.\ Rev.\ Lett.\  {\bf 83} (1999) 1096
+  [hep-ph/9903399].
+  %%CITATION = HEP-PH 9903399;%%
+
+\bibitem{Akhmedov:1998ui}
+  E.~K.~Akhmedov,
+  %``Parametric resonance of neutrino oscillations and passage of solar and
+  %atmospheric neutrinos through the earth,''
+  Nucl.\ Phys.\ B {\bf 538}, 25 (1999)
+  [hep-ph/9805272];
+  %%CITATION = HEP-PH 9805272;%%
+%
+%\bibitem{Akhmedov:1998xq}
+  E.~K.~Akhmedov, A.~Dighe, P.~Lipari and A.~Y.~Smirnov,
+  %``Atmospheric neutrinos at Super-Kamiokande and parametric resonance in
+  %neutrino oscillations,''
+  Nucl.\ Phys.\ B {\bf 542}, 3 (1999)
+  [hep-ph/9808270].
+  %%CITATION = HEP-PH 9808270;%%
+
+\bibitem{Bernabeu:2003yp}
+  J.~Bernabeu, S.~Palomares-Ruiz and S.~T.~Petcov,
+  %``Atmospheric neutrino oscillations, theta(13) and neutrino mass
+  %hierarchy,''
+  Nucl.\ Phys.\ B {\bf 669}, 255 (2003)
+  [hep-ph/0305152].
+  %%CITATION = HEP-PH 0305152;%%
+
+\bibitem{Kim:1998bv}
+  C.~W.~Kim and U.~W.~Lee,
+  %``Comment on the possible electron-neutrino excess in the  Super-Kamiokande
+  %atmospheric neutrino experiment,''
+  Phys.\ Lett.\ B {\bf 444}, 204 (1998)
+  [hep-ph/9809491].
+  %%CITATION = HEP-PH 9809491;%%
+
+\bibitem{Kajita}
+  T.~Kajita, Talk at NNN05, 7--9 April 2005, Aussois, Savoie, France,\\
+  \verb!http://nnn05.in2p3.fr/!
+
+\bibitem{Petcov:2005rv}
+  S.~T.~Petcov and T.~Schwetz,
+  %``Determining the neutrino mass hierarchy with atmospheric neutrinos,''
+  Nucl.\ Phys.\ B {\bf 740}, 1 (2006)
+  [hep-ph/0511277].
+  %%CITATION = HEP-PH 0511277;%%
+
+\bibitem{MenaRequejo:2005hn}
+  O.~Mena-Requejo, S.~Palomares-Ruiz and S.~Pascoli,
+  %``Super-NOvA: A long-baseline neutrino experiment with two off-axis
+  %detectors,''
+  Phys.\ Rev.\ D {\bf 72} (2005) 053002
+  [hep-ph/0504015];
+  %%CITATION = HEP-PH 0504015;%%
+%
+%\bibitem{Mena:2005ri}
+  %O.~Mena, S.~Palomares-Ruiz and S.~Pascoli,
+  %``Determining the neutrino mass hierarchy and CP violation in NOnuA with a
+  %second off-axis detector,''
+  Phys.\ Rev.\ D {\bf 73} (2006) 073007
+  [hep-ph/0510182].
+  %%CITATION = HEP-PH 0510182;%%
+
+\bibitem{Hagiwara:2005pe}
+  K.~Hagiwara, N.~Okamura and K.~Senda,
+  %``Solving the neutrino parameter degeneracy by measuring the T2K off-axis
+  %beam in Korea,''
+  Phys.\ Lett.\ B {\bf 637}, 266 (2006)
+  [hep-ph/0504061].
+  %%CITATION = HEP-PH 0504061;%%
+
+\bibitem{Kachelriess:2004vs}
+  M.~Kachelriess and R.~Tomas,
+  %``Identifying the neutrino mass hierarchy with supernova neutrinos,''
+  hep-ph/0412100.
+  %%CITATION = HEP-PH 0412100;%%
+
+\end{thebibliography}
+\end{document}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
Index: /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-8sept06/CERN-MEMPHYS.tex
===================================================================
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+++ /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/TS-8sept06/CERN-MEMPHYS.tex	(revision 385)
@@ -0,0 +1,2248 @@
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\NeedsTeXFormat{LaTeX2e}
+\documentclass[12pt,a4paper]{article}
+
+%-- used packages ------------------------------------------------------
+
+\usepackage{cite}
+\usepackage{graphicx}
+\usepackage{epsfig}
+\usepackage{amssymb}
+\usepackage{amsmath}
+\usepackage{latexsym}
+
+
+%-- page parameters -------------------------------------------------
+
+\jot = 1.5ex
+\parskip 5pt plus 1pt
+%\parindent 0pt
+\evensidemargin -0.1in   \oddsidemargin  -0.1in
+\textwidth  6.5in       \textheight 9.4in
+\topmargin -.8cm        \headsep    1.0cm
+
+%-- command (re)definitions -----------------------------------------
+
+\newcommand{\capdef}{}
+%\newcommand{\mycaption}[2][\capdef]{\renewcommand{\capdef}{#2}%
+%       \caption[#1]{{\itshape #2}}}
+\newcommand{\mycaption}[2][\capdef]{\renewcommand{\capdef}{#2}%
+       \caption[#1]{{\footnotesize #2}}}
+\makeatletter
+\renewcommand{\fnum@table}{\textbf{\tablename~\thetable}}
+\renewcommand{\fnum@figure}{\textbf{\figurename~\thefigure}}
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+
+\newcounter{myenumi}
+\newcommand{\myitem}{\refstepcounter{myenumi}\item}
+\renewcommand{\themyenumi}{\roman{myenumi}}
+\newenvironment{mylist}{%
+        \setcounter{myenumi}{0}
+        \begin{list}{\textit{\themyenumi)}}{%
+        \setlength{\topsep}{0.2\baselineskip}%
+        \setlength{\partopsep}{-\topsep}%
+        \setlength{\itemsep}{\topsep}%
+        \setlength{\parsep}{0\baselineskip}%
+        \setlength{\leftmargin}{0em}%
+        \setlength{\listparindent}{\parindent}%
+        \setlength{\itemindent}{2.5em}%
+        \setlength{\labelwidth}{1.5em}%
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+{\end{list}}
+
+\newlength{\myem}
+\settowidth{\myem}{m}
+\newcommand{\sep}[1]{#1}
+\newcounter{mysubequation}[equation]
+\renewcommand{\themysubequation}{\alph{mysubequation}}
+\newcommand{\mytag}{\stepcounter{mysubequation}%
+\tag{\theequation\protect\sep{\themysubequation}}}
+\newcommand{\globallabel}[1]{\refstepcounter{equation}\label{#1}}
+
+\makeatletter
+\renewcommand{\section}{\@startsection{section}{1}{0em}{-\baselineskip}%
+{\baselineskip}{\normalfont\large\bfseries}}
+\renewcommand{\subsection}%
+{\@startsection{subsection}{2}{0em}{-0.7\baselineskip}%
+{0.7\baselineskip}{\normalfont\bfseries}}
+\makeatother
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%
+% definitions
+%%%%%%%%%%%%%%%%%%%%%%%%
+\newcommand{\centre}[2]{\multispan{#1}{\hfill #2\hfill}}
+\newcommand{\etal}{\textit{et al.}}
+\newcommand{\stheta}{\ensuremath{\sin^22\theta_{13}}}
+\newcommand{\BB}{$\beta$B}
+\newcommand{\sigdm}{\ensuremath{{\rm sign}(\Delta m^2_{31})}}
+\newcommand{\delCP}{\ensuremath{\delta_{\rm CP}}}
+\newcommand{\thetatt}{\ensuremath{\theta_{23}}}
+
+\def\nubar{$\overline{\nu}\ $}
+\def\nue{\ensuremath{\nu_{e}}}
+\def\nubare{\ensuremath{\overline{\nu}_{e}}}
+\def\nubarecc{$\overline{\nu}_{e}^{CC}\ $}
+\def\numu{\ensuremath{\nu_{\mu}\ }}
+\def\nubarmu{\ensuremath{\overline{\nu}_{\mu}}}
+\def\nubarmucc{$\overline{\nu}_{\mu}^{CC}\ $}
+\def\nutau{\ensuremath{\nu_{\tau}\ }}
+\def\nubartau{\ensuremath{\overline{\nu}_{\tau}}}
+\newcommand{\nuenumu}{\ensuremath{\nue \rightarrow \numu\,}}
+\newcommand{\numunutau}{\ensuremath{\numu \rightarrow \nutau\,}}
+\newcommand{\nuenutau}{\ensuremath{\nue \rightarrow \nutau}}
+\newcommand{\nubarenubarmu}{\ensuremath{\overline{\nu}_e \rightarrow \overline{\nu}_\mu\,}}
+\newcommand{\nubarmunubare}{\ensuremath{\overline{\nu}_\mu \rightarrow \overline{\nu}_e\,}}
+\newcommand{\dmot}{\ensuremath{\Delta m^2_{12}\,}}
+
+\newcommand{\He}{\ensuremath{^6{\mathrm{He}}}}
+\newcommand{\Ne}{\ensuremath{^{18}{\mathrm{Ne}}}}
+\def\Li{^6{\mathrm{Li}}}
+\def\anue{\overline{{\mathrm\nu}}_{\mathrm e}}
+\def\anumu{\overline{{\mathrm\nu}}_{\mathrm \mu}}
+\newcommand{\thetaot}{\ensuremath{\theta_{13}}\,}
+\newcommand{\numunue}{\ensuremath{\nu_\mu \rightarrow \nu_e}}
+\newcommand{\nueovernumu}{\ensuremath{\nue/\numu}}
+
+
+
+\begin{document}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+%%%%                     Title-page                              %%%%
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+%\begin{titlepage}
+
+% the footnote symbols are only redefined for the title page !
+\renewcommand{\thefootnote}{\alph{footnote}}
+
+\begin{flushright}
+LAL-06-35\\
+IC/2006/011\\
+SISSA 16/2006/EP\\
+\end{flushright}
+
+\vspace*{1cm}
+
+\renewcommand{\thefootnote}{\fnsymbol{footnote}}
+\setcounter{footnote}{-1}
+
+{\begin{center} 
+{\Large\textbf{
+Physics potential of the CERN--MEMPHYS\\[2mm] 
+neutrino oscillation project}
+}
+\end{center}}
+
+\vspace*{.8cm}
+
+\begin{center} {\bf
+J.-E.\ Campagne$^a$, 
+M.\ Maltoni$^b$,
+M.\ Mezzetto$^c$, and 
+T.\ Schwetz$^d$}
+\end{center}
+
+{\it
+\begin{center}
+  $^a$Laboratoire de l'Acc\'el\'erateur Lin\'eaire, 
+  IN2P3-CNRS and Universit\'e PARIS-SUD 11\\
+  Centre Scientifique d'Orsay-B\^at.\ 200-B.P.\ 34, 
+  91898 Orsay Cedex, France\\[2mm]
+%  
+  $^b$International Centre for Theoretical Physics, 
+  Strada Costiera 11, 31014 Trieste, Italy\\[2mm]
+%  
+  $^c$Istituto Nazionale Fisica Nucleare, Sezione di Padova,
+  Via Marzolo 8, 35100 Padova, Italy\\[2mm]
+%
+  $^d$Scuola Internazionale Superiore di Studi Avanzati, 
+  Via Beirut 2--4, 34014 Trieste, Italy
+\end{center}}
+
+\vspace*{0.5cm}
+
+
+\begin{abstract}
+We consider the physics potential of CERN based neutrino oscillation
+experiments consisting of a Beta Beam (\BB) and a Super Beam (SPL)
+sending neutrinos to MEMPHYS, a 440~kt water \v{C}erenkov detector at
+Fr\'ejus, at a distance of 130~km from CERN. The $\theta_{13}$
+discovery reach and the sensitivity to CP violation are investigated,
+including a detailed discussion of parameter degeneracies and
+systematical errors. For SPL sensitivities similar to the ones of the
+phase~II of the T2K experiment (T2HK) are obtained, whereas the \BB\
+may reach significantly better sensitivities, depending on the
+achieved number of total ion decays.  The results for the
+CERN--MEMPHYS experiments are less affected by systematical
+uncertainties than T2HK.
+%
+We point out that by a combination of data from \BB\ and SPL a
+measurement with antineutrinos is not necessary and hence the same
+physics results can be obtained within about half of the measurement time
+compared to one single experiment.
+%
+Furthermore, it is shown how including data from atmospheric neutrinos in
+the MEMPHYS detector allows to resolve parameter degeneracies and, in
+particular, provides sensitivity to the neutrino mass hierarchy and
+the octant of $\theta_{23}$.
+%\pacs{14.60.Pq, 14.60.Lm}
+\end{abstract}
+
+\renewcommand{\thefootnote}{\arabic{footnote}}
+\setcounter{footnote}{0}
+
+\newpage
+%\tableofcontents
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Introduction}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+In recent years strong evidence for neutrino oscillations has been
+obtained in solar~\cite{solar}, atmospheric~\cite{sk-atm},
+reactor~\cite{Araki:2004mb}, and accelerator~\cite{Aliu:2004sq}
+neutrino experiments. The very near future of long-baseline (LBL)
+neutrino experiments is devoted to the study of the oscillation
+mechanism in the range of $\Delta m^2_{31} \approx 2.4\times10^{-3} \:
+\mathrm{eV}^2$ indicated by atmospheric neutrinos using conventional
+$\nu_\mu$ beams.  Similar as in the K2K experiment in
+Japan~\cite{Aliu:2004sq}, the presently running MINOS experiment in
+the USA~\cite{MINOS} uses a low energy beam to measure $\Delta m^2_{31}$ by
+observing the $\nu_\mu\rightarrow\nu_\mu$ disappearance probability,
+while the forthcoming OPERA~\cite{OPERA} experiment will be able to
+detect $\nu_\tau$ appearance within the high energy CERN--Gran Sasso
+beam~\cite{CNGS}.
+%
+If we do not consider the LSND anomaly~\cite{LSND} that will be
+further studied soon by the MiniBooNE experiment~\cite{MINIBOONE}, all
+data can be accommodated within the three flavor scenario (see
+Refs.~\cite{FOGLILISI05,Maltoni:2004ei} for recent global analyses),
+and neutrino oscillations are described by two neutrino mass-squared
+differences ($\Delta m^2_{21}$ and $\Delta m^2_{31}$) and the $3\times
+3$ unitary Pontecorvo-Maki-Nakagawa-Sakata (PMNS) lepton mixing
+matrix~\cite{PMNS} with three angles
+($\theta_{12}$,$\theta_{13}$,$\theta_{23}$) and one Dirac CP phase
+$\delCP$.
+
+Future tasks of neutrino physics are an improved sensitivity to the
+last unknown mixing angle, $\theta_{13}$, to explore the CP violation
+mechanism in the leptonic sector, and to determine the sign of $\Delta
+m^2_{31}$ which describes the type of the neutrino mass hierarchy
+(normal, $\Delta m^2_{31} > 0$ or inverted, $\Delta m^2_{31} < 0$).
+%
+The present upper bound on $\theta_{13}$ is dominated by the
+constraint from the Chooz reactor experiment~\cite{CHOOZ}. A global
+analysis of all data yields $\sin^22\theta_{13}<0.082$ at
+90\%~CL~\cite{Maltoni:2004ei}. A main purpose of upcoming reactor and
+accelerator experiments is to improve this bound or to reveal a finite
+value of $\theta_{13}$. In reactor experiments, one uses $\bar{\nu}_e$
+in disappearance mode and the sensitivity is increased with respect to
+present experiments by the use of a near detector close to the
+reactor~\cite{Wpaper}. In accelerator experiments, the first
+generation of so-called Super Beams with sub-mega watt proton drivers
+such as T2K (phase-I)~\cite{T2K} and NO$\nu$A~\cite{Ayres:2004js}, the
+appearance channel $\nu_\mu\to\nu_e$ is explored. This next generation
+of reactor and Super Beam experiments will reach sensitivities of the
+order of $\sin^22\theta_{13} \lesssim 0.01$ ($90\%$~CL) within a time
+scale of several years~\cite{Huber:2003pm}.
+%
+Beyond this medium term program, there are several projects on how to
+enter the high precision age in neutrino oscillations and to attack
+the ultimate goals like the discovery of leptonic CP violation or the
+determination of the neutrino mass hierarchy. In accelerator
+experiments, one can extend the Super Beam concept by moving to
+multi-mega watt proton drivers~\cite{T2K,Albrow:2005kw,SPL,BNLHS} or
+apply novel technologies, such as neutrino beams from decaying ions
+(so-called Beta Beams)~\cite{zucchelli,Albright:2004iw} or from
+decaying muons (so-called Neutrino
+Factories)~\cite{Albright:2004iw,Blondel:2004ae}.
+
+In this work we focus on possible future neutrino oscillation
+facilities hosted at CERN, namely a multi-mega watt Super Beam
+experiment based on a Super Proton Linac (SPL)~\cite{Campagne:2004wt}
+and a $\gamma = 100$ Beta Beam
+(\BB)~\cite{Mezzetto:2003ub}. These experiments will search for
+$\stackrel{\scriptscriptstyle (-)}{\nu}_\mu \to
+\stackrel{\scriptscriptstyle(-)}{\nu}_e$ and
+$\stackrel{\scriptscriptstyle (-)}{\nu}_e \to
+\stackrel{\scriptscriptstyle(-)}{\nu}_\mu$ appearance, respectively,
+by sending the neutrinos to a mega ton scale water \v{C}erenkov
+detector (MEMPHYS)~\cite{memphys}, located at a distance of 130~km from
+CERN under the Fr\'ejus mountain. Similar detectors are under
+consideration also in the US (UNO~\cite{UNO}) and in Japan
+(Hyper-K~\cite{T2K,Nakamura:2003hk}).
+%
+We perform a detailed analysis of the SPL and \BB\ physics
+potential, discussing the discovery reach for $\theta_{13}$ and
+leptonic CP violation. In addition we consider the possibility to
+resolve parameter degeneracies in the LBL data by using the
+atmospheric neutrinos available in the mega ton
+detector~\cite{Huber:2005ep}. This leads to a sensitivity to the
+neutrino mass hierarchy of the CERN--MEMPHYS experiments, despite the
+rather short baseline.
+%
+The physics performances of \BB\ and SPL are compared to the ones
+obtainable at the second phase of the T2K experiment in Japan, which
+is based on an upgraded version of the original T2K beam and the
+Hyper-K detector (T2HK)~\cite{T2K}.
+
+The outline of the paper is as follows.  In Sec.~\ref{sec:analysis} we
+summarize the main characteristics of the \BB, SPL, and T2HK
+experiments and give general details of the physics analysis methods,
+whereas in Sec.~\ref{sec:experiments} we describe in some detail the
+MEMPHYS detector, the \BB, and the SPL Super Beam. In
+Sec.~\ref{sec:degeneracies} we review the problem of parameter
+degeneracies and discuss its implications for the experiments under
+consideration. In Sec.~\ref{sec:sensitivities} we present the
+sensitivities to the ``atmospheric parameters'' $\theta_{23}$ and
+$\Delta m^2_{31}$, the $\theta_{13}$ discovery potential, and the
+sensitivity to CP violation. We also investigate in some detail the
+impact of systematical errors. In Sec.~\ref{sec:synergies} we discuss
+synergies which are offered by the CERN--MEMPHYS facilities.  We
+point out advantages of the case when \BB\ and SPL are available
+simultaneously, and we consider the use of atmospheric neutrino data in
+MEMPHYS in combination with the LBL experiments. Our results are
+summarized in Sec.~\ref{sec:conclusions}.
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Experiments overview and analysis methods}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:analysis}
+
+In this section we give the most important experimental parameters
+which we adopt for the simulation of the CERN--MEMPHYS experiments
+\BB\ and SPL, as well as for the T2HK experiment in Japan. These
+parameters are summarized in Tab.~\ref{tab:setups}. For all
+experiments the detector mass is 440~kt, and the running time is 10
+years, with a division in neutrino and antineutrino running time in
+such a way that roughly an equal number of events is obtained. We
+always use the total available information from appearance as well as
+disappearance channels including the energy spectrum. For all three
+experiments we adopt rather optimistic values for the systematical
+uncertainties of 2\% as default values, but we also consider the case
+when systematics are increased to 5\%. These errors are uncorrelated
+between the various signal channels (neutrinos and antineutrinos), and
+between signals and backgrounds.
+
+\begin{table}
+  \centering
+  \begin{tabular}{lcc@{\qquad\qquad}c}
+  \hline\noalign{\smallskip}
+       & \BB & SPL & T2HK \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  Detector mass & 440~kt & 440~kt & 440~kt\\
+  Baseline      & 130 km & 130 km & 295 km \\
+  Running time ($\nu + \bar\nu$) 
+                & 5 + 5 yr & 2 + 8 yr & 2 + 8 yr \\
+  Beam intensity  & $5.8\,(2.2) \cdot 10^{18}$ He (Ne) dcys/yr & 4 MW & 4 MW\\
+  Systematics on signal  & 2\% & 2\% & 2\%\\
+  Systematics on backgr. & 2\% & 2\% & 2\%\\
+  \noalign{\smallskip}\hline
+  \end{tabular}
+  \mycaption{Summary of default parameters used for the simulation of the
+  \BB, SPL, and T2HK experiments.\label{tab:setups}}
+\end{table}
+
+A more detailed description of the CERN--MEMPHYS experiments is given
+in Sec.~\ref{sec:experiments}. For the T2HK simulation we use the
+setup provided by GLoBES~\cite{Globes} based on
+Ref.~\cite{Huber:2002mx}, which follows closely the LOI~\cite{T2K}. In
+order to allow a fair comparison we introduce the following changes
+with respect to the configuration used in Ref.~\cite{Huber:2002mx}:
+The fiducial mass is set to 440~kt, the systematical errors on the
+background and on the $\nu_e$ and $\bar\nu_e$ appearance signals is
+set to 2\%, and we use a total running time of 10 years, divided into
+2 years of data taking with neutrinos and 8 years with
+antineutrinos. We include an additional background from the
+$\bar\nu_\mu \to \bar\nu_e$ ($\nu_\mu \to \nu_e$) channel in the
+neutrino (antineutrino) mode. Furthermore, we use
+the same CC detection cross section as for the \BB/SPL
+analysis~\cite{Nuance}. For more details see
+Refs.~\cite{T2K,Huber:2002mx}.
+
+\begin{table}
+  \centering
+  \begin{tabular}{lcccccc}
+  \hline\noalign{\smallskip}
+       & \centre{2}{\BB} & \centre{2}{SPL} & \centre{2}{T2HK} \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  & $\delCP=0$ & $\delCP=\pi/2$ & $\delCP=0$ & $\delCP=\pi/2$ & $\delCP=0$ & $\delCP=\pi/2$\\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+%
+  appearance $\nu$ & & & & & & \\
+  background       & \centre{2}{143} &\centre{2}{622} &\centre{2}{898}\\
+  $\stheta=0$      & \centre{2}{28}  &\centre{2}{51}  &\centre{2}{83}  \\
+  $\stheta=10^{-3}$&    76  &   88   &   105  &   14  &   178 &    17  \\ 
+  $\stheta=10^{-2}$&   326  &  365   &   423  &  137  &   746 &   238  \\
+%  
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+%
+  appearance $\bar\nu$ & & & & & & \\
+  background       & \centre{2}{157} &\centre{2}{640} &\centre{2}{1510}\\
+  $\stheta=0$      & \centre{2}{31}  &\centre{2}{57}  &\centre{2}{93}  \\
+  $\stheta=10^{-3}$&    83  &   12   &   102  &  146  &   192 &   269  \\ 
+  $\stheta=10^{-2}$&   351  &  126   &   376  &  516  &   762 &  1007  \\
+%  
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+%
+  disapp. $\nu$ &\centre{2}{100315}&\centre{2}{21653}&\centre{2}{24949}\\
+  background    & \centre{2}{6}   &\centre{2}{1}    &\centre{2}{444}\\
+  disapp. $\bar\nu$&\centre{2}{84125}&\centre{2}{18321}&\centre{2}{34650}\\
+  background       &\centre{2}{5}    &\centre{2}{1}    &\centre{2}{725}\\
+  \noalign{\smallskip}\hline
+%  
+  \end{tabular}
+  \mycaption{Number of events for appearance and disappearance signals
+  and backgrounds for the \BB, SPL, and T2HK experiments as
+  defined in Tab.~\ref{tab:setups}. For the appearance signals the
+  event numbers are given for several values of $\stheta$ and $\delCP
+  = 0$ and $\pi/2$. The background as well as the disappearance event
+  numbers correspond to $\theta_{13}=0$. For the other oscillation
+  parameters the values of Eq.~(\ref{eq:default-params}) are
+  used.\label{tab:events}}
+\end{table}
+
+In Tab.~\ref{tab:events} we give the number of signal and background
+events for the experiment setups as defined in Tab.~\ref{tab:setups}.
+For the appearance channels ($\stackrel{\scriptscriptstyle (-)}{\nu}_e
+\to \stackrel{\scriptscriptstyle(-)}{\nu}_\mu$ for the \BB\ and
+$\stackrel{\scriptscriptstyle (-)}{\nu}_\mu \to
+\stackrel{\scriptscriptstyle(-)}{\nu}_e$ for SPL and T2HK) we give the
+signal events for various values of $\theta_{13}$ and $\delCP$. The
+``signal'' events for $\theta_{13} = 0$ are appearance events induced by
+the oscillations with $\Delta m^2_{21}$. The value $\stheta = 10^{-3}$
+corresponds roughly to the sensitivity limit for the considered
+experiments, whereas $\stheta = 10^{-2}$ gives a good sensitivity
+to CP violation. This can be appreciated by comparing the values of
+$\nu$ and $\bar\nu$ appearance events for $\delCP = 0$ and $\pi/2$. In
+the table the background to the appearance signal is given for
+$\theta_{13} = 0$. Note that in general the number of background
+events depends also on the oscillation parameters, since also the
+background neutrinos in the beam oscillate. This effect is
+consistently taken into account in the analysis, however, for the
+parameter values in the table the change in the background events due
+to oscillations is only of the order of a few events.
+
+The physics analysis is performed with the GLoBES open source
+software~\cite{Globes}, which provides a convenient tool to simulate
+long-baseline experiments and compare different facilities in a
+unified framework. The experiment definition (AEDL) files for the \BB\
+and SPL simulation with GLoBES are available at Ref.~\cite{ISSpage}
+{\bf *** to be updated! ***}. In the analysis parameter degeneracies
+and correlations are fully taken into account and in general all
+oscillation parameters are varied in the fit.
+%
+To simulate the ``data'' we adopt the following
+set of ``true values'' for the oscillation parameters:
+%
+\begin{equation}\label{eq:default-params}
+\begin{array}{l@{\qquad}l}
+  \Delta m^2_{31} = +2.4 \times 10^{-3}~\mathrm{eV}^2\,, & 
+  \sin^2\theta_{23} = 0.5\,,\\ 
+  \Delta m^2_{21} = 7.9 \times 10^{-5}~\mathrm{eV}^2 \,,&
+  \sin^2\theta_{12} = 0.3 \,,
+\end{array}
+\end{equation} 
+%
+and we include a prior knowledge of these values with an accuracy of
+10\% for $\theta_{12}$, $\theta_{23}$, $\Delta m^2_{31}$, and 4\% for
+$\Delta m^2_{21}$ at 1$\sigma$. These values and accuracies are
+motivated by recent global fits to neutrino oscillation
+data~\cite{FOGLILISI05,Maltoni:2004ei}, and they are always used
+except where explicitly stated otherwise.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{The CERN--MEMPHYS experiments}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:experiments}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The MEMPHYS detector}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+MEMPHYS (MEgaton Mass PHYSics)~\cite{memphys} is a mega ton class
+water \v{C}erenkov detector in the straight extrapolation of
+Super-Kamiokande, located at Fr\'ejus, at a distance of 130~km from
+CERN. It is an alternative design of the UNO~\cite{UNO} and
+Hyper-Kamiokande~\cite{Nakamura:2003hk} detectors and shares the same
+physics case, both from the non-accelerator domain (nucleon decay,
+super nova neutrino detection, solar neutrinos, atmospheric neutrinos)
+and from the accelerator domain which is the subject of this paper. A
+recent civil engineering pre-study to envisage the possibly of large
+cavity excavation located under the Fr\'ejus mountain (4800~m.e.w.)
+near the present Modane underground laboratory has been undertaken.
+The main result of this pre-study is that MEMPHYS may be built with
+present techniques as a modular detector consisting of several shafts,
+each with 65~m in diameter, 65~m in height for the total water
+containment. A schematic view of the layout is shown in
+Fig.~\ref{fig:MEMPHYS}. For the present study we have chosen a
+fiducial mass of 440~kt which means 3 shafts and an inner detector of
+57~m in diameter and 57~m in height.  Each inner detector may be
+equipped with photo detectors (81000 per shaft) with a 30\%
+geometrical coverage and the same photo-statistics of Super-Kamiokande
+(with a 40\% coverage). In principle up to 5 shafts are possible,
+corresponding to a fiducial mass of 730~kt.
+%
+The Fr\'ejus site offers a natural protection against cosmic rays by a
+factor $10^6$. If not mentioned otherwise, the event selection and
+particle identification are the Super-Kamiokande algorithms results.
+
+\begin{figure}
+\centering
+\includegraphics[width=0.65\textwidth]{./fig1.eps}
+\mycaption{\label{fig:MEMPHYS}Sketch of the MEMPHYS detector under the
+Fr\'ejus mountain.}	
+\end{figure}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The $\gamma = 100\times100$ baseline Beta Beam}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+The concept of a Beta Beam (\BB) has been introduced by P.~Zucchelli
+in Ref.~\cite{zucchelli}. Neutrinos are produced by the decay of
+radioactive isotopes which are stored in a decay ring. An important
+parameter is the relativistic gamma factor of the ions, which
+determines the energy of the emitted neutrinos. \BB\ performances have
+been computed previously for $\gamma(\He)= 66$~\cite{Mezzetto:2003ub},
+100~\cite{MyNufact04,Donini:2004hu,JJHigh2}, 150~\cite{JJHigh2},
+200~\cite{LindnerBB}, 350~\cite{JJHigh2},
+500~\cite{JJHigh1,LindnerBB}, 1000~\cite{LindnerBB},
+2000~\cite{JJHigh1}, 2488~\cite{Terranova}. Reviews can be found in
+Ref.~\cite{BB-Reviews}, the physics potential of a very low gamma \BB\
+has been studied in Ref.~\cite{Volpe}. Performances of a \BB\ with
+$\gamma > 150$ are extremely promising, however, they are neither
+based on an existing accelerator complex nor on a robust estimation of
+the ion decay rates. For a CERN based \BB, fluxes have been estimated
+in Ref.~\cite{Lindroos} and a design study is in progress for the
+facility \cite{Eurisol}. In this work we assume an integrated flux of
+neutrinos in 10 years, corresponding to $5.8\cdot 10^{19}$ useful \He\
+decays and $2.2 \cdot 10^{19}$ useful \Ne\ decays. These fluxes have
+been assumed in all the physics papers quoted above, and they are two
+times higher than the baseline fluxes computed in
+Ref.~\cite{Lindroos}. These latter fluxes suffer for the known
+limitations of the PS and SPS synchrotrons at CERN, ways to improve
+them have been delineated in Ref.~\cite{Lindroos-Optimization}.
+
+The infrastructure available at CERN as well as the MEMPHYS
+location at a distance of 130~km suggest a $\gamma$-factor of about
+$100$. Such a value implies a mean neutrino energy of 400~MeV, which
+leads to the oscillation maximum at about 200~km for $\Delta m^2_{31}
+= 2.4\times 10^{-3}$~eV$^2$.  We have checked that the performance at
+the somewhat shorter baseline of 130~km is rather similar to the one
+at the oscillation maximum. Moreover, the purpose of this paper is to
+estimate the physics potential for a realistic set-up and not to study
+the optimization of the \BB\ regardless of any logistic consideration
+(see, e.g., Refs.~\cite{LindnerBB,JJHigh2} for such optimization
+studies).
+
+\begin{figure}[!t]
+  \centering
+  \includegraphics[width=0.65\textwidth]{./fig2.eps}
+  \mycaption{\label{fig:QE-Energy} Energy resolution for \nue\
+  interactions in the 200--300~MeV energy range. The quantitiy
+  displayed is the difference between the reconstructed and the true
+  neutrino energy.}
+\end{figure}
+
+The signal events from the $\nu_e \to \nu_\mu$ neutrino and
+antineutrino appearance channels in the \BB\ are \numu charged current
+(CC) events. The Nuance v3r503 Monte Carlo code~\cite{Nuance} is used
+to generate signal events. The selection for these events is based on
+standard Super-Kamiokande particle identification algorithms.  The
+muon identification is reinforced by asking for the detection of the
+Michel decay electron. 
+%
+The neutrino energy is reconstructed by smearing momentum and
+direction of the charged lepton with the Super-Kamiokande resolution
+functions, and applying quasi-elastic (QE) kinematics assuming the
+known incoming neutrino direction. Energy reconstruction in the \BB\
+energy range is remarkably powerful, and the contamination of non-QE
+events very small, as shown in Fig.~\ref{fig:QE-Energy}.
+%
+As pointed out in Ref.~\cite{JJHigh2}, it is necessary to use a
+migration matrix for the neutrino energy reconstruction to properly
+handle Fermi motion smearing and the non-QE event contamination.  We
+use 100 MeV bins for the reconstructed energy and 40 MeV bins for the
+true neutrino energy.  Four migration matrices (for
+$\nu_e,\bar\nu_e,\nu_\mu,\bar\nu_\mu$) are applied to signal events as
+well as backgrounds.  As shown in Ref.~\cite{MezzettoNuFact05} the
+migration matrix approximation has a visible (though small) effect for
+example in the leptonic CP violation discovery potential.
+
+\begin{table}[t]
+     \centering
+     \begin{tabular}{l@{\qquad}rrr@{\qquad}rrr}
+     \hline\noalign{\smallskip}
+       & \multicolumn{3}{ c }{\Ne} & \multicolumn{3}{c}{\He} \\
+     \hline\noalign{\smallskip}
+       & \numu CC & $\pi^+$ & $\pi^-$ & \nubarmu CC & $\pi^+$ & $\pi^-$ \\
+     \hline\noalign{\smallskip}
+      Generated ev.\ & 115367   &  557   &  341 & 101899 &  674   &  400 \\
+      Particle ID    &  95717   &  204   &  100 & 85285  &  240   &  118 \\
+      Decay          &  61347   &  107   &    8 & 69242  &  120   &    8 \\
+\hline\noalign{\smallskip}
+    \end{tabular}
+    \mycaption{\label{tab:sigbck} Events for the \BB\ in a 4400~kt~yr
+    exposure.  \numu(\nubarmu) CC events are computed assuming full
+    oscillations ($P_{\nu_e\to\nu_\mu} = 1$), and pion backgrounds are
+    computed from \nue(\nubare) CC+NC events. In the rows we give the
+    number events generated within the fiducial volume (``Generated
+    ev.''), after muon particle identification (``Particle ID''), and
+    after applying a further identification requiring the detection of
+    the Michel electron (``Decay''). }
+\end{table}
+
+
+Backgrounds from charged pions and atmospheric neutrinos are computed
+with the identical analysis chain as signal events.
+Charged pions generated in NC events (or in NC-like events where the
+leading electron goes undetected) are the main source of background for
+the experiment. To compute this background inclusive NC and CC events
+have been generated with the \BB\ spectrum. Events have been selected
+where the only visible track is a charged pion above the \v{C}erenkov
+threshold. Particle identification efficiencies have been applied to
+those particles. The probability for a pion to survive in water until
+its decay has been computed with Geant~3.21 and cross-checked with a
+Fluka~2003 simulation. This probability is different for positive and
+negative pions, the latter having a higher probability to be absorbed
+before decaying. The surviving events are background, and the
+reconstructed neutrino energy is computed misidentifying these pions
+as muons. Event rates are reported in Tab.~\ref{tab:sigbck}. From
+these numbers it becomes evident that requiring the detection of the
+Michel electron provides an efficient cut to eliminate the pion
+background.
+%
+These background rates are significantly smaller than quoted in
+Ref.~\cite{MyNufact04}, where pion decays were computed with the
+same probabilities as for muons and they are slightly different
+from those quoted in Ref.~\cite{ MezzettoNuFact05}, where an
+older version of Nuance had been used.
+%
+The numbers of Tab.~\ref{tab:sigbck} have been cross-checked by
+comparing the Nuance and Neugen~\cite{Neugen} event
+generators, finding a fair agreement in background rates and energy shape.
+
+Also atmospheric neutrinos can constitute an important source of
+background~\cite{zucchelli,JJHigh2,JJHigh1,MezzettoNuFact05}. This
+background can be suppressed only by keeping a very short duty cycle
+($2.2 \cdot 10^{-3}$ is the target value for the \BB\ design study),
+and this in turn is one of the most challenging bounds on the design
+of the Beta Beam complex. Following Ref.~\cite{MezzettoNuFact05} we
+include the atmospheric neutrino background based on a Monte Carlo
+simulation using Nuance. Events are reconstructed as if they were
+signal neutrino events. We estimate that 5 events/year would survive
+the analysis chain in a full solar year (the \BB\ should run for about
+1/3 of this period) and include these events as backgrounds in the
+analysis. Under these circumstances, the present value of the \BB\
+duty cycle seems to be an overkill, it could be reduced by a factor 5
+at least, see also Ref.~\cite{MezzettoNuFact05} for a discussion of
+the effect of a higher duty cycle.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The $3.5$-GeV SPL Super Beam}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+In the Conceptual Design Report~1 (CDR1) the foreseen Super Proton
+Linac (SPL)~\cite{SPL} has been optimized to provide the protons
+for the muon production in the context of a Neutrino Factory. 
+%
+Recently, in Ref.~\cite{Campagne:2004wt} a new optimization of the
+beam energy as well as the secondary particle focusing and decay has
+been undertaken considering a Super Beam searching for $\nu_\mu
+\rightarrow \nu_e$ and $\bar{\nu}_\mu \rightarrow \bar{\nu}_e$
+appearance as well as $\nu_\mu$, $\bar\nu_\mu$ disappearance in a mega
+ton scale water \v{C}erenkov detector. In particular, a full
+simulation of the beam line from the proton on target interaction up
+to the secondary particle decay tunnel has been performed. The proton
+on a liquid mercury target (30~cm long, $7.5$~mm radius, 13.546
+density) has been simulated with FLUKA~2002.4~\cite{FLUKA} while the
+horn focusing system and the decay tunnel simulation has been
+preformed with GEANT~3.21~\cite{GEANT}.\footnote{Although there are
+differences between the predicted pion and kaon productions as a
+function of proton kinetic energy with FLUKA~2002.4 and 2005.6, the
+results are consistent for the relevant energy of 3.5~GeV. We
+emphasize that the pion and the kaon production cross-sections are
+waiting for experimental confirmation~\cite{HARP-MINERVA} and a new
+optimization would be required if their is a disagreement with the
+present knowledge.}
+
+\begin{figure}[!t]
+  \centering 
+  \includegraphics[width=0.65\textwidth]{./fig3.eps}
+  \mycaption{\label{fig:fluxSPLContrib} Neutrino fluxes, at $130$~km
+  from the target with the horns focusing the positive particles
+  (top panel) or the negative particles (bottom panel). The fluxes are
+  computed for a SPL proton beam of $3.5$~GeV (4~MW), a decay tunnel
+  with a length of $40$~m and a radius of $2$~m.}
+\end{figure}
+
+Since the optimization requirements for a Neutrino Factory are rather
+different than for a Super Beam the new SPL configuration has a
+significant impact on the physics performance (see
+Ref.~\cite{Campagne:2004wt} for a detailed discussion).  The SPL
+fluxes of the four neutrino species ($\nu_\mu$, $\nu_e$,
+$\bar{\nu}_\mu$, $\bar{\nu}_e$) for the positive ($\nu_\mu$ beam) and
+the negative focusing ($\bar{\nu}_\mu$ beam) are show in
+Fig.~\ref{fig:fluxSPLContrib}.  The total number of $\nu_\mu$
+($\bar{\nu}_\mu$) in positive (negative) focusing is about
+$1.18\,(0.97) \times 10^{12}\:\mathrm{m}^{-2}\mathrm{y}^{-1}$ with an
+average energy of $300$~MeV. The $\nu_e$ ($\bar{\nu}_e$) contamination
+in the $\nu_\mu$ ($\bar\nu_\mu$) beam is around $0.7\%$
+($6.0\%$). Following Ref.~\cite{Mezzetto:2003mm}, the $\pi^o$
+background is reduced using a tighter PID cut compared to standard
+Super-Kamiokande analysis. The Michel electron is required for the
+$\mu$ identification.
+%
+For the $\nu_\mu \rightarrow \nu_e$ channel the background consists
+roughly of 90\% $\nu_e \rightarrow \nu_e$ CC interactions, 6\% $\pi^o$
+from NC interactions, 3\% miss identified muons from $\nu_\mu
+\rightarrow \nu_\mu$ CC, and 1\% $\bar{\nu}_e \rightarrow \bar{\nu}_e$
+CC interactions. For the $\bar{\nu}_\mu \rightarrow \bar{\nu}_e$
+channel the contributions to the background are 45\% $\bar{\nu}_e
+\rightarrow \bar{\nu}_e$ CC interactions, 35\% $\nu_e \rightarrow
+\nu_e$ CC interactions, 18\% $\pi^o$ from NC interactions and 2\% miss
+identified muons from $\bar{\nu}_\mu \rightarrow \bar{\nu}_\mu$ CC.
+In addition we include the events from the contamination of 
+``wrong sign'' muon-neutrinos due to $\bar\nu_\mu \to \bar\nu_e$
+($\nu_\mu \to \nu_e$) oscillations in the neutrino (antineutrino)
+mode.
+
+\begin{figure}[!t]
+  \centering
+  \includegraphics[width=0.5\textwidth]{./fig4.eps}
+%
+  \mycaption{\label{fig:fluxComparison} 
+  Comparison of the fluxes from SPL and \BB.}
+\end{figure}
+
+Considering the signal over square-root of background
+ratio, the $3.5$~GeV beam energy is more favorable than the original
+$2.2$~GeV option. Compared to the fluxes used in
+Refs.~\cite{Mezzetto:2003mm,Donini:2004hu} the gain is at least a
+factor $2.5$ and this justifies to reconsider in detail the physics
+potential of the SPL Super Beam.
+%
+Both the appearance and the disappearance channels are used. For the
+spectral analysis we use 10 bins of 100~MeV in the interval $0 < E_\nu
+< 1$~GeV, applying the same migration matrices as for the \BB\ to take
+into account properly the neutrino energy reconstruction. As ultimate
+goal suggested in Ref.~\cite{T2K} a 2\% systematical error is used as
+default both for signal and background, this would be achieved by a
+special care of the design of the close position. However, we discuss
+also how a 5\% systematical error affects the sensitivities.
+%
+Using neutrino cross-sections on water from Ref.~\cite{Nuance}, the
+number of expected $\nu_\mu$ charged current is about $95$ per kt~yr
+{\bf *** does this number change using Nuance Xsects instead of
+Lipari? ***}. In Fig.~\ref{fig:fluxComparison} we compare the fluxes
+from the SPL to the one from the \BB.
+ 
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Degeneracies}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:degeneracies}
+
+
+A characteristic feature in the analysis of future LBL experiments is
+the presence of {\it parameter degeneracies}.  Due to the inherent
+three-flavor structure of the oscillation probabilities, for a given
+experiment in general several disconnected regions in the
+multi-dimensional space of oscillation parameters will be
+present. Traditionally these degeneracies are referred to in the
+following way:
+%
+\begin{itemize}
+\item
+The {\it intrinsic} or
+($\delCP,\theta_{13}$)-degeneracy~\cite{Burguet-Castell:2001ez}:
+For a measurement based on the $\nu_\mu \to \nu_e$ oscillation probability for
+neutrinos and antineutrinos two disconnected solutions appear in the
+($\delCP,\theta_{13}$) plane.
+\item
+The {\it hierarchy} or sign($\Delta
+m^2_{31}$)-degeneracy~\cite{Minakata:2001qm}: The two solutions
+corresponding to the two signs of $\Delta m^2_{31}$ appear in general
+at different values of $\delCP$ and $\theta_{13}$.
+\item
+The {\it octant} or $\theta_{23}$-degeneracy~\cite{Fogli:1996pv}:
+Since LBL experiments are sensitive mainly to $\sin^22\theta_{23}$ it
+is difficult to distinguish the two octants $\theta_{23} < \pi/4$ and
+$\theta_{23} > \pi/4$.  Again, the solutions corresponding to
+$\theta_{23}$ and $\pi/2 - \theta_{23}$ appear in general at different
+values of $\delCP$ and $\theta_{13}$.
+\end{itemize}
+%
+This leads to an eight-fold ambiguity in $\theta_{13}$ and
+$\delCP$~\cite{Barger:2001yr}, and hence degeneracies provide a
+serious limitation for the determination of $\theta_{13}$, $\delCP$,
+and the sign of $\Delta m^2_{31}$. Recent discussions of degeneracies
+can be found for example in
+Refs.~\cite{Huber:2002mx,Huber:2005ep,Yasuda:2004gu,Ishitsuka:2005qi};
+degeneracies in the context of CERN--Fr\'ejus \BB\ and SPL have been
+considered previously in Ref.~\cite{Donini:2004hu}.
+%
+In Fig.~\ref{fig:degeneracies} we illustrate the effect of
+degeneracies for the \BB, SPL, and T2HK experiments. Assuming the
+true parameter values $\delta_\mathrm{CP} = -0.85 \pi$,
+$\sin^22\theta_{13} = 0.03$, $\sin^2\theta_{23} = 0.6$ we show the
+allowed regions in the plane of $\stheta$ and $\delCP$ taking into
+account the solutions with the wrong hierarchy and the wrong octant of
+$\theta_{23}$.
+
+\begin{figure}[!t]
+\centering
+\includegraphics[width=0.95\textwidth]{./fig5.eps}
+%
+  \mycaption{Allowed regions in $\sin^22\theta_{13}$ and
+  $\delta_\mathrm{CP}$ for LBL data alone (contour lines) and LBL+ATM
+  data combined (colored regions). $\mathrm{H^{tr/wr} (O^{tr/wr})}$
+  refers to solutions with the true/wrong mass hierarchy (octant of
+  $\theta_{23}$). The true parameter values are $\delta_\mathrm{CP} =
+  -0.85 \pi$, $\sin^22\theta_{13} = 0.03$, $\sin^2\theta_{23} = 0.6$,
+  and the values from Eq.~(\ref{eq:default-params}) for the other
+  parameters.}
+\label{fig:degeneracies}
+\end{figure}
+
+
+\begin{figure}[!t]
+\centering
+\includegraphics[width=0.9\textwidth]{./fig6.eps}
+%
+  \mycaption{Resolving degeneracies in SPL by successively using the
+  appearance rate measurement, disappearance channel rate and
+  spectrum, spectral information in the appearance channel, and
+  atmospheric neutrinos.  Allowed regions in $\sin^22\theta_{13}$ and
+  $\delta_\mathrm{CP}$ are shown at 95\%~CL, and $\mathrm{H^{tr/wr}
+  (O^{tr/wr})}$ refers to solutions with the true/wrong mass hierarchy
+  (octant of $\theta_{23}$). The true parameter values are
+  $\delta_\mathrm{CP} = -0.85 \pi$, $\sin^22\theta_{13} = 0.03$,
+  $\sin^2\theta_{23} = 0.6$, and the values from
+  Eq.~(\ref{eq:default-params}) for the other parameters.}
+\label{fig:degeneracies_SPL}
+\end{figure}
+
+As visible in Fig.~\ref{fig:degeneracies} for the
+Super Beam experiments SPL and T2HK there is only a four-fold
+degeneracy related to sign($\Delta m^2_{31}$) and the octant of
+$\theta_{23}$, whereas the intrinsic degeneracy can be resolved. 
+%
+Several pieces of information contribute to this effect, as we
+illustrate at the example of SPL in Fig.~\ref{fig:degeneracies_SPL}.
+The dashed curves in the left panel of this figure show the allowed
+regions for only the appearance measurement (for neutrinos and
+antineutrinos) without spectral information, i.e., just a counting
+experiment. In this case the eight-fold degeneracy is present in its
+full beauty, and one finds two solutions (corresponding to the
+intrinsic degeneracy) for each choice of sign($\Delta m^2_{31}$) and
+the octant of $\theta_{23}$. Moreover, the allowed regions are
+relatively large. For the thin solid curves the information from the
+disappearance rate is added. The main effect is to decrease the size
+of the allowed regions in $\stheta$. This is especially pronounced for
+the solutions involving the wrong octant of $\theta_{23}$, since these
+solutions are strongly affected by an uncertainty in $\theta_{23}$
+which gets reduced by the disappearance information. Using in addition
+to the disappearance rate also the spectrum again decreases the size
+of the allowed regions, however, still all eight solutions are present
+(compare dashed curves in the right panel).
+%
+The most relevant effect comes from the inclusion of spectral
+information in the appearance channel, as visible from the comparison
+of the dashed and thick-solid curves in the right panel of
+Fig.~\ref{fig:degeneracies_SPL}. The intrinsic degeneracy gets
+resolved and only four solutions corresponding to the sign and octant
+degeneracies are left.\footnote{The inclusion of spectral information
+might be the source of possible differences to previous studies, see
+e.g.\ Ref.~\cite{Donini:2004hu}.} Note that the thick curves in the
+right panel of Fig.~\ref{fig:degeneracies_SPL} correspond to the
+regions show in Fig.~\ref{fig:degeneracies} for the SPL.
+%
+Finally, by the inclusion of information from atmospheric neutrinos
+all degeneracies can be resolved in this example, and the true
+solution is identified at 95\%~CL (see Sec.~\ref{sec:atmospherics} and
+Ref.~\cite{Huber:2005ep} for further discussions of atmospheric
+neutrinos).
+
+Concerning the \BB\ one observes from Fig.~\ref{fig:degeneracies} that
+in this case the ($\delCP,\theta_{13}$)-degeneracy cannot be resolved
+and one has to deal with eight distinct solutions. One reason for this
+is the absence of precise information on $|\Delta m^2_{31}|$ and
+$\sin^22\theta_{23}$ which is provided by the $\nu_\mu$ disappearance
+in Super Beam experiments but is not available from the \BB. If
+external information on these parameters at the level of 3\% is
+included the allowed regions in Fig.~\ref{fig:degeneracies} are
+significantly reduced. However, still all eight solutions are present,
+which indicates that for the \BB\ spectral information is not
+efficient enough to resolve the ($\delCP,\theta_{13}$)-degeneracy, and
+in this case only the inclusion of atmospheric neutrino data allows a
+nearly complete resolution of the degeneracies.
+
+An important observation from Fig.~\ref{fig:degeneracies} is that
+degeneracies have only a very small impact on the CP violation
+discovery, in the sense that if the true solution is CP violating also
+the fake solutions are located at CP violating values of
+$\delCP$. Indeed, since for the relatively short baselines in the
+experiments under consideration matter effects are very small, the
+sign($\Delta m^2_{31}$)-degenerate solution is located within good
+approximation at $\delCP' \approx \pi -
+\delCP$~\cite{Minakata:2001qm}. Therefore, although degeneracies
+strongly affect the determination of $\theta_{13}$ and $\delCP$ they
+have only a small impact on the CP violation discovery potential.
+Furthermore, as clear from Fig.~\ref{fig:degeneracies} the sign($\Delta
+m^2_{31}$) degeneracy has practically no effect on the $\theta_{13}$
+measurement, whereas the octant degeneracy has very little impact on
+the determination of $\delCP$.
+
+\begin{figure}[!t]
+\centering
+\includegraphics[width=0.9\textwidth]{./fig7.eps}
+%
+  \mycaption{Allowed regions in $\sin^22\theta_{13}$ and
+  $\delta_\mathrm{CP}$ for 5~years data (neutrinos only) from \BB,
+  SPL, and the combination. $\mathrm{H^{tr/wr} (O^{tr/wr})}$ refers to
+  solutions with the true/wrong mass hierarchy (octant of
+  $\theta_{23}$). For the colored regions in the left panel also
+  5~years of atmospheric data are included; the solution with the
+  wrong hierarchy has $\Delta\chi^2 = 4$. The true parameter
+  values are $\delta_\mathrm{CP} = -0.85 \pi$, $\sin^22\theta_{13} =
+  0.03$, $\sin^2\theta_{23} = 0.6$, and the values from
+  Eq.~(\ref{eq:default-params}) for the other parameters. For the \BB\
+  only analysis (middle panel) an external accuracy of 2\% (3\%) for
+  $|\Delta m^2_{31}|$ ($\theta_{23}$) has been assumed, whereas for
+  the left and right panel the default value of 10\% has been used.}
+\label{fig:degeneracies_5yrs}
+\end{figure}
+
+Fig.~\ref{fig:degeneracies} shows also that the fake solutions occur
+at similar locations in the ($\stheta$, $\delCP$) plane for \BB\ and
+SPL. Therefore, as noted in Ref.~\cite{Donini:2004hu}, in this sense
+the two experiments are not complementary, and the combination of
+10~years of \BB\ and SPL data is not very effective in resolving
+degeneracies. This is obvious since the baseline is the same and the
+neutrino energies are similar.
+%
+Note however, that the \BB\ looks for $\nu_e\to\nu_\mu$ appearance,
+whereas in SPL the T-conjugate channel $\nu_\mu\to\nu_e$ is observed.
+Assuming CPT invariance the relation $P_{\nu_\alpha\to\nu_\beta} =
+P_{\bar\nu_\beta\to\bar\nu_\alpha}$ holds, which implies that the
+antineutrino measurement can be replaced by a measurement in the
+T-conjugate channel.  Hence, if \BB\ and SPL experiments are available
+simultaneously the full information can be obtained just from neutrino
+data, and in principle the (time consuming) antineutrino measurement 
+is not necessary. As shown in Fig.~\ref{fig:degeneracies_5yrs} the
+combination of 5~yrs neutrino data from the \BB\ with 5~yrs of
+neutrino data from SPL leads to a result very close to the 10~yrs
+neutrino+antineutrino data from one experiment alone. Hence, if \BB\
+and SPL experiments are available simultaneously the data taking
+period is reduced approximately by a factor of 2 with respect to a
+single experiment. This synergy is discussed later in
+Sec.~\ref{sec:synergies-beams} in the context of the $\theta_{13}$ and
+CP violation discovery potentials.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Physics potential}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:sensitivities}
+
+\subsection{Sensitivity to the atmospheric parameters}
+\label{sec:atm}
+
+The $\nu_\mu$ disappearance channel available in the Super Beam
+experiments SPL and T2HK allows a precise determination of the
+atmospheric parameters $|\Delta m^2_{31}|$ and $\sin^22\theta_{23}$,
+see, e.g., Refs.~\cite{Antusch:2004yx,Minakata:2004pg,Donini:2005db}
+for recent analyses). Fig.~\ref{fig:atm-params} illustrates the
+improvement on these parameters by Super Beam experiments with respect
+to the present knowledge from SK atmospheric and K2K data. We show the
+allowed regions at 99\%~CL for T2K-I, SPL, and T2HK, where in all
+three cases 5~years of neutrino data are assumed. T2K-I corresponds to
+the phase~I of the T2K experiment with a beam power of 0.77~MW and the
+Super-Kamiokande detector as target~\cite{T2K}. In Tab.~\ref{tab:atm-params} we
+give the corresponding relative accuracies at 3$\sigma$ for $|\Delta
+m^2_{31}|$ and $\sin^2\theta_{23}$.
+
+\begin{figure}[!t]
+\centering
+  \includegraphics[width=0.55\textwidth]{./fig8.eps}
+  \mycaption{\label{fig:atm-params} Allowed regions of $\Delta
+  m^2_{31}$ and $\sin^2\theta_{23}$ at 99\%~CL (2 d.o.f.)  after 5~yrs
+  of neutrino data taking for SPL, T2K phase~I, T2HK, and the
+  combination of SPL with 5~yrs of atmospheric neutrino data in the
+  MEMPHYS detector. For the true parameter values we use $\Delta
+  m^2_{31} = 2.2\, (2.6) \times 10^{-3}~\mathrm{eV}^2$ and
+  $\sin^2\theta_{23} = 0.5 \, (0.37)$ for the test point 1 (2), and
+  $\theta_{13} = 0$ and the solar parameters as given in
+  Eq.~(\ref{eq:default-params}). The shaded region corresponds to the
+  99\%~CL region from present SK and K2K data~\cite{Maltoni:2004ei}.}
+\end{figure}
+
+
+\begin{table}[!t]
+  \centering
+  \begin{tabular}{lcrrr}
+  \hline\noalign{\smallskip}
+    & True values  & T2K-I & SPL & T2HK \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  $\Delta m^2_{31}$   & $2.2\cdot 10^{-3}$ eV$^2$ & 4.7\% & 3.2\% & 1.1\% \\
+  $\sin^2\theta_{23}$ & $0.5$                     & 20\%  & 20\%  & 6\%   \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  $\Delta m^2_{31}$   & $2.6\cdot 10^{-3}$ eV$^2$ & 4.4\% & 2.5\% & 0.7\% \\
+  $\sin^2\theta_{23}$ & $0.37$                    & 8.9\% & 3.1\% & 0.8\% \\
+  \noalign{\smallskip}\hline
+  \end{tabular}
+  \mycaption{Accuracies at $3\sigma$ on the atmospheric parameters
+  $|\Delta m^2_{31}|$ and $\sin^2\theta_{23}$ for 5 years of neutrino
+  data from T2K-I, SPL, and T2HK for the two test points shown in
+  Fig.~\ref{fig:atm-params} ($\theta^\mathrm{true}_{13} = 0$). The
+  accuracy for a parameter $x$ is defined as $(x^\mathrm{upper} -
+  x^\mathrm{lower})/(2 x^\mathrm{true})$, where $x^\mathrm{upper}$
+  ($x^\mathrm{lower}$) is the upper (lower) bound at 3$\sigma$ for
+  1~d.o.f.\ obtained by projecting the contour $\Delta \chi^2 = 9$
+  onto the $x$-axis. For the accuracies for test point~2 the octant
+  degenerate solution is neglected.\label{tab:atm-params}}
+\end{table}
+
+From the figure and the table it becomes evident that the T2K setups
+are very good in measuring the atmospheric parameters, and only a
+modest improvement is possible with SPL with respect to T2K phase~I.
+T2HK provides an excellent sensitivity for these parameters, and for
+the example of the test point~2 sub-percent accuracies are obtained at
+3$\sigma$. The disadvantage of SPL with respect to T2HK is the
+limited spectral information. Because of the lower beam energy
+nuclear Fermi motion is a severe limitation for energy reconstruction
+in SPL, whereas in T2K the somewhat higher energy allows an efficient
+use of spectral information of quasi-elastic events. Indeed, due to
+the large number of events in the disappearance channel (cf.\
+Tab.~\ref{tab:events}) the measurement is completely dominated by the
+spectrum, and even increasing the normalization uncertainty up to
+100\% has very little impact on the allowed regions. The effect of
+spectral information on the disappearance measurement is
+discussed in some detail in Ref.~\cite{Donini:2005db}.
+
+For the test point~1, with maximal mixing for $\theta_{23}$, rather
+poor accuracies of $\sim20\%$ for T2K-I and SPL, and $6\%$ for T2HK
+are obtained for $\sin^2\theta_{23}$. The reason is that in the
+disappearance channel $\sin^22\theta_{23}$ is measured with high
+precision, which translates to rather large errors for
+$\sin^2\theta_{23}$ if $\theta_{23} = \pi/4$~\cite{Minakata:2004pg}.
+%
+For the same reason it is difficult to resolve the octant degeneracy,
+and for the test point~2, with a non-maximal value of
+$\sin^2\theta_{23} = 0.37$, for all three LBL experiments the
+degenerate solution is present around $\sin^2\theta_{23} = 0.63$.
+%
+As pointed out in Refs.~\cite{Peres:2003wd,Gonzalez-Garcia:2004cu}
+atmospheric neutrino data may allow to distinguish between the two
+octants of $\theta_{23}$. If 5~years of atmospheric neutrino data in
+MEMPHYS are added to the SPL data, the degenerate solution for the
+test point~2 can be excluded at more than $5\sigma$ and hence the
+octant degeneracy is resolved in this example, see
+Sec.~\ref{sec:atmospherics} for a more detailed discussion.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The $\theta_{13}$ discovery potential}
+\label{sec:th13}
+
+If no finite value of $\theta_{13}$ is discovered by the next round of
+experiments an important task of the experiments under consideration
+here is to push further the sensitivity to this parameter. In this
+section we address this problem, where we use to following definition
+of the $\theta_{13}$ discovery potential: Data are simulated for a
+finite true value of $\stheta$ and a given true value for $\delCP$. If
+the $\Delta\chi^2$ of the fit to these data with $\theta_{13} = 0$ is
+larger than 9 the corresponding true value of $\theta_{13}$ ``is
+discovered at 3$\sigma$''. In other words, the $3\sigma$ discovery
+limit as a function of the true $\delCP$ is given by the true value of
+$\stheta$ for which $\Delta\chi^2(\theta_{13}=0) = 9$. In the fitting
+process we minimize the $\Delta\chi^2$ with respect to $\theta_{12}$,
+$\theta_{23}$, $\Delta m^2_{12}$, and $\Delta m^2_{31}$, and in
+general one has to test also for degenerate solutions in sign($\Delta
+m^2_{31}$) and the octant of $\theta_{23}$.
+
+\begin{figure}
+  \centering \includegraphics[width=0.9\textwidth]{./fig9.eps}
+  \mycaption{$3\sigma$ discovery sensitivity to $\stheta$ for \BB,
+  SPL, and T2HK as a function of the true value of \delCP\ (left
+  panel) and as a function of the fraction of all possible values of
+  \delCP\ (right panel). The width of the bands corresponds to values
+  for the systematical errors between 2\% and 5\%. The black curves
+  correspond to the combination of \BB\ and SPL with 10~yrs of total
+  data taking each for a systematical error of 2\%, and the dashed
+  curves show the sensitivity of the \BB\ when the number of ion
+  decays/yr are reduced by a factor of two with respect to the values
+  given in Tab.~\ref{tab:setups}.\label{fig:th13}}
+\end{figure}
+
+The discovery limits are shown for \BB, SPL, and T2HK in
+Fig.~\ref{fig:th13}. One observes that SPL and T2HK are rather similar
+in performance, whereas the \BB\ with our standard fluxes performs
+significantly better. For all three facilities a guaranteed discovery
+reach of $\stheta \simeq 5\times 10^{-3}$ is obtained, irrespective of
+the actual value of \delCP, however, for certain values of \delCP\ the
+sensitivity is significantly improved. For SPL and T2HK discovery
+limits around $\stheta \simeq 10^{-3}$ are possible for a large
+fraction of all possible values of \delCP, whereas for our standard
+\BB\ a sensitivity below $\stheta = 4\times 10^{-4}$ is reached for
+80\% of all possible values of \delCP. If 10~years of data from \BB\
+and SPL are combined the discovery limit is dominated by the \BB.
+%
+Let us stress that the \BB\ performance depends crucially on the
+neutrino flux intensity, as can be seen from the dashed curves in
+Fig.~\ref{fig:th13}, which has been obtained by reducing the number of
+ion decays/yr by a factor of two with respect to our standard values
+given in Tab.~\ref{tab:setups}. In this case the sensitivity decreases
+significantly, but still values slightly better than from the
+Super Beam experiments are reached.
+
+In Fig.~\ref{fig:th13} we illustrate also the effect of systematical
+errors on the $\theta_{13}$ discovery reach. The lower boundary of the
+band for each experiment corresponds to a systematical error of 2\%,
+whereas the upper boundary is obtained for 5\%. These errors include
+the (uncorrelated) normalization uncertainties on the signal as well
+as on the background, where the crucial uncertainty is the error on
+the background. We find that the \BB\ is basically not affected by
+these errors, since the background has a rather different spectral
+shape (strongly peaked at low energies) than the signal. The fact
+that T2HK is relatively strongly affected by the actual value of the
+systematics can by understood by considering the ratio of signal to
+the square-root of the background using the numbers of
+Tab.~\ref{tab:events}. We shall discuss this issue in more detail in
+the next section in the context of the CP violation discovery reach.
+
+Let us remark that the $\theta_{13}$ sensitivities are practically not
+affected by the sign($\Delta m^2_{31}$)-degeneracy. This is easy to
+understand, since the data is fitted with $\theta_{13} = 0$, and in
+this case both mass hierarchies lead to very similar event rates. If
+the inverted hierarchy is used as the true hierarchy, the peak in the
+discovery limit visible in the left panel of Fig.~\ref{fig:th13}
+around $\delCP \sim \pi$ moves to $\delCP \sim 0$. However, the
+characteristic shape of the curves, and in particular, the sensitivity
+as a function of the \delCP-fraction shown in the right panel are
+hardly affected by the sign of the true $\Delta m^2_{31}$.
+%
+In case of a non-maximal value of $\theta_{23}$ the octant-degeneracy
+has a minor impact on the $\theta_{13}$ discovery potential, as
+illustrated in Fig.~\ref{fig:SPLTheta13Disco} for the SPL. We show the
+discovery limit obtained with the true and the fake octant of
+$\theta_{23}$ for a true value of $\sin^2\theta_{23}= 0.6$. Let us
+note that for true values of $\sin^2\theta_{23} > 0.5$ the
+octant-degenerate solution leads to a worse sensitivity to
+$\theta_{13}$ (see figure), whereas for $\sin^2\theta_{23} < 0.5$ the
+fake solution does not affect the $\theta_{13}$ discovery, since in
+this case the sensitivity is increased.
+
+\begin{figure}
+  \centering
+  \includegraphics[width=0.9\textwidth]{./fig10.eps}
+  \mycaption{\label{fig:SPLTheta13Disco} $3\sigma$ discovery
+  sensitivity to $\stheta$ for the SPL as a function of the true value
+  of \delCP\ for $\sin^2\theta_{23}^\mathrm{true} = 0.6$ and true values for
+  the other parameters as given in Eq.~(\ref{eq:default-params}).}
+\end{figure}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{Sensitivity to CP violation}
+\label{sec:CPV}
+
+In case a finite value of $\theta_{13}$ is established it is important
+to quantitatively assess the discovery potential for leptonic CP
+violation (CPV). The CP symmetry is violated if the complex phase
+\delCP\ is different from $0$ and $\pi$. Therefore, CPV is discovered
+if these values for \delCP\ can be excluded. 
+%
+We evaluate the discovery potential for CPV in the following way:
+Data are calculated by scanning the true values of $\stheta$ and
+$\delCP$. Then these data are fitted with the CP conserving values
+$\delCP = 0$ and $\delCP = \pi$, where all parameters except \delCP\
+are varied and the sign and octant degeneracies are taken into
+account. If no fit with $\Delta \chi^2 < 9$ is found CP conserving
+values of \delCP\ can be excluded at $3\sigma$ for the chosen values
+of $\delta_\mathrm{CP}^\mathrm{true}$ and $\stheta^\mathrm{true}$.
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.65\textwidth]{./fig11.eps}
+%   
+   \mycaption{CPV discovery potential for \BB, SPL, and T2HK: For
+   parameter values inside the ellipse-shaped curves CP conserving
+   values of \delCP\ can be excluded at $3\sigma$ $(\Delta\chi^2>9)$.
+   The width of the bands corresponds to values for the systematical
+   errors from 2\% to 5\%. The dashed curves show the sensitivity of
+   the \BB\ when the number of ion decays/yr are reduced by a factor
+   of two with respect to the values given in Tab.~\ref{tab:setups}
+   for 2\% systematics.\label{fig:CPV}}
+\end{figure}
+
+The CPV discovery potential for \BB, SPL, and T2HK is shown in
+Fig.~\ref{fig:CPV}. As in the case of the $\theta_{13}$ sensitivity we
+find that SPL and T2HK perform rather similar, whereas the \BB\ has
+significantly better sensitivity if our adopted numbers of ion decays
+per year can be achieved. For systematical errors of 2\% maximal CPV
+(for $\delCP^\mathrm{true} = \pi/2, \, 3\pi/2$) can be discovered at
+$3\sigma$ down to $\stheta \simeq 8.8 \,(6.6)\times 10^{-4}$ for SPL
+(T2HK), and $\stheta \simeq 2\times 10^{-4}$ for the \BB. This number
+for the \BB\ is increased by a factor 3 if the fluxes are reduced to
+half of our nominal values.  The best sensitivity to CPV is obtained
+for all three facilities around $\stheta \sim 10^{-2}$. For this value
+CPV can be established for 78\%, 73\%, 75\% of all values of \delCP\
+for \BB, SPL, T2HK, respectively (again for systematics of 2\%).
+
+The widths of the bands in Fig.~\ref{fig:CPV} corresponds to different
+values for systematical errors. The curves which give the best
+sensitivities are obtained for systematics of 2\%, the curves
+corresponding to the worst sensitivity have been computed for
+systematics of 5\%. We change the uncertainty on the signal as well as
+on the background, however, it turns out that the most relevant
+uncertainty is the background normalization. We find that the impact
+of systematics is very small for the \BB. The reason for this is that
+the spectral shape of the background in the \BB\ (from pions and
+atmospheric neutrinos) is very different from the signal, and
+therefore they can be disentangled by the fit of the energy spectrum.
+For the Super Beams the background spectrum is more similar to the
+signal, and therefore an uncertainty on the backgound normalization
+might have a strong impact on the sensitivity, as visible from the SPL
+and T2HK curves in Fig.~\ref{fig:CPV}. In particular T2HK is strongly
+affected, and moving from 2\% to 5\% uncertainy decreases the
+sensitivity to maximal CPV by a factor 3.
+
+This interesting feature can be understood in the following way. A
+rough measure to estimate the sensitivity is given by the signal
+compared to the error on the background. The latter receives
+contributions from the statistical error $\sqrt{B}$ and from the
+systematical uncertainty $\sigma_\mathrm{bkgr}B$, where $B$ is the
+number of background events and $\sigma_\mathrm{bkgr}$ is the
+(relative) systematical error. Hence the importance of the systematics
+can be estimated by the ratio of systematical and statistical errors
+$\sigma_\mathrm{bkgr} B / \sqrt{B} = \sigma_\mathrm{bkgr} \sqrt{B}$.
+Summing the numbers for background events in the neutrino and
+antineutrino channels given in Tab.~\ref{tab:events} one finds that
+systematical errors dominate ($\sigma_\mathrm{bkgr} \sqrt{B} > 1$) if
+$\sigma_\mathrm{bkgr} \gtrsim 6\%,\, 3\%, \, 2\%$ for \BB, SPL, T2HK,
+respectively. 
+%
+In the right panel Fig.~\ref{fig:systematics} we show the sensitivity
+to maximal CPV (as defined in the figure caption) as a function of
+$\sigma_\mathrm{bkgr}$. Indeed, the worsening of the sensitivity due
+to systematics occurs roughly at the values of $\sigma_\mathrm{bkgr}$
+as estimated above. For a more quantitative understanding of these
+curves it is necessary to consider the number of signal and background
+events for neutrinos and antineutrinos separately, as well as to take
+into account spectral information.
+
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.9\textwidth]{./fig12.eps}
+%   
+   \mycaption{Impact of total exposure and systematical errors on the
+   CPV discovery potential of \BB, SPL, and T2HK. We show the
+   smallest true value of $\stheta$ for which $\delCP = \pi/2$ can be
+   distinguished from $\delCP = 0$ or $\delCP = \pi$ at $3\sigma$
+   $(\Delta\chi^2>9)$ as a function of the exposure in kt~yrs (left)
+   and as a function of the systematical error on the background
+   $\sigma_\mathrm{bkgr}$ (right). The widths of the curves in the
+   left panel corresponds to values of $\sigma_\mathrm{bkgr}$ from 2\%
+   to 5\%. The thin solid curves in the left panel corresponds to no
+   systematical errors. The right plot is calculated for the standard
+   exposure of 4400~kt~yrs. No systematical error on the signal has
+   been assumed. \label{fig:systematics}}
+\end{figure}
+
+The left panel of Fig.~\ref{fig:systematics} shows the sensitivity to
+maximal CPV as a function of the exposure\footnote{Note that the CPV
+sensitivity for the \BB\ with reduced fluxes from Fig.~\ref{fig:CPV}
+is worse than the value which follows from Fig.~\ref{fig:systematics}.
+The reason is that in Fig.~\ref{fig:systematics} the total exposure is
+scaled (mass~$\times$~time), i.e., signal and background are scaled in
+the same way, whereas for the dashed curve in Fig.~\ref{fig:CPV} only
+the fluxes are reduced but backgrounds are kept constant.} for values
+of $\sigma_\mathrm{bkgr}$ from 2\% to 5\%. One can observe clearly
+that for the standard exposure of 4400~kt~yrs T2HK is dominated by
+systematics and changing $\sigma_\mathrm{bkgr}$ from 2\% to 5\% has a
+big impact on the sensitivity. In contrast the CERN--MEMPHYS
+experiments (especially the \BB) are rather stable with respect to
+systematics and for the standard exposure they are still statistics
+dominated. We conclude that in T2HK systematics have to be under very
+good control\footnote{As a possible solution to this problem for T2HK
+it has been proposed in Ref.~\cite{Ishitsuka:2005qi} to place one half
+of the Hyper-K detector mass at Kamioka and the second half at the
+same off-axis angle in Korea.}, whereas this issue is less important
+for \BB\ and SPL.
+%
+We have checked explicitly that the systematical error on the signal
+has negligible impact on these results. Therefore, we have set this
+error to zero for calculating Fig.~\ref{fig:systematics} to highlight
+the importance of the background error. In all other calculations also
+the signal error is included, in particular also in Fig.~\ref{fig:CPV}.
+
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.8\textwidth]{./fig13.eps}
+%   
+   \mycaption{Impact of degeneracies on the CPV discovery potential
+   for the \BB. We show the sensitivity to CPV at $3\sigma$
+   $(\Delta\chi^2>9)$ computed for 4 different combinations of the
+   true values of the hierarchy (NH or IH) and $\theta_{23}$
+   ($\sin^2\theta_{23} = 0.4$ or $0.6$). Dashed curves are computed
+   neglecting degeneracies in the fit.\label{fig:deltacp}}
+\end{figure}
+
+Finally, in Fig.~\ref{fig:deltacp} we illustrate the impact of
+degeneracies, as well as the true hierarchy and \thetatt-octant on the
+CPV sensitivity.  Curves of different colors correspond to the four
+different choices for \sigdm\ and the \thetatt-octant of the true
+parameters. For the solid curves the simulated data for each choice of
+true \sigdm\ and \thetatt-octant are fitted by taking into account all
+four degenerate solutions, i.e., also for the fit all four
+combinations of \sigdm\ and \thetatt-octant are used. One observes
+from the figure that the true hierarchy and octant have a rather small
+impact on the \BB\ CPV sensitivity, in particular the sensitivity to
+maximal CPV is completely independent.  The main effect of changing the
+true hierarchy is to exchange the behavior between $0 < \delCP <
+180^\circ$ and $180^\circ < \delCP < 360^\circ$. For $\stheta \lesssim
+10^{-2}$ the sensitivity gets slightly worse if
+$\thetatt^\mathrm{true} > \pi/4$ compared to $\thetatt^\mathrm{true} <
+\pi/4$.
+
+The dashed curves in Fig.~\ref{fig:deltacp} are computed without
+taking into account the degeneracies, i.e., for each choice of true
+\sigdm\ and \thetatt-octant the data are fitted only with this
+particular choice. The effect of the degeneracies becomes visible for
+large values of \thetaot. Note that this is just the region where they
+can be reduced by a combined analysis with atmospheric neutrinos (see
+Sec.~\ref{sec:atmospherics} or Ref.~\cite{Huber:2005ep}).
+ 
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Synergies provided by the CERN--MEMPHYS facilities}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:synergies}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{Combining Beta Beam and Super Beam}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:synergies-beams}
+
+In this section we discuss synergies which emerge if both \BB\ and SPL
+are available. The main difference between these two beams is the
+different initial neutrino flavor,
+$\stackrel{\scriptscriptstyle(-)}{\nu}_e$ for \BB\ and
+$\stackrel{\scriptscriptstyle (-)}{\nu}_\mu$ for SPL. This implies
+that at near detectors all relevant cross sections can be measured. In
+particular, the near detector of the \BB\ will measure the cross
+section for the SPL appearance search, and vice versa.
+%
+If both experiments run with neutrinos and antineutrinos all possible
+transition probabilities are covered: $P_{\nu_e\to\nu_\mu}$,
+$P_{\bar\nu_e\to\bar\nu_\mu}$, $P_{\nu_\mu\to\nu_e}$, and
+$P_{\bar\nu_\mu\to\bar\nu_e}$. Together with the fact that matter
+effects are very small because of the relatively short baseline, this
+means that in addition to CP also direct tests of the T and CPT
+symmetries are possible.
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.9\textwidth]{./fig14.eps}
+%   
+   \mycaption{Discovery potential of a finite value of $\stheta$ at
+   $3\sigma$ $(\Delta\chi^2>9)$ for 5~yrs neutrino data from
+   \BB, SPL, and the combination of \BB\ + SPL compared to
+   10~yrs data from T2HK (2~yrs neutrinos + 8~yrs antineutrinos).
+   \label{fig:th13-5yrs}}
+\end{figure}
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.6\textwidth]{./fig15.eps}
+%   
+   \mycaption{Sensitivity to CPV at $3\sigma$ $(\Delta\chi^2>9)$ for
+   combining 5~yrs neutrino data from \BB\ and SPL compared to
+   10~yrs data from T2HK (2~yrs neutrinos + 8~yrs antineutrinos).
+   \label{fig:CP-5yrs}}
+\end{figure}
+
+However, if the CPT symmetry is assumed in principle all information
+can be obtained just from neutrino data because of the relations
+$P_{\bar\nu_e\to\bar\nu_\mu} = P_{\nu_\mu\to\nu_e}$ and
+$P_{\bar\nu_\mu\to\bar\nu_e} = P_{\nu_e\to\nu_\mu}$. As mentioned
+already in Sec.~\ref{sec:degeneracies} this implies that (time
+consuming) antineutrino running can be avoided. We illustrate this
+synergy in Figs.~\ref{fig:th13-5yrs} and \ref{fig:CP-5yrs}. In
+Fig.~\ref{fig:th13-5yrs} we show the $\theta_{13}$ discovery potential
+of 5 years of neutrino data from \BB\ and SPL. From the left panel the
+complementarity of the two experiments is obvious, since each of them
+is most sensitive in a different region of \delCP. (As expected from
+general properties of the oscillation probabilities the sensitivity
+curves of \BB\ and SPL are approximately related by the transformation
+$\delCP \to 2\pi - \delCP$.) Combining these two data sets results in
+a sensitivity slightly better than from 10 years (2$\nu$+8$\bar\nu$)
+of T2HK data.
+%
+As visible in Fig.~\ref{fig:CP-5yrs} also for the CPV discovery this
+synergy works and 5 years of neutrino data from \BB\ and SPL lead to a
+similar sensitivity as 10 years of T2HK.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{Resolving degeneracies with atmospheric neutrinos}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:atmospherics}
+
+It was pointed out in Ref.~\cite{Huber:2005ep} that for LBL
+experiments based on mega ton scale water \v{C}erenkov detectors data
+from atmospheric neutrinos (ATM) provide an attractive method to
+resolve degeneracies. Atmospheric neutrinos are sensitive to the
+neutrino mass hierarchy if $\theta_{13}$ is sufficiently large due to
+Earth matter effects, mainly in multi-GeV $e$-like
+events~\cite{Petcov:1998su,Akhmedov:1998ui,Bernabeu:2003yp}. Moreover,
+sub-GeV $e$-like events provide sensitivity to the octant of
+$\theta_{23}$~\cite{Kim:1998bv,Peres:2003wd,Gonzalez-Garcia:2004cu}
+due to oscillations with $\Delta m^2_{21}$ (see also
+Ref.~\cite{Kajita} for a discussion of atmospheric neutrinos in the
+context of Hyper-K). 
+%
+Following Ref.~\cite{Huber:2005ep} we investigate here the synergy
+from a combination of LBL data from \BB\ and SPL with ATM data in the
+MEMPHYS detector. A general three-flavor analysis of ATM data is
+performed based on Ref.~\cite{Gonzalez-Garcia:2004cu} and references
+therein. 
+%
+We include fully-contained $e$-like and $\mu$-like events (further
+divided into sub-GeV $p_l<400$~MeV, sub-GeV $p_l > 400$~MeV, and
+Multi-GeV events), partially-contained $\mu$-like events, stopping
+muons, and through-going muons. Each of these data samples is divided
+into 10 zenith bins, so we have a total of 90 data points. The
+simulation of the atmospheric event rates has been adapted to the
+actual geometry of the MEMPHYS detector proposal (see
+Fig.~\ref{fig:MEMPHYS}). Details of the statistical analysis can be
+found in Ref.~\cite{Gonzalez-Garcia:2004wg}. Note that our analysis of
+atmospheric data is conservative, since there is room for improvement
+by including multi-ring events as well as by optimizing the energy
+binning.\footnote{The impact of energy binning on the hierarchy
+determination with atmospheric neutrinos has been discussed recently
+in Ref.~\cite{Petcov:2005rv} in the context of magnetized iron
+detectors.}
+ 
+\begin{figure}[!t]
+\centering
+  \includegraphics[width=0.9\textwidth]{./fig16.eps}
+%
+  \mycaption{Sensitivity to the mass hierarchy at $2\sigma$
+  $(\Delta\chi^2 = 4)$ as a function of the true values of
+  $\sin^22\theta_{13}$ and $\delta_\mathrm{CP}$ (left), and the
+  fraction of true values of $\delCP$ (right). The solid curves are
+  the sensitivities from the combination of long-baseline and
+  atmospheric neutrino data, the dashed curves correspond to
+  long-baseline data only. For comparison we show in the right panel
+  also the sensitivities of NO$\nu$A and NO$\nu$A+T2K extracted from
+  Fig.~13.14 of Ref.~\cite{Ayres:2004js}. For the curve labeled
+  ``NO$\nu$A (p.dr.)+T2K@4~MW'' a proton driver has been assumed for
+  NO$\nu$A and the T2K beam has been up-graded to 4~MW, see
+  Ref.~\cite{Ayres:2004js} for details.}
+  \label{fig:hierarchy}
+\end{figure}
+
+The effect of degeneracies in LBL data has been discussed in
+Sec.~\ref{sec:degeneracies}, see Figs.~\ref{fig:degeneracies} and
+\ref{fig:degeneracies_SPL}. As discussed there, for given true
+parameter values the data can be fitted with the wrong hierarchy
+and/or with the wrong octant of $\theta_{23}$. Hence, from LBL data
+alone the hierarchy and the octant cannot be determined and
+ambiguities exist in the determination of $\theta_{13}$ and
+$\delta_\mathrm{CP}$.
+%
+If the LBL data are combined with ATM data only the colored regions in
+Fig.~\ref{fig:degeneracies} survive, i.e., in this particular example
+for SPL and T2HK the degeneracies are completely lifted at 95\%~CL,
+the mass hierarchy and the octant of $\theta_{23}$ can be identified,
+and the ambiguities in $\theta_{13}$ and $\delta_\mathrm{CP}$ are
+resolved. For the \BB\ an island corresponding to the wrong hierarchy
+does survive at the 95\%~CL for 2~dof. Still, the solution with the
+wrong sign of $\Delta m^2_{31}$ is disfavored with $\Delta\chi^2 =
+5.1$ with respect to the true solution, which corresponds to
+2.4$\sigma$ for 1~dof.
+%
+Let us note that in Fig.~\ref{fig:degeneracies} we have chosen a
+favorable value of $\sin^2\theta_{23} = 0.6$; for values
+$\sin^2\theta_{23} < 0.5$ in general the sensitivity of ATM data is
+weaker~\cite{Huber:2005ep}.
+
+In Fig.~\ref{fig:hierarchy} we show how the combination of ATM+LBL
+data leads to a non-trivial sensitivity to the neutrino mass
+hierarchy, i.e.\ to the sign of $\Delta m^2_{31}$. For LBL data alone
+(dashed curves) there is practically no sensitivity for the
+CERN--MEMPHYS experiments (because of the very small matter effects
+due to the relatively short baseline), and the sensitivity of T2HK
+depends strongly on the true value of $\delta_\mathrm{CP}$. However,
+by including data from atmospheric neutrinos (solid curves) the mass
+hierarchy can be identified at $2\sigma$~CL provided
+$\sin^22\theta_{13} \gtrsim 0.03-0.05$ for \BB\ and SPL, and
+$\sin^22\theta_{13} \gtrsim 0.02-0.03$ for T2HK, where for the CERN
+experiments the sensitivity shows somewhat more dependence on the true
+value of $\delta_\mathrm{CP}$. As an example we have chosen in that
+figure a true value of $\theta_{23} = \pi/4$. Generically the
+hierarchy sensitivity increases with increasing $\theta_{23}$, see
+Ref.~\cite{Huber:2005ep} for a detailed discussion.
+
+Although \BB\ and SPL alone have no sensitivity to the hierarchy at
+all, we find that the combination of them does provide rather good
+sensitivity even without atmosheric data. The reason for this
+interesting effect is the following. Because of the rather short
+baseline the matter effect is too small to distinguish between NH and
+IH given only neutrino and antineutrino information in one channel.
+However, the tiny matter effect suffices to move the hierarchy
+degenerate solution to slightly different locations in the ($\stheta$,
+$\delCP$) plane for the $\stackrel{\scriptscriptstyle(-)}{\nu}_e \to
+\stackrel{\scriptscriptstyle (-)}{\nu}_\mu$ (\BB) and
+$\stackrel{\scriptscriptstyle(-)}{\nu}_\mu \to
+\stackrel{\scriptscriptstyle (-)}{\nu}_e$ (SPL) channels (compare
+Fig.~\ref{fig:degeneracies}). Hence, if all four CP and T conjugate
+channels are available (as it is the case for the \BB+SPL combination)
+already the small matter effect picked up allong the 130~km
+CERN--MEMPHYS distance provides sensitivity to the mass hierarchy for
+$\sin^22\theta_{13} \gtrsim 0.03$, or $\sin^22\theta_{13} \gtrsim 0.02$
+if also atmospheric neutrino data is included.
+
+For comparison we show in the right panel of Fig.~\ref{fig:hierarchy}
+also the sensitivity of the NO$\nu$A~\cite{Ayres:2004js} experiment,
+and of NO$\nu$A+T2K, where in the second case a beam upgrade by a
+proton driver has been assumed for NO$\nu$A, and for T2K the
+Super-Kamiokande detector has been used but the beam intensity has
+been increased by assuming 4~MW power. More details on these
+sensitivities can be found in Ref.~\cite{Ayres:2004js}.
+%
+Let us note that in general LBL experiments with two detectors (or the
+combination of two different LBL experiments) are a competitive method
+to atmospheric neutrinos for the hierarchy determination, see, e.g.,
+Refs.~\cite{Ishitsuka:2005qi,MenaRequejo:2005hn,Hagiwara:2005pe} for
+recent analyses.
+%
+We mention also the possibility to determine the neutrino mass
+hierarchy by using neutrino events from a galactic Super Nova
+explosion in mega ton \v{C}erenkov detectors such as MEMPHYS, see,
+e.g., Ref.~\cite{Kachelriess:2004vs}.
+
+\begin{figure}[!t]
+\centering
+  \includegraphics[width=0.55\textwidth]{./fig17.eps}
+%
+  \mycaption{$\Delta\chi^2$ of the solution with the wrong octant of
+  $\theta_{23}$ as a function of the true value of
+  $\sin^2\theta_{23}$. We have assumed a true value of $\theta_{13} =
+  0$.}
+  \label{fig:octant}
+\end{figure}
+
+Fig.~\ref{fig:octant} shows the potential of ATM+LBL data to exclude
+the octant degenerate solution. Since this effect is based mainly on
+oscillations with $\Delta m^2_{21}$ there is very good sensitivity
+even for $\theta_{13} = 0$; a finite value of $\theta_{13}$ in general
+improves the sensitivity~\cite{Huber:2005ep}.  From the figure one can
+read off that atmospheric data alone can can resolve the correct
+octant at $3\sigma$ if $|\sin^2\theta_{23} - 0.5| \gtrsim 0.085$. If
+atmospheric data is combined with the LBL data from SPL or T2HK there
+is sensitivity to the octant for $|\sin^2\theta_{23} - 0.5| \gtrsim
+0.05$. The improvement of the octant sensitivity with respect to
+previous analyses~\cite{Huber:2005ep,Gonzalez-Garcia:2004cu} follows
+from changes in the analysis of sub-GeV atmospheric events, where now
+three bins {\bf *** to be confirmed ***} in lepton momentum are used
+instead of one. Note that since in Fig.~\ref{fig:octant} we have
+assumed a true value of $\theta_{13} = 0$, combining the \BB\ with ATM
+does not improve the sensitivity with respect to atmospheric data
+alone.
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Summary}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:conclusions}
+
+In this work we have studied the physics potential of the
+CERN--MEMPHYS neutrino oscillation project. We consider a Beta Beam
+(\BB) with $\gamma = 100$ for the stored ions, where existing
+facilities at CERN can be used optimally, and a Super Beam based on an
+optimized Super Proton Linac (SPL) with a beam energy of 3.5~GeV and
+4~MW power. As target we assume the MEMPHYS detector, a 440~kt water
+\v{C}erenkov detector at Fr\'ejus, at a distance of 130~km from
+CERN. The main characteristics of the experiments are summarized in
+Tab.~\ref{tab:setups}.
+%
+The adopted neutrino fluxes are based on realistic calculations of ion
+production and storage for the \BB, and a full simulation of the beam
+line (particle production and decay of secondaries) for SPL. Special
+care has be given to the issue of backgrounds, which we include by
+means of detailed event simulations and applying Super-Kamiokande particle
+identification algorithms.
+
+The physics potential of the \BB\ and SPL experiments in terms of
+$\theta_{13}$ discovery reach and sensitivity to CP violation has been
+addressed where parameter degeneracies are fully taken into account.
+The main results on these performance indicators are summarized in
+Figs.~\ref{fig:th13} and \ref{fig:CPV}.
+%
+We obtain a guaranteed discovery reach of $\stheta \simeq 5\times
+10^{-3}$ at $3\sigma$, irrespective of the actual value of \delCP. For
+certain values of \delCP\ the sensitivity is significantly improved,
+and for \BB\ (SPL) discovery limits arround $\stheta \simeq 3\,(10)
+\times 10^{-4}$ are possible for a large fraction of all possible
+values of \delCP.
+%
+Maximal CP violation (for $\delCP^\mathrm{true} = \pi/2, \, 3\pi/2$)
+can be discovered at $3\sigma$ down to $\stheta \simeq 2\, (9)\times
+10^{-4}$ for \BB\ (SPL), whereas the best sensitivity to CP violation
+is obtained for $\stheta \sim 10^{-2}$: For $\stheta = 10^{-2}$ CP
+violation can be established at $3\sigma$ for 78\% (73\%) of all
+possible true values of \delCP\ for \BB\ (SPL).
+%
+We stress that the \BB\ performance in general depends crucially on
+the number of ion decays per year.
+%
+The impact of the value of systematical uncertainties on signal and
+background on our results is discussed.
+%
+The \BB\ and SPL sensitivities are compared to the ones of the
+phase~II of the T2K experiment in Japan (T2HK), which is a competing
+proposal of similar size and timescale. In general we obtain rather
+similar sensitivities for T2HK and SPL, and hence the CERN--MEMPHYS
+experiments provide a viable alternative to T2HK. We find that \BB\
+and SPL are less sensitive to systematical errors, whereas the
+sensitivity of T2HK crucially depends on the systematical error on the
+background.\footnote{Let us note that in the present study we have not
+considered the recent ``T2KK'' proposal~\cite{Ishitsuka:2005qi}, where
+one half of the Hyper-K detector mass is at Kamioka and the second
+half in Korea. For such a setup our results do not apply and
+especially the conclusion on systematical errors may be different.}
+
+Assuming that both \BB\ and SPL experiments are available, we point
+out that one can benefit from the different oscillation channels
+$\nu_e\to\nu_\mu$ for \BB\ and $\nu_\mu\to\nu_e$ for SPL, since by the
+combination of these channels the time intensive antineutrino
+measurements can be avoided. We show that 5 years of neutrino data from
+\BB\ and SPL lead to similar results as 2 years of neutrino plus 8
+years of antineutrino data from T2HK.
+%
+Furthermore, we discuss the use of atmospheric neutrinos in the
+MEMPHYS detector to resolve parameter degeneracies in the
+long-baseline data. This effect leads to a sensitivity to the neutrino
+mass hierarchy at $2\sigma$~CL for $\sin^22\theta_{13} \gtrsim
+0.03-0.05$ for \BB\ and SPL, although these experiments alone (without
+atmospheric data) have no sensitivity at all. The optimal hierarchy
+sensitivity is obtained from combining \BB+SPL+atmospheric data.
+Furthermore, the combination of atmospheric data with a Super Beam
+provides a possibility to determine the octant of $\theta_{23}$.
+
+To conclude, we have shown that the CERN--MEMPHYS neutrino oscillation
+project based on a Beta Beam and/or a Super Beam plus a mega ton scale
+water \v{C}erenkov detector offers interesting and competitive physics
+possibilities and is worth to be considered as a serious option in
+the worldwide process of identifying future high precision neutrino
+oscillation facilities~\cite{ISSpage}.
+
+\subsection*{Acknowledgment}
+
+We thank J.~Argyriades for communication on the Super-K atmospheric
+neutrino analysis, A.~Cazes for his work on the SPL simulation, and
+P.~Huber for his patience in answering questions concerning the use of
+GLoBES. T.S.\ is supported by the $6^\mathrm{th}$~Framework Program
+of the European Community under a Marie Curie Intra-European
+Fellowship.
+
+
+%\newpage
+\begin{thebibliography}{99}
+
+\bibitem{solar}
+  B.~T.~Cleveland {\it et al.},
+  Astrophys.\ J.\  {\bf 496} (1998) 505;
+  %%CITATION = ASJOA,496,505;%%
+%
+  J.N.~Abdurashitov {\it et al.}  [SAGE],
+  J.\ Exp.\ Theor.\ Phys.\  {\bf 95} (2002) 181
+  % [Zh.\ Eksp.\ Teor.\ Fiz.\  {\bf 122} (2002) 211].
+  [astro-ph/0204245];
+  %%CITATION = ASTRO-PH 0204245;%%
+%
+  T. Kirsten {\it et al.} [GALLEX and GNO], 
+  Nucl. Phys. B (Proc. Suppl.)  {\bf 118} (2003) 33;
+%
+  S.~Fukuda {\it et al.} [Super-Kamiokande],
+  %``Determination of solar neutrino 
+  % oscillation parameters using 1496 days  of Super-Kamiokande-I data,''
+  Phys. Lett. {\bf B539} (2002) 179;
+%
+%\bibitem{ahmad:2002ka}
+  Q.R. Ahmad {\em et~al.} [SNO],
+  Phys. Rev. Lett. {\bf 89}, 011302 (2002) 
+  [nucl-ex/0204009];
+  %%CITATION = NUCL-EX 0204009;%%
+%
+%\bibitem{Aharmim:2005gt}
+  B.~Aharmim {\it et al.}  [SNO],
+  %``Electron energy spectra, fluxes, and day-night asymmetries of B-8 solar
+  %neutrinos from the 391-day salt phase SNO data set,''
+  Phys.\ Rev.\ C {\bf 72} (2005) 055502
+  [nucl-ex/0502021].
+  %%CITATION = NUCL-EX 0502021;%%
+
+\bibitem{sk-atm}
+%\bibitem{Fukuda:1998mi}
+  Super-Kamiokande Coll.,
+  Y.~Fukuda {\it et al.},
+  %``Evidence for oscillation of atmospheric neutrinos,''
+  Phys.\ Rev.\ Lett.\  {\bf 81} (1998) 1562
+  [hep-ex/9807003];
+  %%CITATION = HEP-EX 9807003;%%
+%
+%\bibitem{Ashie:2005ik}
+  Y.~Ashie {\it et al.},%  [Super-Kamiokande Collaboration],
+  %``A measurement of atmospheric neutrino oscillation parameters by
+  %Super-Kamiokande I,''
+  Phys.\ Rev.\ D {\bf 71}, 112005 (2005)
+  [hep-ex/0501064].
+  %%CITATION = HEP-EX 0501064;%%
+
+\bibitem{Araki:2004mb}
+  T.~Araki {\it et al.} [KamLAND Coll.],
+  %``Measurement of neutrino oscillation with KamLAND: Evidence of spectral
+  %distortion,''
+  Phys.\ Rev.\ Lett.\  {\bf 94}, 081801 (2005)
+  [hep-ex/0406035].
+  %%CITATION = HEP-EX 0406035;%%
+
+
+\bibitem{Aliu:2004sq}
+  E.~Aliu {\it et al.}  [K2K Coll.],
+  %``Evidence for muon neutrino oscillation in an accelerator-based
+  %experiment,''
+  Phys.\ Rev.\ Lett.\  {\bf 94}, 081802 (2005)
+  [hep-ex/0411038].
+  %%CITATION = HEP-EX 0411038;%%
+
+\bibitem{MINOS} 
+  T. Thomson [MINOS Coll.], 
+  Nucl.\ Phys.\ B (Proc. Suppl.) {\bf 143}, 249 (2005); 
+  P. Adamson \etal, NuMi-L-337.
+
+\bibitem{OPERA}
+  D. Autiero [OPERA Coll.], 
+  Nucl.\ Phys.\ B (Proc. Suppl.) {\bf 143}, 257 (2005);
+  M. Guler  \etal, \textit{Experiment proposal}, 
+  CERN/SPSC 2000-028 SPSC/P318 LNGS P25/2000.
+
+\bibitem{CNGS}
+  G. Acquistapace \etal, CERN-98-02.
+
+\bibitem{LSND}
+  A. Athanassopoulos \etal, Phys.\ Rev.\ Lett.\ {\bf 81}, 1774  (1998);
+  A. Aguilar \etal, Phys.\ Rev.\ D {\bf 64}, 112007 (2001).
+
+\bibitem{MINIBOONE}
+  I. Stancu \etal, FERMILAB-TM-2207.
+
+\bibitem{FOGLILISI05}
+  G.~L.~Fogli, E.~Lisi, A.~Marrone and A.~Palazzo,
+  %``Global analysis of three-flavor neutrino masses and mixings,''
+  hep-ph/0506083;
+
+\bibitem{Maltoni:2004ei}
+  M.~Maltoni, T.~Schwetz, M.~A.~Tortola and J.~W.~F.~Valle,
+  %``Status of global fits to neutrino oscillations,''
+  New J.\ Phys.\  {\bf 6}, 122 (2004)
+  [hep-ph/0405172];
+  %%CITATION = HEP-PH 0405172;%%
+%
+%\bibitem{Schwetz:2005jr}
+  T.~Schwetz,
+  %``Neutrino oscillations: Current status and prospects,''
+  Acta Phys.\ Polon.\ B {\bf 36}, 3203 (2005)
+  [hep-ph/0510331].
+  %%CITATION = HEP-PH 0510331;%%
+
+\bibitem{PMNS}
+  B.~Pontecorvo, Sov.\ Phys.--JETP {\bf 6}, 429 (1957) 
+  [Zh.\ Eksp.\ Teor.\ Fiz.\ \textbf{33}, 549 (1957)];
+  Z.~Maki, M.~Nakagawa and S.~Sakata, 
+  Prog.\ Theor.\ Phys.\ \textbf{28}, 870 (1962);
+  B.~Pontecorvo, Sov.\ Phys.--JETP \textbf{26}, 984 (1968) 
+  [Zh. Eksp. Teor. Fiz. \textbf{53}, 1717 (1967)];
+  V.~N.~Gribov and B.~Pontecorvo, 
+  Phys.\ Lett.\ B \textbf{28}, 493 (1969). 
+
+\bibitem{CHOOZ}
+  Chooz Collaboration,
+  M. Apollonio \etal, Phys.\ Lett.\ B {\bf 466}, 415 (1999);
+%\bibitem{Apollonio:2002gd}
+  M.~Apollonio {\it et al.},
+  %``Search for neutrino oscillations on a long base-line at the CHOOZ  nuclear
+  %power station,''
+  Eur.\ Phys.\ J.\ C {\bf 27}, 331 (2003)
+  [hep-ex/0301017].
+  %%CITATION = HEP-EX 0301017;%%
+
+\bibitem{Wpaper}
+  K.~Anderson \etal, White paper report on using nuclear 
+  reactors to search for a value of $\theta_{13}$, 
+  hep-ex/0402041;
+%
+  F.~Ardellier \etal, Letter of intent for Double-Chooz, 
+  hep-ex/0405032.
+
+\bibitem{T2K}
+  Y.~Itow {\it et al.},
+  The JHF-Kamioka neutrino project,
+  hep-ex/0106019;
+  %%CITATION = HEP-EX 0106019;%%
+%
+%\bibitem{Kobayashi:2005hu}
+  T.~Kobayashi,
+  %``Super beams,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 143} (2005) 303.
+  %%CITATION = NUPHZ,143,303;%%
+
+\bibitem{Ayres:2004js}
+  D.~S.~Ayres {\it et al.} [NOvA Coll.],
+  %``NOvA proposal to build a 30-kiloton off-axis detector to study neutrino
+  %oscillations in the Fermilab NuMI beamline,''
+  hep-ex/0503053.
+  %%CITATION = HEP-EX 0503053;%%
+
+\bibitem{Huber:2003pm}
+  P.~Huber, M.~Lindner, T.~Schwetz and W.~Winter,
+  %``Reactor neutrino experiments compared to superbeams,''
+  Nucl.\ Phys.\ B {\bf 665} (2003) 487
+  [hep-ph/0303232];
+  %%CITATION = HEP-PH 0303232;%%
+%
+%\bibitem{Huber:2004ug}
+  P.~Huber, M.~Lindner, M.~Rolinec, T.~Schwetz and W.~Winter,
+  %``Prospects of accelerator and reactor neutrino oscillation experiments  for
+  %the coming ten years,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 073014
+  [hep-ph/0403068].
+  %%CITATION = HEP-PH 0403068;%%
+
+\bibitem{Albrow:2005kw}
+  M.~G.~Albrow {\it et al.},
+  Physics at a Fermilab proton driver,
+  hep-ex/0509019.
+  %%CITATION = HEP-EX 0509019;%%
+
+\bibitem{SPL}
+%\bibitem{Autin:2000mn}
+  B.~Autin {\it et al.},
+  Conceptual design of the SPL, a high-power superconducting H- linac at
+  CERN, CERN-2000-012.
+
+\bibitem{BNLHS}
+%\bibitem{Diwan:2003bp}
+  M.~V.~Diwan {\it et al.},
+  %``Very long baseline neutrino oscillation experiments for precise
+  %measurements of mixing parameters and CP violating effects,''
+  Phys.\ Rev.\ D {\bf 68} (2003) 012002
+  [hep-ph/0303081].
+  %%CITATION = HEP-PH 0303081;%%
+
+\bibitem{zucchelli}
+%\bibitem{Zucchelli:2002sa}
+  P.~Zucchelli,
+  %``A novel concept for a anti-nu/e / nu/e neutrino factory: The Beta Beam,''
+  Phys.\ Lett.\ B {\bf 532} (2002) 166.
+  %%CITATION = PHLTA,B532,166;%%
+
+\bibitem{Albright:2004iw}
+  C.~Albright {\it et al.}  [Neutrino Factory/Muon Collider Coll.],
+  %``The neutrino factory and Beta Beam experiments and development,''
+  physics/0411123.
+  %%CITATION = PHYS-ICS 0411123;%%
+
+\bibitem{Blondel:2004ae}
+  A.~Blondel {\it et al.},
+  ECFA/CERN studies of a European neutrino factory complex,
+  CERN-2004-002
+
+\bibitem{Campagne:2004wt}
+  J.~E.~Campagne and A.~Cazes,
+  %``The theta(13) and delta(CP) sensitivities of the SPL-Frejus project
+  %revisited,''
+  Eur.\ Phys.\ J.\ C {\bf 45} (2006) 643
+  [hep-ex/0411062].
+  %%CITATION = HEP-EX 0411062;%%
+
+\bibitem{Mezzetto:2003ub}
+  M.~Mezzetto,
+  %``Physics reach of the beta beam,''
+  J.\ Phys.\ G {\bf 29} (2003) 1771
+  [hep-ex/0302007];
+  %%CITATION = HEP-EX 0302007;%%
+%
+  J.~Bouchez, M.~Lindroos, M.~Mezzetto,
+  %``Beta Beams: Present design and expected performances,''
+  AIP Conf.\ Proc.\  {\bf 721} (2004) 37
+  [hep-ex/0310059].
+  %%CITATION = HEP-EX 0310059;%%
+
+\bibitem{memphys}
+  A.~de Bellefon {\it et al.}, 
+  MEMPHYS: A large scale water \v{C}erenkov detector
+  at Fr\'ejus, Contribution to the CERN strategic committee,\\
+  \verb!http://apc-p7.org/APC_CS/Experiences/MEMPHYS/!
+
+\bibitem{UNO} 
+  C.~K.~Jung,
+  Feasibility of a next generation underground water Cherenkov detector:
+  UNO, hep-ex/0005046.
+  %%CITATION = HEP-EX 0005046;%%
+
+\bibitem{Nakamura:2003hk}
+  K.~Nakamura,
+  %``Hyper-Kamiokande: A next generation water Cherenkov detector,''
+  Int.\ J.\ Mod.\ Phys.\ A {\bf 18} (2003) 4053.
+  %%CITATION = IMPAE,A18,4053;%%
+
+\bibitem{Huber:2005ep}
+  P.~Huber, M.~Maltoni, T.~Schwetz,
+  %``Resolving parameter degeneracies in long-baseline experiments by
+  %atmospheric neutrino data,''
+  Phys.\ Rev.\ D {\bf 71} (2005) 053006
+  [hep-ph/0501037].
+  %%CITATION = HEP-PH 0501037;%%
+
+\bibitem{Globes}
+  P.~Huber, M.~Lindner and W.~Winter,
+  %``Simulation of long-baseline neutrino oscillation experiments with
+  %GLoBES,''
+  Comput.\ Phys.\ Commun.\  {\bf 167} (2005) 195
+  [hep-ph/0407333],
+  \verb!http://www.ph.tum.de/~globes!
+
+\bibitem{Huber:2002mx}
+  P.~Huber, M.~Lindner and W.~Winter,
+  %``Superbeams versus neutrino factories,''
+  Nucl.\ Phys.\ B {\bf 645} (2002) 3
+  [hep-ph/0204352].
+  %%CITATION = HEP-PH 0204352;%%
+
+\bibitem{Nuance}
+  NUANCE event generator (v3), 
+  \verb!http://nuint.ps.uci.edu/nuance/!,
+  D.~Casper,
+  %``The nuance neutrino physics simulation, and the future,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 112} (2002) 161
+  [hep-ph/0208030].
+
+\bibitem{ISSpage}
+  Webpage of the International Scoping Study physics working group:\\
+  \verb!http://www.hep.ph.ic.ac.uk/iss/wg1-phys-phen/index.html!
+
+\bibitem{MyNufact04}
+  M.~Mezzetto,
+  %``SPL and Beta Beams to the Frejus,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 149} (2005) 179.
+
+\bibitem{Donini:2004hu}
+  A.~Donini, E.~Fernandez-Martinez, P.~Migliozzi, S.~Rigolin and L.~Scotto Lavina,
+  %``Study of the eightfold degeneracy with a standard beta-beam and a
+  %super-beam facility,''
+  Nucl.\ Phys.\ B {\bf 710}, 402 (2005)
+  [hep-ph/0406132].
+  %%CITATION = HEP-PH 0406132;%%
+
+\bibitem{JJHigh2} 
+%\bibitem{Burguet-Castell:2005pa}
+  J.~Burguet-Castell, D.~Casper, E.~Couce, J.~J.~Gomez-Cadenas and P.~Hernandez,
+  %``Optimal beta-beam at the CERN-SPS,''
+  Nucl.\ Phys.\ B {\bf 725} (2005) 306
+  [hep-ph/0503021].
+  %%CITATION = HEP-PH 0503021;%%
+
+\bibitem{LindnerBB}
+%\bibitem{Huber:2005jk}
+  P.~Huber, M.~Lindner, M.~Rolinec and W.~Winter,
+  %``Physics and optimization of beta-beams: From low to very high gamma,''
+  hep-ph/0506237.
+  %%CITATION = HEP-PH 0506237;%%
+
+\bibitem{JJHigh1}
+ J.~Burguet-Castell, D.~Casper, J.~J.~Gomez-Cadenas, P.~Hernandez and F.~Sanchez,
+ Nucl.\ Phys.\ B {\bf 695} (2004) 217
+ [hep-ph/0312068].
+
+\bibitem{Terranova}
+  F.~Terranova, A.~Marotta, P.~Migliozzi and M.~Spinetti,
+  %``High energy beta beams without massive detectors,''
+  Eur.\ Phys.\ J.\ C {\bf 38}, 69 (2004)
+  [hep-ph/0405081].
+  %%CITATION = HEP-PH 0405081;%%
+
+\bibitem{BB-Reviews}
+  M.~Mezzetto, %``Beta Beams,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 143} (2005) 309
+  [hep-ex/0410083];
+%
+  C.~Volpe,
+  %``Topical review on 'beta-beams',''
+  hep-ph/0605033.
+
+\bibitem{Volpe}
+  C.~Volpe,
+  %``What about a Beta Beam facility for low energy neutrinos?,''
+  J.\ Phys.\ G {\bf 30} (2004) L1
+  [hep-ph/0303222].
+
+\bibitem{Lindroos}
+%\bibitem{Autin:2002ms}
+  B.~Autin {\it et al.},
+  %``The acceleration and storage of radioactive ions for a neutrino  factory,''
+  J.\ Phys.\ G {\bf 29}, 1785 (2003)
+  [physics/0306106];
+  %%CITATION = PHYS-ICS 0306106;%%
+% 
+  M.~Benedikt, S.~Hancock and M.~Lindroos,
+  % ``Baseline Design for a Beta-Beam Neutrino Factory'', 
+  Proceedings of EPAC, 2004,
+  \verb!http://accelconf.web.cern.ch/AccelConf/e04!;
+%
+  M.~Lindroos, EURISOL DS/TASK12/TN-05-02.
+
+\bibitem{Eurisol}
+  Eurisol Beta Beam webpage: \verb!http://beta-beam.web.cern.ch/beta-beam/!.
+
+\bibitem{Lindroos-Optimization}
+  M.~Benedikt, A.~Fabich, S.~Hancock and M.~Lindroos,
+  %``Optimization Of The Beta-Beam Baseline,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 155} (2006) 211.
+
+\bibitem{Neugen}
+  The NEUGEN neutrino event generator,
+  \verb!http://minos.phy.tufts.edu/gallag/neugen/!.
+
+\bibitem{MezzettoNuFact05}
+  M.~Mezzetto,
+  %``Physics potential of the gamma = 100,100 beta beam,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 155} (2006) 214
+  [hep-ex/0511005].
+
+\bibitem{FLUKA}
+A.~Fasso \etal, Proceedings of the MonteCarlo 2000 conference, 
+Lisbon, October 26 2000, 
+A.~Kling \etal\ (eds.), Springer-Verlag Berlin (2001), 159-164 and 955-960. 
+
+\bibitem{GEANT}
+Application Software group, Computing and Network Division \etal, 
+GEANT Description and Simulation Tool, CERN Geneva, Switzerland
+
+\bibitem{HARP-MINERVA}
+  C. Catanesi \etal\ [HARP Coll.], CERN-SPSC 2002/019;
+%
+%\bibitem{Drakoulakos:2004gn}
+  D.~Drakoulakos {\it et al.}  [Minerva Coll.],
+  %``Proposal to perform a high-statistics neutrino scattering experiment  using
+  %a fine-grained detector in the NuMI beam,''
+  hep-ex/0405002.
+  %%CITATION = HEP-EX 0405002;%%
+
+\bibitem{Mezzetto:2003mm}
+  M.~Mezzetto,
+  %``Physics potential of the SPL super beam,''
+  J.\ Phys.\ G {\bf 29}, 1781 (2003)
+  [hep-ex/0302005].
+  %%CITATION = HEP-EX 0302005;%%
+
+\bibitem{Burguet-Castell:2001ez}
+  J.~Burguet-Castell, M.~B.~Gavela, J.~J.~Gomez-Cadenas, P.~Hernandez and O.~Mena,
+  %``On the measurement of leptonic CP violation,''
+  Nucl.\ Phys.\ B {\bf 608} (2001) 301
+  [hep-ph/0103258].
+  %%CITATION = HEP-PH 0103258;%%
+
+\bibitem{Minakata:2001qm}
+  H.~Minakata and H.~Nunokawa,
+  %``Exploring neutrino mixing with low energy superbeams,''
+  JHEP {\bf 0110}, 001 (2001)
+  [hep-ph/0108085].
+  %%CITATION = HEP-PH 0108085;%%
+
+\bibitem{Fogli:1996pv}
+  G.~L.~Fogli and E.~Lisi,
+  %``Tests of three-flavor mixing in long-baseline neutrino oscillation
+  %experiments,''
+  Phys.\ Rev.\ D {\bf 54}, 3667 (1996)
+  [hep-ph/9604415].
+  %%CITATION = HEP-PH 9604415;%%
+
+\bibitem{Barger:2001yr}
+  V.~Barger, D.~Marfatia and K.~Whisnant,
+  %``Breaking eight-fold degeneracies in neutrino CP violation, mixing, and
+  %mass hierarchy,''
+  Phys.\ Rev.\ D {\bf 65}, 073023 (2002)
+  [hep-ph/0112119].
+  %%CITATION = HEP-PH 0112119;%%
+
+\bibitem{Yasuda:2004gu}
+  O.~Yasuda,
+  %``New plots and parameter degeneracies in neutrino oscillations,''
+  New J.\ Phys.\  {\bf 6}, 83 (2004)
+  [hep-ph/0405005].
+  %%CITATION = HEP-PH 0405005;%%
+
+\bibitem{Ishitsuka:2005qi}
+  M.~Ishitsuka, T.~Kajita, H.~Minakata and H.~Nunokawa,
+  %``Resolving neutrino mass hierarchy and CP degeneracy by two identical
+  %detectors with different baselines,''
+  Phys.\ Rev.\ D {\bf 72} (2005) 033003
+  [hep-ph/0504026].
+  %%CITATION = HEP-PH 0504026;%%
+
+\bibitem{Antusch:2004yx}
+  S.~Antusch, P.~Huber, J.~Kersten, T.~Schwetz and W.~Winter,
+  %``Is there maximal mixing in the lepton sector?,''
+  Phys.\ Rev.\ D {\bf 70}, 097302 (2004)
+  [hep-ph/0404268].
+  %%CITATION = HEP-PH 0404268;%%
+
+\bibitem{Minakata:2004pg}
+  H.~Minakata, M.~Sonoyama and H.~Sugiyama,
+  %``Determination of theta(23) in long-baseline neutrino oscillation
+  %experiments with three-flavor mixing effects,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 113012
+  [hep-ph/0406073].
+  %%CITATION = HEP-PH 0406073;%%
+
+\bibitem{Donini:2005db}
+  A.~Donini, E.~Fernandez-Martinez, D.~Meloni and S.~Rigolin,
+  %``nu/mu disappearance at the SPL, T2K-I, NOnuA and the neutrino factory,''
+  hep-ph/0512038.
+  %%CITATION = HEP-PH 0512038;%%
+
+\bibitem{Peres:2003wd}
+  O.L.G.~Peres, A.Y.~Smirnov,
+  %``Atmospheric neutrinos: LMA oscillations, U(e3) induced interference and
+  %CP-violation,''
+  Nucl.\ Phys.\ B {\bf 680} (2004) 479
+  [hep-ph/0309312].
+  %%CITATION = HEP-PH 0309312;%%
+
+\bibitem{Gonzalez-Garcia:2004cu}
+  M.C.~Gonzalez-Garcia, M.~Maltoni, A.Y. Smirnov,
+  %``Measuring the deviation of the 2-3 lepton mixing from maximal with
+  %atmospheric neutrinos,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 093005
+  [hep-ph/0408170].
+  %%CITATION = HEP-PH 0408170;%%
+
+\bibitem{Petcov:1998su}
+  S.~T.~Petcov,
+  %``Diffractive-like (or parametric-resonance-like?) enhancement of the  earth
+  %(day-night) effect for solar neutrinos crossing the earth core,''
+  Phys.\ Lett.\ B {\bf 434} (1998) 321
+  [hep-ph/9805262];
+  %%CITATION = HEP-PH 9805262;%%
+%
+%\bibitem{Chizhov:1998ug}
+  M.~Chizhov, M.~Maris and S.~T.~Petcov,
+  %``On the oscillation length resonance in the transitions of solar and
+  %atmospheric neutrinos crossing the earth core,''
+  hep-ph/9810501;
+  %%CITATION = HEP-PH 9810501;%%
+%
+%\bibitem{Chizhov:1999az}
+  M.~V.~Chizhov and S.~T.~Petcov,
+  %``New conditions for a total neutrino conversion in a medium,''
+  Phys.\ Rev.\ Lett.\  {\bf 83} (1999) 1096
+  [hep-ph/9903399].
+  %%CITATION = HEP-PH 9903399;%%
+
+\bibitem{Akhmedov:1998ui}
+  E.~K.~Akhmedov,
+  %``Parametric resonance of neutrino oscillations and passage of solar and
+  %atmospheric neutrinos through the earth,''
+  Nucl.\ Phys.\ B {\bf 538}, 25 (1999)
+  [hep-ph/9805272];
+  %%CITATION = HEP-PH 9805272;%%
+%
+%\bibitem{Akhmedov:1998xq}
+  E.~K.~Akhmedov, A.~Dighe, P.~Lipari and A.~Y.~Smirnov,
+  %``Atmospheric neutrinos at Super-Kamiokande and parametric resonance in
+  %neutrino oscillations,''
+  Nucl.\ Phys.\ B {\bf 542}, 3 (1999)
+  [hep-ph/9808270].
+  %%CITATION = HEP-PH 9808270;%%
+
+\bibitem{Bernabeu:2003yp}
+  J.~Bernabeu, S.~Palomares-Ruiz and S.~T.~Petcov,
+  %``Atmospheric neutrino oscillations, theta(13) and neutrino mass
+  %hierarchy,''
+  Nucl.\ Phys.\ B {\bf 669}, 255 (2003)
+  [hep-ph/0305152].
+  %%CITATION = HEP-PH 0305152;%%
+
+\bibitem{Kim:1998bv}
+  C.~W.~Kim and U.~W.~Lee,
+  %``Comment on the possible electron-neutrino excess in the  Super-Kamiokande
+  %atmospheric neutrino experiment,''
+  Phys.\ Lett.\ B {\bf 444}, 204 (1998)
+  [hep-ph/9809491].
+  %%CITATION = HEP-PH 9809491;%%
+
+\bibitem{Kajita}
+  T.~Kajita, Talk at NNN05, 7--9 April 2005, Aussois, Savoie, France,\\
+  \verb!http://nnn05.in2p3.fr/!
+
+\bibitem{Gonzalez-Garcia:2004wg}
+  M.~C.~Gonzalez-Garcia and M.~Maltoni,
+  %``Atmospheric neutrino oscillations and new physics,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 033010
+  [hep-ph/0404085].
+  %%CITATION = HEP-PH 0404085;%%
+
+\bibitem{Petcov:2005rv}
+  S.~T.~Petcov and T.~Schwetz,
+  %``Determining the neutrino mass hierarchy with atmospheric neutrinos,''
+  Nucl.\ Phys.\ B {\bf 740}, 1 (2006)
+  [hep-ph/0511277].
+  %%CITATION = HEP-PH 0511277;%%
+
+\bibitem{MenaRequejo:2005hn}
+  O.~Mena-Requejo, S.~Palomares-Ruiz and S.~Pascoli,
+  %``Super-NOvA: A long-baseline neutrino experiment with two off-axis
+  %detectors,''
+  Phys.\ Rev.\ D {\bf 72} (2005) 053002
+  [hep-ph/0504015];
+  %%CITATION = HEP-PH 0504015;%%
+%
+%\bibitem{Mena:2005ri}
+  %O.~Mena, S.~Palomares-Ruiz and S.~Pascoli,
+  %``Determining the neutrino mass hierarchy and CP violation in NOnuA with a
+  %second off-axis detector,''
+  hep-ph/0510182.
+  %%CITATION = HEP-PH 0510182;%%
+
+\bibitem{Hagiwara:2005pe}
+  K.~Hagiwara, N.~Okamura and K.~Senda,
+  %``Solving the neutrino parameter degeneracy by measuring the T2K off-axis
+  %beam in Korea,''
+  hep-ph/0504061.
+  %%CITATION = HEP-PH 0504061;%%
+
+\bibitem{Kachelriess:2004vs}
+  M.~Kachelriess and R.~Tomas,
+  %``Identifying the neutrino mass hierarchy with supernova neutrinos,''
+  hep-ph/0412100.
+  %%CITATION = HEP-PH 0412100;%%
+
+\end{thebibliography}
+\end{document}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
Index: /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/c2m.tar/CERN-MEMPHYS.tex
===================================================================
--- /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/c2m.tar/CERN-MEMPHYS.tex	(revision 385)
+++ /Backup NB/Talks/MEMPHYSetal/CERN-Frejus/c2m.tar/CERN-MEMPHYS.tex	(revision 385)
@@ -0,0 +1,2571 @@
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\NeedsTeXFormat{LaTeX2e}
+\documentclass[12pt,a4paper]{article}
+
+%-- used packages ------------------------------------------------------
+
+\usepackage{cite}
+\usepackage{graphicx}
+\usepackage{epsfig}
+\usepackage{amssymb}
+\usepackage{amsmath}
+\usepackage{latexsym}
+
+
+%-- page parameters -------------------------------------------------
+
+\jot = 1.5ex
+\parskip 5pt plus 1pt
+%\parindent 0pt
+\evensidemargin -0.1in   \oddsidemargin  -0.1in
+\textwidth  6.5in       \textheight 9.4in
+\topmargin -.8cm        \headsep    1.0cm
+
+%-- command (re)definitions -----------------------------------------
+
+\newcommand{\capdef}{}
+%\newcommand{\mycaption}[2][\capdef]{\renewcommand{\capdef}{#2}%
+%       \caption[#1]{{\itshape #2}}}
+\newcommand{\mycaption}[2][\capdef]{\renewcommand{\capdef}{#2}%
+       \caption[#1]{{\footnotesize #2}}}
+\makeatletter
+\renewcommand{\fnum@table}{\textbf{\tablename~\thetable}}
+\renewcommand{\fnum@figure}{\textbf{\figurename~\thefigure}}
+\makeatother
+\def\ltap{\ \raisebox{-.4ex}{\rlap{$\sim$}} \raisebox{.4ex}{$<$}\ }
+\def\gtap{\ \raisebox{-.4ex}{\rlap{$\sim$}} \raisebox{.4ex}{$>$}\ }
+
+\newcounter{myenumi}
+\newcommand{\myitem}{\refstepcounter{myenumi}\item}
+\renewcommand{\themyenumi}{\roman{myenumi}}
+\newenvironment{mylist}{%
+        \setcounter{myenumi}{0}
+        \begin{list}{\textit{\themyenumi)}}{%
+        \setlength{\topsep}{0.2\baselineskip}%
+        \setlength{\partopsep}{-\topsep}%
+        \setlength{\itemsep}{\topsep}%
+        \setlength{\parsep}{0\baselineskip}%
+        \setlength{\leftmargin}{0em}%
+        \setlength{\listparindent}{\parindent}%
+        \setlength{\itemindent}{2.5em}%
+        \setlength{\labelwidth}{1.5em}%
+        \setlength{\labelsep}{0.75em}}}%
+{\end{list}}
+
+\newlength{\myem}
+\settowidth{\myem}{m}
+\newcommand{\sep}[1]{#1}
+\newcounter{mysubequation}[equation]
+\renewcommand{\themysubequation}{\alph{mysubequation}}
+\newcommand{\mytag}{\stepcounter{mysubequation}%
+\tag{\theequation\protect\sep{\themysubequation}}}
+\newcommand{\globallabel}[1]{\refstepcounter{equation}\label{#1}}
+
+\makeatletter
+\renewcommand{\section}{\@startsection{section}{1}{0em}{-\baselineskip}%
+{\baselineskip}{\normalfont\large\bfseries}}
+\renewcommand{\subsection}%
+{\@startsection{subsection}{2}{0em}{-0.7\baselineskip}%
+{0.7\baselineskip}{\normalfont\bfseries}}
+\makeatother
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%
+% definitions
+%%%%%%%%%%%%%%%%%%%%%%%%
+\newcommand{\centre}[2]{\multispan{#1}{\hfill #2\hfill}}
+\newcommand{\etal}{\textit{et al.}}
+\newcommand{\stheta}{\ensuremath{\sin^22\theta_{13}}}
+\newcommand{\BB}{$\beta$B}
+\newcommand{\sigdm}{\ensuremath{{\rm sign}(\Delta m^2_{31})}}
+\newcommand{\delCP}{\ensuremath{\delta_{\rm CP}}}
+\newcommand{\thetatt}{\ensuremath{\theta_{23}}}
+
+\def\nubar{$\overline{\nu}\ $}
+\def\nue{\ensuremath{\nu_{e}}}
+\def\nubare{\ensuremath{\overline{\nu}_{e}}}
+\def\nubarecc{$\overline{\nu}_{e}^{CC}\ $}
+\def\numu{\ensuremath{\nu_{\mu}\ }}
+\def\nubarmu{\ensuremath{\overline{\nu}_{\mu}}}
+\def\nubarmucc{$\overline{\nu}_{\mu}^{CC}\ $}
+\def\nutau{\ensuremath{\nu_{\tau}\ }}
+\def\nubartau{\ensuremath{\overline{\nu}_{\tau}}}
+\newcommand{\nuenumu}{\ensuremath{\nue \rightarrow \numu\,}}
+\newcommand{\numunutau}{\ensuremath{\numu \rightarrow \nutau\,}}
+\newcommand{\nuenutau}{\ensuremath{\nue \rightarrow \nutau}}
+\newcommand{\nubarenubarmu}{\ensuremath{\overline{\nu}_e \rightarrow \overline{\nu}_\mu\,}}
+\newcommand{\nubarmunubare}{\ensuremath{\overline{\nu}_\mu \rightarrow \overline{\nu}_e\,}}
+\newcommand{\dmot}{\ensuremath{\Delta m^2_{12}\,}}
+
+\newcommand{\He}{\ensuremath{^6{\mathrm{He}}}}
+\newcommand{\Ne}{\ensuremath{^{18}{\mathrm{Ne}}}}
+\def\Li{^6{\mathrm{Li}}}
+\def\anue{\overline{{\mathrm\nu}}_{\mathrm e}}
+\def\anumu{\overline{{\mathrm\nu}}_{\mathrm \mu}}
+\newcommand{\thetaot}{\ensuremath{\theta_{13}}\,}
+\newcommand{\numunue}{\ensuremath{\nu_\mu \rightarrow \nu_e}}
+\newcommand{\nueovernumu}{\ensuremath{\nue/\numu}}
+
+\newcommand{\Efin}{E^\text{fin}}
+\newcommand{\Emin}{E_\text{min}}
+
+
+\begin{document}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+%%%%                     Title-page                              %%%%
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+%\begin{titlepage}
+
+% the footnote symbols are only redefined for the title page !
+\renewcommand{\thefootnote}{\alph{footnote}}
+
+\begin{flushright}
+LAL-06-35\\
+IC/2006/011\\
+SISSA 16/2006/EP\\
+\end{flushright}
+
+\vspace*{0.5cm}
+
+\renewcommand{\thefootnote}{\fnsymbol{footnote}}
+\setcounter{footnote}{-1}
+
+{\begin{center} 
+{\Large\textbf{
+Physics potential of the CERN--MEMPHYS\\[2mm] 
+neutrino oscillation project}
+}
+\end{center}}
+
+\vspace*{0.5cm}
+
+\begin{center} {\bf
+J.-E.\ Campagne$^a$, 
+M.\ Maltoni$^b$,
+M.\ Mezzetto$^c$, and 
+T.\ Schwetz$^d$}
+\end{center}
+
+{\it
+\begin{center}
+  $^a$Laboratoire de l'Acc\'el\'erateur Lin\'eaire,
+  Universit\'e Paris-Sud, IN2P3/CNRS\\
+  B.P.\ 34, 91898 Orsay Cedex, France\\[2mm]
+%  
+  $^b$International Centre for Theoretical Physics, 
+  Strada Costiera 11, I-31014 Trieste, Italy\\ 
+  {\rm and}\\
+  Departamento de F\'isica Te\'orica \& Instituto de F\'isica Te\'orica,
+  Facultad de Ciencias C-XI,\\ 
+  Universidad Aut\'onoma de Madrid, Cantoblanco, E-28049 Madrid, Spain\\[2mm]
+%  
+  $^c$Istituto Nazionale Fisica Nucleare, Sezione di Padova,
+  Via Marzolo 8, 35100 Padova, Italy\\[2mm]
+%
+  $^d$Scuola Internazionale Superiore di Studi Avanzati, 
+  Via Beirut 2--4, 34014 Trieste, Italy\\ 
+  {\rm and}\\
+  CERN, Physics Department, Theory Division, CH-1211 Geneva 23, Switzerland
+\end{center}}
+
+\vspace*{0.5cm}
+
+
+\begin{abstract}
+We consider the physics potential of CERN based neutrino oscillation
+experiments consisting of a Beta Beam (\BB) and a Super Beam (SPL)
+sending neutrinos to MEMPHYS, a 440~kt water \v{C}erenkov detector at
+Fr\'ejus, at a distance of 130~km from CERN. The $\theta_{13}$
+discovery reach and the sensitivity to CP violation are investigated,
+including a detailed discussion of parameter degeneracies and
+systematical errors. For SPL sensitivities similar to the ones of the
+phase~II of the T2K experiment (T2HK) are obtained, whereas the \BB\
+may reach significantly better sensitivities, depending on the
+achieved number of total ion decays.  The results for the
+CERN--MEMPHYS experiments are less affected by systematical
+uncertainties than T2HK.
+%
+We point out that by a combination of data from \BB\ and SPL a
+measurement with antineutrinos is not necessary and hence the same
+physics results can be obtained within about half of the measurement time
+compared to one single experiment.
+%
+Furthermore, it is shown how including data from atmospheric neutrinos in
+the MEMPHYS detector allows to resolve parameter degeneracies and, in
+particular, provides sensitivity to the neutrino mass hierarchy and
+the octant of $\theta_{23}$.
+%\pacs{14.60.Pq, 14.60.Lm}
+\end{abstract}
+
+\renewcommand{\thefootnote}{\arabic{footnote}}
+\setcounter{footnote}{0}
+
+\newpage
+%\tableofcontents
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Introduction}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+In recent years strong evidence for neutrino oscillations has been
+obtained in solar~\cite{solar},
+atmospheric~\cite{Fukuda:1998mi,Ashie:2005ik},
+reactor~\cite{Araki:2004mb}, and accelerator~\cite{Aliu:2004sq}
+neutrino experiments. The very near future of long-baseline (LBL)
+neutrino experiments is devoted to the study of the oscillation
+mechanism in the range of $\Delta m^2_{31} \approx 2.4\times10^{-3} \:
+\mathrm{eV}^2$ indicated by atmospheric neutrinos using conventional
+$\nu_\mu$ beams.  Similar as in the K2K experiment in
+Japan~\cite{Aliu:2004sq}, the presently running MINOS experiment in
+the USA~\cite{MINOS} uses a low energy beam to measure $\Delta
+m^2_{31}$ by observing the $\nu_\mu\rightarrow\nu_\mu$ disappearance
+probability, while the OPERA~\cite{OPERA} experiment will be able to
+detect $\nu_\tau$ appearance within the high energy CERN--Gran Sasso
+beam~\cite{CNGS}.
+%
+If we do not consider the LSND anomaly~\cite{LSND} that will be
+further studied soon by the MiniBooNE experiment~\cite{MINIBOONE}, all
+data can be accommodated within the three flavor scenario (see
+Refs.~\cite{FOGLILISI05,Maltoni:2004ei} for recent global analyses),
+and neutrino oscillations are described by two neutrino mass-squared
+differences ($\Delta m^2_{21}$ and $\Delta m^2_{31}$) and the $3\times
+3$ unitary Pontecorvo-Maki-Nakagawa-Sakata (PMNS) lepton mixing
+matrix~\cite{PMNS} with three angles
+($\theta_{12}$,$\theta_{13}$,$\theta_{23}$) and one Dirac CP phase
+$\delCP$.
+
+Future tasks of neutrino physics are an improved sensitivity to the
+last unknown mixing angle, $\theta_{13}$, to explore the CP violation
+mechanism in the leptonic sector, and to determine the sign of $\Delta
+m^2_{31}$ which describes the type of the neutrino mass hierarchy
+(normal, $\Delta m^2_{31} > 0$ or inverted, $\Delta m^2_{31} < 0$).
+%
+The present upper bound on $\theta_{13}$ is dominated by the
+constraint from the Chooz reactor experiment~\cite{CHOOZ}. A global
+analysis of all data yields $\sin^22\theta_{13}<0.082$ at
+90\%~CL~\cite{Maltoni:2004ei}. A main purpose of upcoming reactor and
+accelerator experiments is to improve this bound or to reveal a finite
+value of $\theta_{13}$. In reactor experiments, one uses $\bar{\nu}_e$
+in disappearance mode and the sensitivity is increased with respect to
+present experiments by the use of a near detector close to the
+reactor~\cite{Wpaper}. In accelerator experiments, the first
+generation of so-called Super Beams with sub-mega watt proton drivers
+such as T2K (phase-I)~\cite{T2K} and NO$\nu$A~\cite{Ayres:2004js}, the
+appearance channel $\nu_\mu\to\nu_e$ is explored. This next generation
+of reactor and Super Beam experiments will reach sensitivities of the
+order of $\sin^22\theta_{13} \lesssim 0.01$ ($90\%$~CL) within a time
+scale of several years~\cite{Huber:2003pm}.
+%
+Beyond this medium term program, there are several projects on how to
+enter the high precision age in neutrino oscillations and to attack
+the ultimate goals like the discovery of leptonic CP violation or the
+determination of the neutrino mass hierarchy. In accelerator
+experiments, one can extend the Super Beam concept by moving to
+multi-mega watt proton drivers~\cite{T2K,Albrow:2005kw,SPL,BNLHS} or
+apply novel technologies, such as neutrino beams from decaying ions
+(so-called Beta Beams)~\cite{zucchelli,Albright:2004iw} or from
+decaying muons (so-called Neutrino
+Factories)~\cite{Albright:2004iw,Blondel:2004ae}.
+
+In this work we focus on possible future neutrino oscillation
+facilities hosted at CERN, namely a multi-mega watt Super Beam
+experiment based on a Super Proton Linac (SPL)~\cite{Campagne:2004wt}
+and a $\gamma = 100$ Beta Beam
+(\BB)~\cite{Mezzetto:2003ub}. These experiments will search for
+$\stackrel{\scriptscriptstyle (-)}{\nu}_\mu \to
+\stackrel{\scriptscriptstyle(-)}{\nu}_e$ and
+$\stackrel{\scriptscriptstyle (-)}{\nu}_e \to
+\stackrel{\scriptscriptstyle(-)}{\nu}_\mu$ appearance, respectively,
+by sending the neutrinos to a mega ton scale water \v{C}erenkov
+detector (MEMPHYS)~\cite{memphys}, located at a distance of 130~km from
+CERN under the Fr\'ejus mountain. Similar detectors are under
+consideration also in the US (UNO~\cite{UNO}) and in Japan
+(Hyper-K~\cite{T2K,Nakamura:2003hk}).
+%
+We perform a detailed analysis of the SPL and \BB\ physics
+potential, discussing the discovery reach for $\theta_{13}$ and
+leptonic CP violation. In addition we consider the possibility to
+resolve parameter degeneracies in the LBL data by using the
+atmospheric neutrinos available in the mega ton
+detector~\cite{Huber:2005ep}. This leads to a sensitivity to the
+neutrino mass hierarchy of the CERN--MEMPHYS experiments, despite the
+rather short baseline.
+%
+The physics performances of \BB\ and SPL are compared to the ones
+obtainable at the second phase of the T2K experiment in Japan, which
+is based on an upgraded version of the original T2K beam and the
+Hyper-K detector (T2HK)~\cite{T2K}.
+
+The outline of the paper is as follows.  In Sec.~\ref{sec:analysis} we
+summarize the main characteristics of the \BB, SPL, and T2HK
+experiments and give general details of the physics analysis methods,
+whereas in Sec.~\ref{sec:experiments} we describe in some detail the
+MEMPHYS detector, the \BB, the SPL Super Beam, and our atmospheric
+neutrino analysis. In Sec.~\ref{sec:degeneracies} we review the
+problem of parameter degeneracies and discuss its implications for the
+experiments under consideration. In Sec.~\ref{sec:sensitivities} we
+present the sensitivities to the ``atmospheric parameters''
+$\theta_{23}$ and $\Delta m^2_{31}$, the $\theta_{13}$ discovery
+potential, and the sensitivity to CP violation. We also investigate in
+some detail the impact of systematical errors. In
+Sec.~\ref{sec:synergies} we discuss synergies which are offered by the
+CERN--MEMPHYS facilities.  We point out advantages of the case when
+\BB\ and SPL are available simultaneously, and we consider the use of
+atmospheric neutrino data in MEMPHYS in combination with the LBL
+experiments. Our results are summarized in Sec.~\ref{sec:conclusions}.
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Experiments overview and analysis methods}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:analysis}
+
+In this section we give the most important experimental parameters
+which we adopt for the simulation of the CERN--MEMPHYS experiments
+\BB\ and SPL, as well as for the T2HK experiment in Japan. These
+parameters are summarized in Tab.~\ref{tab:setups}. For all
+experiments the detector mass is 440~kt, and the running time is 10
+years, with a division in neutrino and antineutrino running time in
+such a way that roughly an equal number of events is obtained. We
+always use the total available information from appearance as well as
+disappearance channels including the energy spectrum. For all three
+experiments we adopt rather optimistic values for the systematical
+uncertainties of 2\% as default values, but we also consider the case
+when systematics are increased to 5\%. These errors are uncorrelated
+between the various signal channels (neutrinos and antineutrinos), and
+between signals and backgrounds.
+
+\begin{table}
+  \centering
+  \begin{tabular}{lcc@{\qquad\qquad}c}
+  \hline\noalign{\smallskip}
+       & \BB & SPL & T2HK \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  Detector mass & 440~kt & 440~kt & 440~kt\\
+  Baseline      & 130 km & 130 km & 295 km \\
+  Running time ($\nu + \bar\nu$) 
+                & 5 + 5 yr & 2 + 8 yr & 2 + 8 yr \\
+  Beam intensity  & $5.8\,(2.2) \cdot 10^{18}$ He (Ne) dcys/yr & 4 MW & 4 MW\\
+  Systematics on signal  & 2\% & 2\% & 2\%\\
+  Systematics on backgr. & 2\% & 2\% & 2\%\\
+  \noalign{\smallskip}\hline
+  \end{tabular}
+  \mycaption{Summary of default parameters used for the simulation of the
+  \BB, SPL, and T2HK experiments.\label{tab:setups}}
+\end{table}
+
+A more detailed description of the CERN--MEMPHYS experiments is given
+in Sec.~\ref{sec:experiments}. For the T2HK simulation we use the
+setup provided by GLoBES~\cite{Globes} based on
+Ref.~\cite{Huber:2002mx}, which follows closely the LOI~\cite{T2K}. In
+order to allow a fair comparison we introduce the following changes
+with respect to the configuration used in Ref.~\cite{Huber:2002mx}:
+The fiducial mass is set to 440~kt, the systematical errors on the
+background and on the $\nu_e$ and $\bar\nu_e$ appearance signals is
+set to 2\%, and we use a total running time of 10 years, divided into
+2 years of data taking with neutrinos and 8 years with
+antineutrinos. We include an additional background from the
+$\bar\nu_\mu \to \bar\nu_e$ ($\nu_\mu \to \nu_e$) channel in the
+neutrino (antineutrino) mode. Furthermore, we use
+the same CC detection cross section as for the \BB/SPL
+analysis~\cite{Nuance}. For more details see
+Refs.~\cite{T2K,Huber:2002mx}.
+
+Recently the idea was put forward to observe the T2K beam with a
+second detector placed in
+Korea~\cite{Ishitsuka:2005qi,Kajita:2006bt,Hagiwara:2005pe}.  In the
+so-called T2KK setup the Hyper-Kamiokande detector is split into two
+detectors of 270~kt each, one of them is located in Korea at a
+distance of about 1050~km from the source, and the other is placed at
+Kamioka at a distance of 295~km. Here we will confine ourselves to the
+standard T2HK setup, since the purpose of our work is not a T2HK
+optimization study investigating various configurations for that
+experiment. In contrast, here T2HK mainly serves as a point of
+reference to which we compare the CERN--MEMPHYS experiments. For this
+aim we prefer to stick to the ``minimal'' one-detector configuration
+at a relatively short baseline, since two-detector setups with very
+long baselines clearly represent a different class of experiments
+whose consideration goes beyond the scope of the present
+work. Nevertheless we will comment briefly also on T2KK performances
+obtained in Refs.~\cite{Ishitsuka:2005qi,Kajita:2006bt}.
+
+
+\begin{table}
+  \centering
+  \begin{tabular}{lcccccc}
+  \hline\noalign{\smallskip}
+       & \centre{2}{\BB} & \centre{2}{SPL} & \centre{2}{T2HK} \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  & $\delCP=0$ & $\delCP=\pi/2$ & $\delCP=0$ & $\delCP=\pi/2$ & $\delCP=0$ & $\delCP=\pi/2$\\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+%
+  appearance $\nu$ & & & & & & \\
+  background       & \centre{2}{143} &\centre{2}{622} &\centre{2}{898}\\
+  $\stheta=0$      & \centre{2}{28}  &\centre{2}{51}  &\centre{2}{83}  \\
+  $\stheta=10^{-3}$&    76  &   88   &   105  &   14  &   178 &    17  \\ 
+  $\stheta=10^{-2}$&   326  &  365   &   423  &  137  &   746 &   238  \\
+%  
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+%
+  appearance $\bar\nu$ & & & & & & \\
+  background       & \centre{2}{157} &\centre{2}{640} &\centre{2}{1510}\\
+  $\stheta=0$      & \centre{2}{31}  &\centre{2}{57}  &\centre{2}{93}  \\
+  $\stheta=10^{-3}$&    83  &   12   &   102  &  146  &   192 &   269  \\ 
+  $\stheta=10^{-2}$&   351  &  126   &   376  &  516  &   762 &  1007  \\
+%  
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+%
+  disapp. $\nu$ &\centre{2}{100315}&\centre{2}{21653}&\centre{2}{24949}\\
+  background    & \centre{2}{6}   &\centre{2}{1}    &\centre{2}{444}\\
+  disapp. $\bar\nu$&\centre{2}{84125}&\centre{2}{18321}&\centre{2}{34650}\\
+  background       &\centre{2}{5}    &\centre{2}{1}    &\centre{2}{725}\\
+  \noalign{\smallskip}\hline
+%  
+  \end{tabular}
+  \mycaption{Number of events for appearance and disappearance signals
+  and backgrounds for the \BB, SPL, and T2HK experiments as
+  defined in Tab.~\ref{tab:setups}. For the appearance signals the
+  event numbers are given for several values of $\stheta$ and $\delCP
+  = 0$ and $\pi/2$. The background as well as the disappearance event
+  numbers correspond to $\theta_{13}=0$. For the other oscillation
+  parameters the values of Eq.~(\ref{eq:default-params}) are
+  used.\label{tab:events}}
+\end{table}
+
+In Tab.~\ref{tab:events} we give the number of signal and background
+events for the experiment setups as defined in Tab.~\ref{tab:setups}.
+For the appearance channels ($\stackrel{\scriptscriptstyle (-)}{\nu}_e
+\to \stackrel{\scriptscriptstyle(-)}{\nu}_\mu$ for the \BB\ and
+$\stackrel{\scriptscriptstyle (-)}{\nu}_\mu \to
+\stackrel{\scriptscriptstyle(-)}{\nu}_e$ for SPL and T2HK) we give the
+signal events for various values of $\theta_{13}$ and $\delCP$. The
+``signal'' events for $\theta_{13} = 0$ are appearance events induced by
+the oscillations with $\Delta m^2_{21}$. The value $\stheta = 10^{-3}$
+corresponds roughly to the sensitivity limit for the considered
+experiments, whereas $\stheta = 10^{-2}$ gives a good sensitivity
+to CP violation. This can be appreciated by comparing the values of
+$\nu$ and $\bar\nu$ appearance events for $\delCP = 0$ and $\pi/2$. In
+the table the background to the appearance signal is given for
+$\theta_{13} = 0$. Note that in general the number of background
+events depends also on the oscillation parameters, since also the
+background neutrinos in the beam oscillate. This effect is
+consistently taken into account in the analysis, however, for the
+parameter values in the table the change in the background events due
+to oscillations is only of the order of a few events.
+
+The physics analysis is performed with the GLoBES open source
+software~\cite{Globes}, which provides a convenient tool to simulate
+long-baseline experiments and compare different facilities in a
+unified framework. The experiment definition (AEDL) files for the \BB\
+and SPL simulation with GLoBES are available at Ref.~\cite{Globes}.
+In the analysis parameter degeneracies and correlations are fully
+taken into account and in general all oscillation parameters are
+varied in the fit.
+%
+To simulate the ``data'' we adopt the following
+set of ``true values'' for the oscillation parameters:
+%
+\begin{equation}\label{eq:default-params}
+\begin{array}{l@{\qquad}l}
+  \Delta m^2_{31} = +2.4 \times 10^{-3}~\mathrm{eV}^2\,, & 
+  \sin^2\theta_{23} = 0.5\,,\\ 
+  \Delta m^2_{21} = 7.9 \times 10^{-5}~\mathrm{eV}^2 \,,&
+  \sin^2\theta_{12} = 0.3 \,,
+\end{array}
+\end{equation} 
+%
+and we include a prior knowledge of these values with an accuracy of
+10\% for $\theta_{12}$, $\theta_{23}$, $\Delta m^2_{31}$, and 4\% for
+$\Delta m^2_{21}$ at 1$\sigma$. These values and accuracies are
+motivated by recent global fits to neutrino oscillation
+data~\cite{FOGLILISI05,Maltoni:2004ei}, and they are always used
+except where explicitly stated otherwise.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{The CERN--MEMPHYS experiments}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:experiments}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The MEMPHYS detector}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+MEMPHYS (MEgaton Mass PHYSics)~\cite{memphys} is a mega ton class
+water \v{C}erenkov detector in the straight extrapolation of
+Super-Kamiokande, located at Fr\'ejus, at a distance of 130~km from
+CERN. It is an alternative design of the UNO~\cite{UNO} and
+Hyper-Kamiokande~\cite{Nakamura:2003hk} detectors and shares the same
+physics case, both from the non-accelerator domain (nucleon decay,
+super nova neutrino detection, solar neutrinos, atmospheric neutrinos)
+and from the accelerator domain which is the subject of this paper. A
+recent civil engineering pre-study to envisage the possibly of large
+cavity excavation located under the Fr\'ejus mountain (4800~m.e.w.)
+near the present Modane underground laboratory has been undertaken.
+The main result of this pre-study is that MEMPHYS may be built with
+present techniques as a modular detector consisting of several shafts,
+each with 65~m in diameter, 65~m in height for the total water
+containment. A schematic view of the layout is shown in
+Fig.~\ref{fig:MEMPHYS}. For the present study we have chosen a
+fiducial mass of 440~kt which means 3 shafts and an inner detector of
+57~m in diameter and 57~m in height.  Each inner detector may be
+equipped with photo detectors (81000 per shaft) with a 30\%
+geometrical coverage and the same photo-statistics as Super-Kamiokande
+(with a 40\% coverage). In principle up to 5 shafts are possible,
+corresponding to a fiducial mass of 730~kt.
+%
+The Fr\'ejus site offers a natural protection against cosmic rays by a
+factor $10^6$. If not mentioned otherwise, the event selection and
+particle identification are the Super-Kamiokande algorithms results.
+
+\begin{figure}
+\centering
+\includegraphics[width=0.65\textwidth]{./fig1.eps}
+\mycaption{\label{fig:MEMPHYS}Sketch of the MEMPHYS detector under the
+Fr\'ejus mountain.}	
+\end{figure}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The $\gamma = 100\times100$ baseline Beta Beam}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+The concept of a Beta Beam (\BB) has been introduced by P.~Zucchelli
+in Ref.~\cite{zucchelli}. Neutrinos are produced by the decay of
+radioactive isotopes which are stored in a decay ring. An important
+parameter is the relativistic gamma factor of the ions, which
+determines the energy of the emitted neutrinos. \BB\ performances have
+been computed previously for $\gamma(\He)= 66$~\cite{Mezzetto:2003ub},
+100~\cite{MyNufact04,Donini:2004hu,JJHigh2}, 150~\cite{JJHigh2},
+200~\cite{LindnerBB}, 350~\cite{JJHigh2},
+500~\cite{JJHigh1,LindnerBB}, 1000~\cite{LindnerBB},
+2000~\cite{JJHigh1}, 2488~\cite{Terranova}. Reviews can be found in
+Ref.~\cite{BB-Reviews}, the physics potential of a very low gamma \BB\
+has been studied in Ref.~\cite{Volpe}. Performances of a \BB\ with
+$\gamma > 150$ are extremely promising, however, they are neither
+based on an existing accelerator complex nor on detailed calculations
+of the ion decay rates. For a CERN based \BB, fluxes have been
+estimated in Ref.~\cite{Lindroos} and a design study is in progress
+for the facility \cite{Eurisol}. In this work we assume an integrated
+flux of neutrinos in 10 years corresponding to $2.9\cdot 10^{19}$
+useful \He\ decays and $1.1 \cdot 10^{19}$ useful \Ne\ decays. These
+fluxes have been assumed in all the physics papers quoted above, and
+they are two times higher than the baseline fluxes computed in
+Ref.~\cite{Lindroos}. These latter fluxes suffer for the known
+limitations of the PS and SPS synchrotrons at CERN, ways to improve
+them have been delineated in Ref.~\cite{Lindroos-Optimization}.
+
+The infrastructure available at CERN as well as the MEMPHYS
+location at a distance of 130~km suggest a $\gamma$-factor of about
+$100$. Such a value implies a mean neutrino energy of 400~MeV, which
+leads to the oscillation maximum at about 200~km for $\Delta m^2_{31}
+= 2.4\times 10^{-3}$~eV$^2$.  We have checked that the performance at
+the somewhat shorter baseline of 130~km is rather similar to the one
+at the oscillation maximum. Moreover, the purpose of this paper is to
+estimate the physics potential for a realistic set-up and not to study
+the optimization of the \BB\ regardless of any logistic consideration
+(see, e.g., Refs.~\cite{LindnerBB,JJHigh2} for such optimization
+studies).
+
+The signal events from the $\nu_e \to \nu_\mu$ neutrino and
+antineutrino appearance channels in the \BB\ are \numu charged current
+(CC) events. The Nuance v3r503 Monte Carlo code~\cite{Nuance} is used
+to generate signal events. The selection for these events is based on
+standard Super-Kamiokande particle identification algorithms.  The
+muon identification is reinforced by asking for the detection of the
+Michel decay electron. 
+%
+The neutrino energy is reconstructed by smearing momentum and
+direction of the charged lepton with the Super-Kamiokande resolution
+functions, and applying quasi-elastic (QE) kinematics assuming the
+known incoming neutrino direction. Energy reconstruction in the \BB\
+energy range is remarkably powerful, and the contamination of non-QE
+events very small, as shown in Fig.~\ref{fig:QE-Energy}.
+%
+As pointed out in Ref.~\cite{JJHigh2}, it is necessary to use a
+migration matrix for the neutrino energy reconstruction to properly
+handle Fermi motion smearing and the non-QE event contamination.  We
+use 100~MeV bins for the reconstructed energy and 40~MeV bins for the
+true neutrino energy.  Four migration matrices (for
+$\nu_e,\bar\nu_e,\nu_\mu,\bar\nu_\mu$) are applied to signal events as
+well as backgrounds. As suggested from Fig.~\ref{fig:QE-Energy} the 
+results using migration matrices are very similar to a Gaussian
+energy resolution.
+
+\begin{figure}[!t]
+  \centering
+  \includegraphics[width=0.65\textwidth]{./fig2.eps}
+  \mycaption{\label{fig:QE-Energy} Energy resolution for \nue\
+  interactions in the 200--300~MeV energy range. The quantity
+  displayed is the difference between the reconstructed and the true
+  neutrino energy.}
+\end{figure}
+
+Backgrounds from charged pions and atmospheric neutrinos are computed
+with the identical analysis chain as signal events.
+Charged pions generated in NC events (or in NC-like events where the
+leading electron goes undetected) are the main source of background for
+the experiment. To compute this background inclusive NC and CC events
+have been generated with the \BB\ spectrum. Events have been selected
+where the only visible track is a charged pion above the \v{C}erenkov
+threshold. Particle identification efficiencies have been applied to
+those particles. The probability for a pion to survive in water until
+its decay has been computed with Geant~3.21 and cross-checked with a
+Fluka~2003 simulation. This probability is different for positive and
+negative pions, the latter having a higher probability to be absorbed
+before decaying. The surviving events are background, and the
+reconstructed neutrino energy is computed misidentifying these pions
+as muons. Event rates are reported in Tab.~\ref{tab:sigbck}. From
+these numbers it becomes evident that requiring the detection of the
+Michel electron provides an efficient cut to eliminate the pion
+background.
+%
+These background rates are significantly smaller than quoted in
+Ref.~\cite{MyNufact04}, where pion decays were computed with the
+same probabilities as for muons and they are slightly different
+from those quoted in Ref.~\cite{ MezzettoNuFact05}, where an
+older version of Nuance had been used.
+%
+The numbers of Tab.~\ref{tab:sigbck} have been cross-checked by
+comparing the Nuance and Neugen~\cite{Neugen} event
+generators, finding a fair agreement in background rates and energy shape.
+
+\begin{table}[t]
+     \centering
+     \begin{tabular}{l@{\qquad}rrr@{\qquad}rrr}
+     \hline\noalign{\smallskip}
+       & \multicolumn{3}{ c }{\Ne} & \multicolumn{3}{c}{\He} \\
+     \hline\noalign{\smallskip}
+       & \numu CC & $\pi^+$ & $\pi^-$ & \nubarmu CC & $\pi^+$ & $\pi^-$ \\
+     \hline\noalign{\smallskip}
+      Generated ev.\ & 115367   &  557   &  341 & 101899 &  674   &  400 \\
+      Particle ID    &  95717   &  204   &  100 & 85285  &  240   &  118 \\
+      Decay          &  61347   &  107   &    8 & 69242  &  120   &    8 \\
+\hline\noalign{\smallskip}
+    \end{tabular}
+    \mycaption{\label{tab:sigbck} Events for the \BB\ in a 4400~kt~yr
+    exposure.  \numu(\nubarmu) CC events are computed assuming full
+    oscillations ($P_{\nu_e\to\nu_\mu} = 1$), and pion backgrounds are
+    computed from \nue(\nubare) CC+NC events. In the rows we give the
+    number events generated within the fiducial volume (``Generated
+    ev.''), after muon particle identification (``Particle ID''), and
+    after applying a further identification requiring the detection of
+    the Michel electron (``Decay''). }
+\end{table}
+
+Also atmospheric neutrinos can constitute an important source of
+background~\cite{zucchelli,JJHigh2,JJHigh1,MezzettoNuFact05}. This
+background can be suppressed only by keeping a very short duty cycle
+($2.2 \cdot 10^{-3}$ is the target value for the \BB\ design study),
+and this in turn is one of the most challenging bounds on the design
+of the Beta Beam complex. Following Ref.~\cite{MezzettoNuFact05} we
+include the atmospheric neutrino background based on a Monte Carlo
+simulation using Nuance. Events are reconstructed as if they were
+signal neutrino events. We estimate that 5 events/year would survive
+the analysis chain in a full solar year (the \BB\ should run for about
+1/3 of this period) and include these events as backgrounds in the
+analysis. Under these circumstances, the present value of the \BB\
+duty cycle seems to be an overkill, it could be reduced by a factor 5
+at least, see also Ref.~\cite{MezzettoNuFact05} for a discussion of
+the effect of a higher duty cycle.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The $3.5$-GeV SPL Super Beam}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
+In the recent Conceptual Design Report 2 (CDR2) the foreseen Super
+Proton Linac (SPL)~\cite{SPL} will provide the protons for the muon
+production in the context of a Neutrino Factory, and at a first stage
+will feed protons to a fixed target experiment to produce an intense
+conventional neutrino beam (``Super Beam''). The parameters of the
+beam line take into account the optimization~\cite{Campagne:2004wt} of
+the beam energy as well as the secondary particle focusing and decay
+to search for $\nu_\mu \rightarrow \nu_e$ and $\bar{\nu}_\mu
+\rightarrow \bar{\nu}_e$ appearance as well as $\nu_\mu$,
+$\bar\nu_\mu$ disappearance in a mega ton scale water \v{C}erenkov
+detector. In particular, a full simulation of the beam line from the
+proton on target interaction up to the secondary particle decay tunnel
+has been performed. The proton on a liquid mercury target (30~cm long,
+$7.5$~mm radius, 13.546 density) has been simulated with
+FLUKA~2002.4~\cite{FLUKA} while the horn focusing system and the decay
+tunnel simulation has been preformed with
+GEANT~3.21~\cite{GEANT}.\footnote{Although there are differences
+between the predicted pion and kaon productions as a function of
+proton kinetic energy with FLUKA~2002.4 and 2005.6, the results are
+consistent for the relevant energy of 3.5~GeV. We emphasize that the
+pion and the kaon production cross-sections are waiting for
+experimental confirmation~\cite{HARP-MINERVA} and a new optimization
+would be required if their is a disagreement with the present
+knowledge.}
+
+\begin{figure}[!t]
+  \centering 
+  \includegraphics[width=0.65\textwidth]{./fig3.eps}
+  \mycaption{\label{fig:fluxSPLContrib} Neutrino fluxes, at $130$~km
+  from the target with the horns focusing the positive particles
+  (top panel) or the negative particles (bottom panel). The fluxes are
+  computed for a SPL proton beam of $3.5$~GeV (4~MW), a decay tunnel
+  with a length of $40$~m and a radius of $2$~m.}
+\end{figure}
+
+Since the optimization requirements for a Neutrino Factory are rather
+different than for a Super Beam the new SPL configuration has a
+significant impact on the physics performance (see
+Ref.~\cite{Campagne:2004wt} for a detailed discussion).  The SPL
+fluxes of the four neutrino species ($\nu_\mu$, $\nu_e$,
+$\bar{\nu}_\mu$, $\bar{\nu}_e$) for the positive ($\nu_\mu$ beam) and
+the negative focusing ($\bar{\nu}_\mu$ beam) are show in
+Fig.~\ref{fig:fluxSPLContrib}.  The total number of $\nu_\mu$
+($\bar{\nu}_\mu$) in positive (negative) focusing is about
+$1.18\,(0.97) \times 10^{12}\:\mathrm{m}^{-2}\mathrm{y}^{-1}$ with an
+average energy of $300$~MeV. The $\nu_e$ ($\bar{\nu}_e$) contamination
+in the $\nu_\mu$ ($\bar\nu_\mu$) beam is around $0.7\%$
+($6.0\%$). 
+%
+Following Ref.~\cite{Mezzetto:2003mm}, the $\pi^o$ background is
+reduced using a tighter PID cut compared to the standard
+Super-Kamiokande analysis used in K2K, but the cuts are looser than
+for T2K. Indeed, at SPL energies the $\pi^o$ background is less severe
+than for T2HK. This is because the resonant cross section is
+suppressed, and the produced pions have an energy where the angle
+between the two gammas is very wide, leading to a small probability
+that the two gamma rings overlap. This results in a higher signal
+efficiency of SPL compared to T2HK (70\% against 40\%) and a smaller
+rate of $\pi^o$ background.
+%
+The Michel electron is required for the $\mu$ identification.
+%
+For the $\nu_\mu \rightarrow \nu_e$ channel the background consists
+roughly of 90\% $\nu_e \rightarrow \nu_e$ CC interactions, 6\% $\pi^o$
+from NC interactions, 3\% miss identified muons from $\nu_\mu
+\rightarrow \nu_\mu$ CC, and 1\% $\bar{\nu}_e \rightarrow \bar{\nu}_e$
+CC interactions. For the $\bar{\nu}_\mu \rightarrow \bar{\nu}_e$
+channel the contributions to the background are 45\% $\bar{\nu}_e
+\rightarrow \bar{\nu}_e$ CC interactions, 35\% $\nu_e \rightarrow
+\nu_e$ CC interactions, 18\% $\pi^o$ from NC interactions and 2\% miss
+identified muons from $\bar{\nu}_\mu \rightarrow \bar{\nu}_\mu$ CC.
+In addition we include the events from the contamination of 
+``wrong sign'' muon-neutrinos due to $\bar\nu_\mu \to \bar\nu_e$
+($\nu_\mu \to \nu_e$) oscillations in the neutrino (antineutrino)
+mode. 
+%
+We have checked that with the envisaged duty cycle of $2.4\times
+10^{-4}$ the background from atmospheric neutrinos is negligible for
+the SPL.
+
+\begin{figure}[!t]
+  \centering
+  \includegraphics[width=0.5\textwidth]{./fig4.eps}
+%
+  \mycaption{\label{fig:fluxComparison} 
+  Comparison of the fluxes from SPL and \BB.}
+\end{figure}
+
+Considering the signal over square-root of background
+ratio, the $3.5$~GeV beam energy is more favorable than the original
+$2.2$~GeV option. Compared to the fluxes used in
+Refs.~\cite{Mezzetto:2003mm,Donini:2004hu} the gain is at least a
+factor $2.5$ and this justifies to reconsider in detail the physics
+potential of the SPL Super Beam.
+%
+Both the appearance and the disappearance channels are used. For the
+spectral analysis we use 10 bins of 100~MeV in the interval $0 < E_\nu
+< 1$~GeV, applying the same migration matrices as for the \BB\ to take
+into account properly the neutrino energy reconstruction. As ultimate
+goal suggested in Ref.~\cite{T2K} a 2\% systematical error is used as
+default both for signal and background, this would be achieved by a
+special care of the design of the close position. However, we discuss
+also how a 5\% systematical error affects the sensitivities.
+%
+Using neutrino cross-sections on water from Ref.~\cite{Nuance}, the
+number of expected $\nu_\mu$ charged current is about $98$ per
+kt~yr. In Fig.~\ref{fig:fluxComparison} we compare the fluxes from the
+SPL to the one from the \BB.
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The atmospheric neutrino analysis}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:atm-details}
+
+The simulation of atmospheric neutrino data in MEMPHYS is based on the
+analysis presented in Ref.~\cite{Huber:2005ep}, with the following
+differences:
+%
+\begin{itemize}
+  \item We replace the neutrino fluxes at Kamioka with those at Gran
+    Sasso. We use the Honda calculations~\cite{Honda:2004yz}, which
+    unfortunately are not yet available for the Fr\'ejus
+    site. However, since the fluxes increase with the geomagnetic
+    latitude and Fr\'ejus is northern than Gran Sasso, our choice is
+    conservative.
+    
+  \item We take into account the specific geometry of the MEMPHYS
+    detector. This is particularly important to properly separate
+    fully contained from partially contained events, as well as
+    stopping muon from through-going muon events.
+    
+  \item We divide our total data sample into 420 different bins:
+    fully contained single-ring events, further subdivided according
+    to flavor ($e$-like or $\mu$-like), lepton momentum (8 bins:
+    0.1--0.3, 0.3--0.5, 0.5--1, 1--2, 2--3, 3--5, 5--8,
+    8--$\infty$~GeV) and lepton direction (20 bins in zenith angle);
+%
+    fully contained multi-ring events, further subdivided according to
+    flavor ($e$-like or $\mu$-like), reconstructed neutrino energy (3
+    bins: 0--1.33, 1.33--5, 5--$\infty$~GeV) and lepton direction (10
+    bins in zenith angle);
+%    	
+    partially contained $\mu$-like events, divided into 20 zenith bins;
+%	
+    up-going muons, divided into stopping and through-going events, and in
+    10 zenith bins each.
+
+    \item We include in our calculations the neutral-current
+      contamination of each bin. To this extent we assume that the
+      ratio between neural-current and \emph{unoscillated}
+      charged-current events in MEMPHYS is the same as in
+      Super-Kamiokande, and we take this ratio from
+      Ref.~\cite{Ashie:2005ik}.
+      
+    \item We consider also multi-ring events, which we define
+      as fully contained charged-current events which are \emph{not}
+      tagged as single-ring. Again, we assume that the survival
+      efficiency and the NC contamination are the same as for
+      Super-Kamiokande~\cite{Ashie:2005ik}.
+\end{itemize}
+
+The expected number of contained events is given by:
+%
+\begin{multline} \label{eq:contained}
+    N_b(\vec\omega) = N_b^\text{NC} +
+    n_\text{tgt} T \sum_{\alpha,\beta,\pm}
+    \int_0^\infty dh \int_{-1}^{+1} dc_\nu
+    \int_{\Emin}^\infty dE_\nu \int_{\Emin}^{E_\nu} dE_l
+    \int_{-1}^{+1} dc_a \int_0^{2\pi} d\varphi_a
+    \\
+    \frac{d^3 \Phi_\alpha^\pm}{dE_\nu \, dc_\nu \, dh}(E_\nu, c_\nu, h)
+    \, P_{\alpha\to\beta}^\pm(E_\nu, c_\nu, h \,|\, \vec\omega)
+    \, \frac{d^2\sigma_\beta^\pm}{dE_l \, dc_a}(E_\nu, E_l, c_a)
+    \, \varepsilon_\beta^b(E_l, c_l(c_\nu, c_a, \varphi_a))
+    \,,
+\end{multline}
+%
+where $P_{\alpha\to\beta}^+$ ($P_{\alpha\to\beta}^-$) is the
+$\nu_\alpha \to \nu_\beta$ ($\bar{\nu}_\alpha \to \bar{\nu}_\beta$)
+conversion probability for given values of the neutrino energy
+$E_\nu$, the cosine $c_\nu$ of the angle between the incoming neutrino
+and the vertical direction, the production altitude $h$, and the
+neutrino oscillation parameters $\vec\omega$. We calculate the
+conversion probability numerically in the general three-flavor
+framework taking into account matter effects from a realistic Earth
+density profile. Further, $N_b^\text{NC}$ is the neutral-current
+background for the bin $b$, $n_\text{tgt}$ is the number of targets,
+$T$ is the experiment running time, $\Phi_\alpha^+$ ($\Phi_\alpha^-$)
+is the flux of atmospheric neutrinos (antineutrinos) of type $\alpha$,
+and $\sigma_\beta^+$ ($\sigma_\beta^-$) is the charged-current
+neutrino- (antineutrino-) nucleon interaction cross section.
+%
+The variable $E_l$ is the energy of the final lepton of type $\beta$,
+while $c_a$ and $\varphi_a$ parametrize the opening angle between the
+incoming neutrino and the final lepton directions as determined by the
+kinematics of the neutrino interaction.
+%
+Finally, $\varepsilon_\beta^b$ gives the probability that a charged
+lepton of type $\beta$, energy $E_l$ and direction $c_l$ contributes
+to the bin $b$.
+
+Up-going muon events are calculated as follows:
+%
+\begin{multline} \label{eq:upgoing}
+    N_b(\vec\omega) = \rho_\text{rock} T \sum_{\alpha,\pm} 
+    \int_0^\infty dh \int_{-1}^{+1} dc_\nu
+    \int_{\Emin}^\infty dE_\nu 
+    \int_{\Emin}^{E_\nu} dE^0_\mu \int_{\Emin}^{E^0_\mu} d\Efin_\mu
+    \int_{-1}^{+1} dc_a \int_0^{2\pi} d\varphi_a
+    \\
+    \frac{d^3 \Phi_\alpha^\pm}{dE_\nu \, dc_\nu \, dh}(E_\nu, c_\nu, h)
+    \, P_{\alpha\to\mu}^\pm(E_\nu, c_\nu, h \,|\, \vec\omega)
+    \, \frac{d^2\sigma_\mu^\pm}{dE^0_\mu \, dc_a}(E_\nu, dE^0_\mu, c_a)
+    \\
+    \times R_\text{rock}(E^0_\mu,\Efin_\mu)
+    \, \mathcal{A}_\text{eff}^b(\Efin_\mu,
+    c_l(c_\nu, c_a, \varphi_a)) \,,
+\end{multline}
+%
+where $\rho_\text{rock}$ is the density of targets in standard rock,
+$R_\text{rock}$ is the effective muon range~\cite{Lipari:1991ut} for a
+muon which is produced with energy $E^0_\mu$ and reaches the detector
+with energy $\Efin_\mu$, and $\mathcal{A}_\text{eff}^b$ is the
+effective area for the bin $b$. The other variables and physical
+quantities are the same as for contained events.
+
+The statistical analysis is based on the pull method, as described in
+Ref.~\cite{Gonzalez-Garcia:2004wg}. In our analysis we include three
+different kind of experimental uncertainties:
+%
+Flux uncertainties: total normalization (20\%), tilt factor (5\%),
+zenith angle (5\%), $\nu/\bar\nu$ ratio (5\%), and $\mu/e$ ratio
+(5\%);
+%    
+cross-section uncertainties: total normalization (15\%) and $\mu/e$
+ratio (1\%) for each type of charged-current interaction
+(quasi-elastic, one-pion production, and deep-inelastic scattering),
+and total normalization (15\%) for the neutral-current contributions;
+%    
+systematic uncertainties: same as in previous analyses, details are
+given in the Appendix of Ref.~\cite{Gonzalez-Garcia:2004wg}. In
+addition, we assume independent normalization uncertainties (20\%) for
+$e$-like and $\mu$-like multi-ring events.
+%
+Since we are dividing our data sample into a large number of bins, it
+is important to use Poisson statistics as some of the bins contain
+only a few number of events. We therefore write our $\chi^2$ as:
+%
+\begin{equation} \label{eq:poisson}
+    \chi^2(\vec\omega) = \min_{\vec\xi} \left[ 2 \sum_b \left(
+    N_b^\text{th}(\vec\omega,\, \vec\xi)
+    - N_b^\text{ex} + N_b^\text{ex} \ln\frac{N_b^\text{ex}}
+    {N_b^\text{th}(\vec\omega,\, \vec\xi)} \right) 
+    + \sum_n \xi_n^2 \right] \,,
+\end{equation}
+%
+where the number of events for a given value of the pulls $\vec\xi$ is
+given by:
+%
+\begin{equation} \label{eq:theopulls}
+    N_b^\text{th}(\vec\omega,\, \vec\xi) = N_b^\text{th}(\vec\omega) \,
+    \exp\left( \sum_n \pi_b^n(\vec\omega)\, \xi_n \right) \,.
+\end{equation}
+%
+The use of an exponential dependence on the pulls in
+Eq.~\eqref{eq:theopulls}, rather than the usual linear dependence,
+ensures that the theoretical predictions remain positive for
+\emph{any} value of the pulls, thus avoiding numerical inconsistencies
+during the pull minimization procedure.
+
+ 
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Degeneracies}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:degeneracies}
+
+
+A characteristic feature in the analysis of future LBL experiments is
+the presence of {\it parameter degeneracies}.  Due to the inherent
+three-flavor structure of the oscillation probabilities, for a given
+experiment in general several disconnected regions in the
+multi-dimensional space of oscillation parameters will be
+present. Traditionally these degeneracies are referred to in the
+following way:
+%
+\begin{itemize}
+\item
+The {\it intrinsic} or
+($\delCP,\theta_{13}$)-degeneracy~\cite{Burguet-Castell:2001ez}:
+For a measurement based on the $\nu_\mu \to \nu_e$ oscillation probability for
+neutrinos and antineutrinos two disconnected solutions appear in the
+($\delCP,\theta_{13}$) plane.
+\item
+The {\it hierarchy} or sign($\Delta
+m^2_{31}$)-degeneracy~\cite{Minakata:2001qm}: The two solutions
+corresponding to the two signs of $\Delta m^2_{31}$ appear in general
+at different values of $\delCP$ and $\theta_{13}$.
+\item
+The {\it octant} or $\theta_{23}$-degeneracy~\cite{Fogli:1996pv}:
+Since LBL experiments are sensitive mainly to $\sin^22\theta_{23}$ it
+is difficult to distinguish the two octants $\theta_{23} < \pi/4$ and
+$\theta_{23} > \pi/4$.  Again, the solutions corresponding to
+$\theta_{23}$ and $\pi/2 - \theta_{23}$ appear in general at different
+values of $\delCP$ and $\theta_{13}$.
+\end{itemize}
+%
+This leads to an eight-fold ambiguity in $\theta_{13}$ and
+$\delCP$~\cite{Barger:2001yr}, and hence degeneracies provide a
+serious limitation for the determination of $\theta_{13}$, $\delCP$,
+and the sign of $\Delta m^2_{31}$. Recent discussions of degeneracies
+can be found for example in
+Refs.~\cite{Huber:2002mx,Huber:2005ep,Yasuda:2004gu,Ishitsuka:2005qi};
+degeneracies in the context of CERN--Fr\'ejus \BB\ and SPL have been
+considered previously in Ref.~\cite{Donini:2004hu}.
+%
+In Fig.~\ref{fig:degeneracies} we illustrate the effect of
+degeneracies for the \BB, SPL, and T2HK experiments. Assuming the
+true parameter values $\delta_\mathrm{CP} = -0.85 \pi$,
+$\sin^22\theta_{13} = 0.03$, $\sin^2\theta_{23} = 0.6$ we show the
+allowed regions in the plane of $\stheta$ and $\delCP$ taking into
+account the solutions with the wrong hierarchy and the wrong octant of
+$\theta_{23}$.
+
+\begin{figure}[!t]
+\centering
+\includegraphics[width=0.95\textwidth]{./fig5.eps}
+%
+  \mycaption{Allowed regions in $\sin^22\theta_{13}$ and
+  $\delta_\mathrm{CP}$ for LBL data alone (contour lines) and LBL+ATM
+  data combined (colored regions). $\mathrm{H^{tr/wr} (O^{tr/wr})}$
+  refers to solutions with the true/wrong mass hierarchy (octant of
+  $\theta_{23}$). The true parameter values are $\delta_\mathrm{CP} =
+  -0.85 \pi$, $\sin^22\theta_{13} = 0.03$, $\sin^2\theta_{23} = 0.6$,
+  and the values from Eq.~(\ref{eq:default-params}) for the other
+  parameters. The running time is ($5\nu + 5\bar\nu$)~yrs for \BB\ and
+  ($2\nu + 8\bar\nu$)~yrs for the Super Beams.}
+\label{fig:degeneracies}
+\end{figure}
+
+
+\begin{figure}[!t]
+\centering
+\includegraphics[width=0.9\textwidth]{./fig6.eps}
+%
+  \mycaption{Resolving degeneracies in SPL by successively using the
+  appearance rate measurement, disappearance channel rate and
+  spectrum, spectral information in the appearance channel, and
+  atmospheric neutrinos.  Allowed regions in $\sin^22\theta_{13}$ and
+  $\delta_\mathrm{CP}$ are shown at 95\%~CL, and $\mathrm{H^{tr/wr}
+  (O^{tr/wr})}$ refers to solutions with the true/wrong mass hierarchy
+  (octant of $\theta_{23}$). The true parameter values are
+  $\delta_\mathrm{CP} = -0.85 \pi$, $\sin^22\theta_{13} = 0.03$,
+  $\sin^2\theta_{23} = 0.6$, and the values from
+  Eq.~(\ref{eq:default-params}) for the other parameters. The running
+  time is ($2\nu + 8\bar\nu$)~yrs.
+
+}
+\label{fig:degeneracies_SPL}
+\end{figure}
+
+As visible in Fig.~\ref{fig:degeneracies} for the
+Super Beam experiments SPL and T2HK there is only a four-fold
+degeneracy related to sign($\Delta m^2_{31}$) and the octant of
+$\theta_{23}$, whereas the intrinsic degeneracy can be resolved. 
+%
+Several pieces of information contribute to this effect, as we
+illustrate at the example of SPL in Fig.~\ref{fig:degeneracies_SPL}.
+The dashed curves in the left panel of this figure show the allowed
+regions for only the appearance measurement (for neutrinos and
+antineutrinos) without spectral information, i.e., just a counting
+experiment. In this case the eight-fold degeneracy is present in its
+full beauty, and one finds two solutions (corresponding to the
+intrinsic degeneracy) for each choice of sign($\Delta m^2_{31}$) and
+the octant of $\theta_{23}$. Moreover, the allowed regions are
+relatively large. For the thin solid curves the information from the
+disappearance rate is added. The main effect is to decrease the size
+of the allowed regions in $\stheta$. This is especially pronounced for
+the solutions involving the wrong octant of $\theta_{23}$, since these
+solutions are strongly affected by an uncertainty in $\theta_{23}$
+which gets reduced by the disappearance information. Using in addition
+to the disappearance rate also the spectrum again decreases the size
+of the allowed regions, however, still all eight solutions are present
+(compare dashed curves in the right panel).
+%
+The most relevant effect comes from the inclusion of spectral
+information in the appearance channel, as visible from the comparison
+of the dashed and thick-solid curves in the right panel of
+Fig.~\ref{fig:degeneracies_SPL}. The intrinsic degeneracy gets
+resolved and only four solutions corresponding to the sign and octant
+degeneracies are left (see, e.g.,
+Refs.~\cite{Huber:2002mx,Huber:2005ep,Ishitsuka:2005qi}).\footnote{The
+inclusion of spectral information might be the source of possible
+differences to previous studies, see e.g.\ Ref.~\cite{Donini:2004hu}.}
+Note that the thick curves in the right panel of
+Fig.~\ref{fig:degeneracies_SPL} correspond to the regions show in
+Fig.~\ref{fig:degeneracies} for the SPL.
+%
+Finally, by the inclusion of information from atmospheric neutrinos
+all degeneracies can be resolved in this example, and the true
+solution is identified at 95\%~CL (see Sec.~\ref{sec:atmospherics} and
+Ref.~\cite{Huber:2005ep} for further discussions of atmospheric
+neutrinos).
+
+Concerning the \BB\ one observes from Fig.~\ref{fig:degeneracies} that
+in this case the ($\delCP,\theta_{13}$)-degeneracy cannot be resolved
+and one has to deal with eight distinct solutions. One reason for this
+is the absence of precise information on $|\Delta m^2_{31}|$ and
+$\sin^22\theta_{23}$ which is provided by the $\nu_\mu$ disappearance
+in Super Beam experiments but is not available from the \BB. If
+external information on these parameters at the level of 3\% is
+included the allowed regions in Fig.~\ref{fig:degeneracies} are
+significantly reduced. However, still all eight solutions are present,
+which indicates that for the \BB\ spectral information is not
+efficient enough to resolve the ($\delCP,\theta_{13}$)-degeneracy, and
+in this case only the inclusion of atmospheric neutrino data allows a
+nearly complete resolution of the degeneracies.
+
+An important observation from Fig.~\ref{fig:degeneracies} is that
+degeneracies have only a very small impact on the CP violation
+discovery, in the sense that if the true solution is CP violating also
+the fake solutions are located at CP violating values of
+$\delCP$. Indeed, since for the relatively short baselines in the
+experiments under consideration matter effects are very small, the
+sign($\Delta m^2_{31}$)-degenerate solution is located within good
+approximation at $\delCP' \approx \pi -
+\delCP$~\cite{Minakata:2001qm}. Therefore, although degeneracies
+strongly affect the determination of $\theta_{13}$ and $\delCP$ they
+have only a small impact on the CP violation discovery potential.
+Furthermore, as clear from Fig.~\ref{fig:degeneracies} the sign($\Delta
+m^2_{31}$) degeneracy has practically no effect on the $\theta_{13}$
+measurement, whereas the octant degeneracy has very little impact on
+the determination of $\delCP$.
+
+\begin{figure}[!t]
+\centering
+\includegraphics[width=0.9\textwidth]{./fig7.eps}
+%
+  \mycaption{Allowed regions in $\sin^22\theta_{13}$ and
+  $\delta_\mathrm{CP}$ for 5~years data (neutrinos only) from \BB,
+  SPL, and the combination. $\mathrm{H^{tr/wr} (O^{tr/wr})}$ refers to
+  solutions with the true/wrong mass hierarchy (octant of
+  $\theta_{23}$). For the colored regions in the left panel also
+  5~years of atmospheric data are included; the solution with the
+  wrong hierarchy has $\Delta\chi^2 = 4$. The true parameter
+  values are $\delta_\mathrm{CP} = -0.85 \pi$, $\sin^22\theta_{13} =
+  0.03$, $\sin^2\theta_{23} = 0.6$, and the values from
+  Eq.~(\ref{eq:default-params}) for the other parameters. For the \BB\
+  only analysis (middle panel) an external accuracy of 2\% (3\%) for
+  $|\Delta m^2_{31}|$ ($\theta_{23}$) has been assumed, whereas for
+  the left and right panel the default value of 10\% has been used.}
+\label{fig:degeneracies_5yrs}
+\end{figure}
+
+Fig.~\ref{fig:degeneracies} shows also that the fake solutions occur
+at similar locations in the ($\stheta$, $\delCP$) plane for \BB\ and
+SPL. Therefore, as noted in Ref.~\cite{Donini:2004hu}, in this sense
+the two experiments are not complementary, and the combination of
+10~years of \BB\ and SPL data is not very effective in resolving
+degeneracies. This is obvious since the baseline is the same and the
+neutrino energies are similar.
+%
+Note however, that the \BB\ looks for $\nu_e\to\nu_\mu$ appearance,
+whereas in SPL the T-conjugate channel $\nu_\mu\to\nu_e$ is observed.
+Assuming CPT invariance the relation $P_{\nu_\alpha\to\nu_\beta} =
+P_{\bar\nu_\beta\to\bar\nu_\alpha}$ holds, which implies that the
+antineutrino measurement can be replaced by a measurement in the
+T-conjugate channel.  Hence, if \BB\ and SPL experiments are available
+simultaneously the full information can be obtained just from neutrino
+data, and in principle the (time consuming) antineutrino measurement 
+is not necessary. As shown in Fig.~\ref{fig:degeneracies_5yrs} the
+combination of 5~yrs neutrino data from the \BB\ with 5~yrs of
+neutrino data from SPL leads to a result very close to the 10~yrs
+neutrino+antineutrino data from one experiment alone. Hence, if \BB\
+and SPL experiments are available simultaneously the data taking
+period is reduced approximately by a factor of 2 with respect to a
+single experiment. This synergy is discussed later in
+Sec.~\ref{sec:synergies-beams} in the context of the $\theta_{13}$ and
+CP violation discovery potentials.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Physics potential}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:sensitivities}
+
+\subsection{Sensitivity to the atmospheric parameters}
+\label{sec:atm}
+
+The $\nu_\mu$ disappearance channel available in the Super Beam
+experiments SPL and T2HK allows a precise determination of the
+atmospheric parameters $|\Delta m^2_{31}|$ and $\sin^22\theta_{23}$,
+see, e.g., Refs.~\cite{Antusch:2004yx,Minakata:2004pg,Donini:2005db}
+for recent analyses). Fig.~\ref{fig:atm-params} illustrates the
+improvement on these parameters by Super Beam experiments with respect
+to the present knowledge from SK atmospheric and K2K data. We show the
+allowed regions at 99\%~CL for T2K-I, SPL, and T2HK, where in all
+three cases 5~years of neutrino data are assumed. T2K-I corresponds to
+the phase~I of the T2K experiment with a beam power of 0.77~MW and the
+Super-Kamiokande detector as target~\cite{T2K}. In Tab.~\ref{tab:atm-params} we
+give the corresponding relative accuracies at 3$\sigma$ for $|\Delta
+m^2_{31}|$ and $\sin^2\theta_{23}$.
+
+\begin{figure}[!t]
+\centering
+  \includegraphics[width=0.55\textwidth]{./fig8.eps}
+  \mycaption{\label{fig:atm-params} Allowed regions of $\Delta
+  m^2_{31}$ and $\sin^2\theta_{23}$ at 99\%~CL (2 d.o.f.)  after 5~yrs
+  of neutrino data taking for SPL, T2K phase~I, T2HK, and the
+  combination of SPL with 5~yrs of atmospheric neutrino data in the
+  MEMPHYS detector. For the true parameter values we use $\Delta
+  m^2_{31} = 2.2\, (2.6) \times 10^{-3}~\mathrm{eV}^2$ and
+  $\sin^2\theta_{23} = 0.5 \, (0.37)$ for the test point 1 (2), and
+  $\theta_{13} = 0$ and the solar parameters as given in
+  Eq.~(\ref{eq:default-params}). The shaded region corresponds to the
+  99\%~CL region from present SK and K2K data~\cite{Maltoni:2004ei}.}
+\end{figure}
+
+
+\begin{table}[!t]
+  \centering
+  \begin{tabular}{lcrrr}
+  \hline\noalign{\smallskip}
+    & True values  & T2K-I & SPL & T2HK \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  $\Delta m^2_{31}$   & $2.2\cdot 10^{-3}$ eV$^2$ & 4.7\% & 3.2\% & 1.1\% \\
+  $\sin^2\theta_{23}$ & $0.5$                     & 20\%  & 20\%  & 6\%   \\
+  \noalign{\smallskip}\hline\noalign{\smallskip}
+  $\Delta m^2_{31}$   & $2.6\cdot 10^{-3}$ eV$^2$ & 4.4\% & 2.5\% & 0.7\% \\
+  $\sin^2\theta_{23}$ & $0.37$                    & 8.9\% & 3.1\% & 0.8\% \\
+  \noalign{\smallskip}\hline
+  \end{tabular}
+  \mycaption{Accuracies at $3\sigma$ on the atmospheric parameters
+  $|\Delta m^2_{31}|$ and $\sin^2\theta_{23}$ for 5 years of neutrino
+  data from T2K-I, SPL, and T2HK for the two test points shown in
+  Fig.~\ref{fig:atm-params} ($\theta^\mathrm{true}_{13} = 0$). The
+  accuracy for a parameter $x$ is defined as $(x^\mathrm{upper} -
+  x^\mathrm{lower})/(2 x^\mathrm{true})$, where $x^\mathrm{upper}$
+  ($x^\mathrm{lower}$) is the upper (lower) bound at 3$\sigma$ for
+  1~d.o.f.\ obtained by projecting the contour $\Delta \chi^2 = 9$
+  onto the $x$-axis. For the accuracies for test point~2 the octant
+  degenerate solution is neglected.\label{tab:atm-params}}
+\end{table}
+
+From the figure and the table it becomes evident that the T2K setups
+are very good in measuring the atmospheric parameters, and only a
+modest improvement is possible with SPL with respect to T2K phase~I.
+T2HK provides an excellent sensitivity for these parameters, and for
+the example of the test point~2 sub-percent accuracies are obtained at
+3$\sigma$. The disadvantage of SPL with respect to T2HK is the
+limited spectral information. Because of the lower beam energy
+nuclear Fermi motion is a severe limitation for energy reconstruction
+in SPL, whereas in T2K the somewhat higher energy allows an efficient
+use of spectral information of quasi-elastic events. Indeed, due to
+the large number of events in the disappearance channel (cf.\
+Tab.~\ref{tab:events}) the measurement is completely dominated by the
+spectrum, and even increasing the normalization uncertainty up to
+100\% has very little impact on the allowed regions. The effect of
+spectral information on the disappearance measurement is
+discussed in some detail in Ref.~\cite{Donini:2005db}.
+
+In the interpretation of the numbers given in
+Tab.~\ref{tab:atm-params} one should consider that at accuracies below
+1\% systematics might become important, which are not accounted for
+here. We do include the most relevant systematics (see
+Secs.~\ref{sec:analysis} and \ref{sec:experiments}), however, at that
+level additional uncertainties related to, for example, the spectral
+shapes of signal and/or background, or the energy calibration might
+eventually limit the accuracy.
+
+For the test point~1, with maximal mixing for $\theta_{23}$, rather
+poor accuracies of $\sim20\%$ for T2K-I and SPL, and $6\%$ for T2HK
+are obtained for $\sin^2\theta_{23}$. The reason is that in the
+disappearance channel $\sin^22\theta_{23}$ is measured with high
+precision, which translates to rather large errors for
+$\sin^2\theta_{23}$ if $\theta_{23} = \pi/4$~\cite{Minakata:2004pg}.
+%
+For the same reason it is difficult to resolve the octant degeneracy,
+and for the test point~2, with a non-maximal value of
+$\sin^2\theta_{23} = 0.37$, for all three LBL experiments the
+degenerate solution is present around $\sin^2\theta_{23} = 0.63$.
+%
+As pointed out in Refs.~\cite{Peres:2003wd,Gonzalez-Garcia:2004cu}
+atmospheric neutrino data may allow to distinguish between the two
+octants of $\theta_{23}$. If 5~years of atmospheric neutrino data in
+MEMPHYS are added to the SPL data, the degenerate solution for the
+test point~2 can be excluded at more than $5\sigma$ and hence the
+octant degeneracy is resolved in this example, see
+Sec.~\ref{sec:atmospherics} for a more detailed discussion.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{The $\theta_{13}$ discovery potential}
+\label{sec:th13}
+
+If no finite value of $\theta_{13}$ is discovered by the next round of
+experiments an important task of the experiments under consideration
+here is to push further the sensitivity to this parameter. In this
+section we address this problem, where we use to following definition
+of the $\theta_{13}$ discovery potential: Data are simulated for a
+finite true value of $\stheta$ and a given true value for $\delCP$. If
+the $\Delta\chi^2$ of the fit to these data with $\theta_{13} = 0$ is
+larger than 9 the corresponding true value of $\theta_{13}$ ``is
+discovered at 3$\sigma$''. In other words, the $3\sigma$ discovery
+limit as a function of the true $\delCP$ is given by the true value of
+$\stheta$ for which $\Delta\chi^2(\theta_{13}=0) = 9$. In the fitting
+process we minimize the $\Delta\chi^2$ with respect to $\theta_{12}$,
+$\theta_{23}$, $\Delta m^2_{12}$, and $\Delta m^2_{31}$, and in
+general one has to test also for degenerate solutions in sign($\Delta
+m^2_{31}$) and the octant of $\theta_{23}$.
+
+\begin{figure}
+  \centering \includegraphics[width=0.9\textwidth]{./fig9.eps}
+  \mycaption{$3\sigma$ discovery sensitivity to $\stheta$ for \BB,
+  SPL, and T2HK as a function of the true value of \delCP\ (left
+  panel) and as a function of the fraction of all possible values of
+  \delCP\ (right panel). The running time is ($5\nu + 5\bar\nu$)~yrs
+  for \BB\ and ($2\nu + 8\bar\nu$)~yrs for the Super Beams. The width
+  of the bands corresponds to values for the systematical errors
+  between 2\% and 5\%. The black curves correspond to the combination
+  of \BB\ and SPL with 10~yrs of total data taking each for a
+  systematical error of 2\%, and the dashed curves show the
+  sensitivity of the \BB\ when the number of ion decays/yr are reduced
+  by a factor of two with respect to the values given in
+  Tab.~\ref{tab:setups}.\label{fig:th13}}
+\end{figure}
+
+The discovery limits are shown for \BB, SPL, and T2HK in
+Fig.~\ref{fig:th13}. One observes that SPL and T2HK are rather similar
+in performance, whereas the \BB\ with our standard fluxes performs
+significantly better. For all three facilities a guaranteed discovery
+reach of $\stheta \simeq 5\times 10^{-3}$ is obtained, irrespective of
+the actual value of \delCP, however, for certain values of \delCP\ the
+sensitivity is significantly improved. For SPL and T2HK discovery
+limits around $\stheta \simeq 10^{-3}$ are possible for a large
+fraction of all possible values of \delCP, whereas for our standard
+\BB\ a sensitivity below $\stheta = 4\times 10^{-4}$ is reached for
+80\% of all possible values of \delCP. If 10~years of data from \BB\
+and SPL are combined the discovery limit is dominated by the \BB.
+%
+Let us stress that the \BB\ performance depends crucially on the
+neutrino flux intensity, as can be seen from the dashed curves in
+Fig.~\ref{fig:th13}, which has been obtained by reducing the number of
+ion decays/yr by a factor of two with respect to our standard values
+given in Tab.~\ref{tab:setups}. In this case the sensitivity decreases
+significantly, but still values slightly better than from the
+Super Beam experiments are reached.
+
+The peak of the sensitivity curves around $\delCP \approx \pi$ appears
+due to the interplay of neutrino and antineutrino data. For the Super
+Beams neutrino (antineutrino) data are most sensitive in the region
+$\pi \lesssim \delCP \lesssim 2\pi$ ($0 \lesssim \delCP \lesssim
+\pi$), and opposite for the \BB, compare also Fig.~\ref{fig:th13-5yrs}
+in Sec.~\ref{sec:synergies-beams}. The particular shape of the
+sensitivity curves emerges from the relative location of the
+corresponding curves for neutrino and antineutrino data, which is
+controlled by the $L/E_\nu$ value where the experiment is operated and
+the value of $|\Delta m^2_{31}|$. The fact that the peak is most
+pronounced for the \BB\ follows from the somewhat smaler $L/E_\nu$ of
+the \BB\ compared to the Super Beams, whereas the shapes for SPL and
+T2HK are similar because of the similar $L/E_\nu$ values.
+
+In Fig.~\ref{fig:th13} we illustrate also the effect of systematical
+errors on the $\theta_{13}$ discovery reach. The lower boundary of the
+band for each experiment corresponds to a systematical error of 2\%,
+whereas the upper boundary is obtained for 5\%. These errors include
+the (uncorrelated) normalization uncertainties on the signal as well
+as on the background, where the crucial uncertainty is the error on
+the background. We find that the \BB\ is basically not affected by
+these errors, since the background has a rather different spectral
+shape (strongly peaked at low energies) than the signal. The fact
+that T2HK is relatively strongly affected by the actual value of the
+systematics can by understood by considering the ratio of signal to
+the square-root of the background using the numbers of
+Tab.~\ref{tab:events}. We shall discuss this issue in more detail in
+the next section in the context of the CP violation discovery reach.
+
+\begin{figure}
+  \centering \includegraphics[width=0.9\textwidth]{./fig10.eps}
+  \mycaption{\label{fig:SPLTheta13Disco} $3\sigma$ discovery
+  sensitivity to $\stheta$ for the SPL as a function of the true value
+  of \delCP\ for $\sin^2\theta_{23}^\mathrm{true} = 0.6$ and true
+  values for the other parameters as given in
+  Eq.~(\ref{eq:default-params}). The running time is ($2\nu +
+  8\bar\nu$)~yrs.
+}
+\end{figure}
+
+Let us remark that the $\theta_{13}$ sensitivities are practically not
+affected by the sign($\Delta m^2_{31}$)-degeneracy. This is easy to
+understand, since the data is fitted with $\theta_{13} = 0$, and in
+this case both mass hierarchies lead to very similar event rates. If
+the inverted hierarchy is used as the true hierarchy, the peak in the
+discovery limit visible in the left panel of Fig.~\ref{fig:th13}
+around $\delCP \sim \pi$ moves to $\delCP \sim 0$. However, the
+characteristic shape of the curves, and in particular, the sensitivity
+as a function of the \delCP-fraction shown in the right panel are
+hardly affected by the sign of the true $\Delta m^2_{31}$.
+%
+In case of a non-maximal value of $\theta_{23}$ the octant-degeneracy
+has a minor impact on the $\theta_{13}$ discovery potential, as
+illustrated in Fig.~\ref{fig:SPLTheta13Disco} for the SPL. We show the
+discovery limit obtained with the true and the fake octant of
+$\theta_{23}$ for a true value of $\sin^2\theta_{23}= 0.6$. Let us
+note that for true values of $\sin^2\theta_{23} > 0.5$ the
+octant-degenerate solution leads to a worse sensitivity to
+$\theta_{13}$ (see figure), whereas for $\sin^2\theta_{23} < 0.5$ the
+fake solution does not affect the $\theta_{13}$ discovery, since in
+this case the sensitivity is increased.
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{Sensitivity to CP violation}
+\label{sec:CPV}
+
+In case a finite value of $\theta_{13}$ is established it is important
+to quantitatively assess the discovery potential for leptonic CP
+violation (CPV). The CP symmetry is violated if the complex phase
+\delCP\ is different from $0$ and $\pi$. Therefore, CPV is discovered
+if these values for \delCP\ can be excluded. 
+%
+We evaluate the discovery potential for CPV in the following way:
+Data are calculated by scanning the true values of $\stheta$ and
+$\delCP$. Then these data are fitted with the CP conserving values
+$\delCP = 0$ and $\delCP = \pi$, where all parameters except \delCP\
+are varied and the sign and octant degeneracies are taken into
+account. If no fit with $\Delta \chi^2 < 9$ is found CP conserving
+values of \delCP\ can be excluded at $3\sigma$ for the chosen values
+of $\delta_\mathrm{CP}^\mathrm{true}$ and $\stheta^\mathrm{true}$.
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.65\textwidth]{./fig11.eps}
+%   
+   \mycaption{CPV discovery potential for \BB, SPL, and T2HK: For
+   parameter values inside the ellipse-shaped curves CP conserving
+   values of \delCP\ can be excluded at $3\sigma$ $(\Delta\chi^2>9)$.
+   The running time is ($5\nu + 5\bar\nu$)~yrs for \BB\ and ($2\nu +
+   8\bar\nu$)~yrs for the Super Beams. The width of the bands
+   corresponds to values for the systematical errors from 2\% to
+   5\%. The dashed curves show the sensitivity of the \BB\ when the
+   number of ion decays/yr are reduced by a factor of two with respect
+   to the values given in Tab.~\ref{tab:setups} for 2\%
+   systematics.\label{fig:CPV}}
+\end{figure}
+
+The CPV discovery potential for \BB, SPL, and T2HK is shown in
+Fig.~\ref{fig:CPV}. As in the case of the $\theta_{13}$ sensitivity we
+find that SPL and T2HK perform rather similar, whereas the \BB\ has
+significantly better sensitivity if our adopted numbers of ion decays
+per year can be achieved. For systematical errors of 2\% maximal CPV
+(for $\delCP^\mathrm{true} = \pi/2, \, 3\pi/2$) can be discovered at
+$3\sigma$ down to $\stheta \simeq 8.8 \,(6.6)\times 10^{-4}$ for SPL
+(T2HK), and $\stheta \simeq 2\times 10^{-4}$ for the \BB. This number
+for the \BB\ is increased by a factor 3 if the fluxes are reduced to
+half of our nominal values.  The best sensitivity to CPV is obtained
+for all three facilities around $\stheta \sim 10^{-2}$. For this value
+CPV can be established for 78\%, 73\%, 75\% of all values of \delCP\
+for \BB, SPL, T2HK, respectively (again for systematics of 2\%).
+
+The widths of the bands in Fig.~\ref{fig:CPV} corresponds to different
+values for systematical errors. The curves which give the best
+sensitivities are obtained for systematics of 2\%, the curves
+corresponding to the worst sensitivity have been computed for
+systematics of 5\%. We change the uncertainty on the signal as well as
+on the background, however, it turns out that the most relevant
+uncertainty is the background normalization. We find that the impact
+of systematics is very small for the \BB. The reason for this is that
+the spectral shape of the background in the \BB\ (from pions and
+atmospheric neutrinos) is very different from the signal, and
+therefore they can be disentangled by the fit of the energy spectrum.
+For the Super Beams the background spectrum is more similar to the
+signal, and therefore an uncertainty on the background normalization
+might have a strong impact on the sensitivity, as visible from the SPL
+and T2HK curves in Fig.~\ref{fig:CPV}. In particular T2HK is strongly
+affected, and moving from 2\% to 5\% uncertainy decreases the
+sensitivity to maximal CPV by a factor 3.
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.9\textwidth]{./fig12.eps}
+%   
+   \mycaption{Impact of total exposure and systematical errors on the
+   CPV discovery potential of \BB, SPL, and T2HK. We show the
+   smallest true value of $\stheta$ for which $\delCP = \pi/2$ can be
+   distinguished from $\delCP = 0$ or $\delCP = \pi$ at $3\sigma$
+   $(\Delta\chi^2>9)$ as a function of the exposure in kt~yrs (left)
+   and as a function of the systematical error on the background
+   $\sigma_\mathrm{bkgr}$ (right). The widths of the curves in the
+   left panel corresponds to values of $\sigma_\mathrm{bkgr}$ from 2\%
+   to 5\%. The thin solid curves in the left panel corresponds to no
+   systematical errors. The right plot is calculated for the standard
+   exposure of 4400~kt~yrs. No systematical error on the signal has
+   been assumed. \label{fig:systematics}}
+\end{figure}
+
+This interesting feature can be understood in the following way. A
+rough measure to estimate the sensitivity is given by the signal
+compared to the error on the background. The latter receives
+contributions from the statistical error $\sqrt{B}$ and from the
+systematical uncertainty $\sigma_\mathrm{bkgr}B$, where $B$ is the
+number of background events and $\sigma_\mathrm{bkgr}$ is the
+(relative) systematical error. Hence the importance of the systematics
+can be estimated by the ratio of systematical and statistical errors
+$\sigma_\mathrm{bkgr} B / \sqrt{B} = \sigma_\mathrm{bkgr} \sqrt{B}$.
+Summing the numbers for background events in the neutrino and
+antineutrino channels given in Tab.~\ref{tab:events} one finds that
+systematical errors dominate ($\sigma_\mathrm{bkgr} \sqrt{B} > 1$) if
+$\sigma_\mathrm{bkgr} \gtrsim 6\%,\, 3\%, \, 2\%$ for \BB, SPL, T2HK,
+respectively. 
+%
+In the right panel Fig.~\ref{fig:systematics} we show the sensitivity
+to maximal CPV (as defined in the figure caption) as a function of
+$\sigma_\mathrm{bkgr}$. Indeed, the worsening of the sensitivity due
+to systematics occurs roughly at the values of $\sigma_\mathrm{bkgr}$
+as estimated above. For a more quantitative understanding of these
+curves it is necessary to consider the number of signal and background
+events for neutrinos and antineutrinos separately, as well as to take
+into account spectral information.
+
+
+The left panel of Fig.~\ref{fig:systematics} shows the sensitivity to
+maximal CPV as a function of the exposure\footnote{Note that the CPV
+sensitivity for the \BB\ with reduced fluxes from Fig.~\ref{fig:CPV}
+is worse than the value which follows from Fig.~\ref{fig:systematics}.
+The reason is that in Fig.~\ref{fig:systematics} the total exposure is
+scaled (mass~$\times$~time), i.e., signal and background are scaled in
+the same way, whereas for the dashed curve in Fig.~\ref{fig:CPV} only
+the fluxes are reduced but backgrounds are kept constant.} for values
+of $\sigma_\mathrm{bkgr}$ from 2\% to 5\%. One can observe clearly
+that for the standard exposure of 4400~kt~yrs T2HK is dominated by
+systematics and changing $\sigma_\mathrm{bkgr}$ from 2\% to 5\% has a
+big impact on the sensitivity. In contrast the CERN--MEMPHYS
+experiments (especially the \BB) are rather stable with respect to
+systematics and for the standard exposure they are still statistics
+dominated. We conclude that in T2HK systematics have to be under very
+good control, whereas this issue is less important for \BB\ and SPL.
+%
+We have checked explicitly that the systematical error on the signal
+has negligible impact on these results. Therefore, we have set this
+error to zero for calculating Fig.~\ref{fig:systematics} to highlight
+the importance of the background error. In all other calculations also
+the signal error is included, in particular also in Fig.~\ref{fig:CPV}.
+
+Let us remark that for the T2KK configuration (with one half of the
+Hyper-K detector mass at Kamioka and the second half at the same
+off-axis angle in Korea) the problem of systematics might be less
+severe than for T2HK, since both detectors observe the same flux and
+background. 
+%
+Note however, that an important issue for the CPV sensitivity is
+whether systematics between neutrino and antineutrino data are
+correlated or not. We have checked that the worse sensitivies for T2HK
+shown in Fig.~\ref{fig:CPV} compared to the results obtained in
+Refs.~\cite{Ishitsuka:2005qi,Kajita:2006bt} can be traced back to the
+fact that in these papers neutrino and antineutrino systematics are
+correlated, whereas we consider them to be independent. Note that our
+approach is conservative, and the assumption of uncorrelated errors
+has been adopted also for the CERN--MEMPHYS experiments.
+
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.8\textwidth]{./fig13.eps}
+%   
+   \mycaption{Impact of degeneracies on the CPV discovery potential
+   for the \BB. We show the sensitivity to CPV at $3\sigma$
+   $(\Delta\chi^2>9)$ computed for 4 different combinations of the
+   true values of the hierarchy (NH or IH) and $\theta_{23}$
+   ($\sin^2\theta_{23} = 0.4$ or $0.6$). Dashed curves are computed
+   neglecting degeneracies in the fit. The running time is ($5\nu +
+   5\bar\nu$)~yrs.
+\label{fig:deltacp}}
+\end{figure}
+
+Finally, in Fig.~\ref{fig:deltacp} we illustrate the impact of
+degeneracies, as well as the true hierarchy and \thetatt-octant on the
+CPV sensitivity.  Curves of different colors correspond to the four
+different choices for \sigdm\ and the \thetatt-octant of the true
+parameters. For the solid curves the simulated data for each choice of
+true \sigdm\ and \thetatt-octant are fitted by taking into account all
+four degenerate solutions, i.e., also for the fit all four
+combinations of \sigdm\ and \thetatt-octant are used. One observes
+from the figure that the true hierarchy and octant have a rather small
+impact on the \BB\ CPV sensitivity, in particular the sensitivity to
+maximal CPV is completely independent.  The main effect of changing the
+true hierarchy is to exchange the behavior between $0 < \delCP <
+180^\circ$ and $180^\circ < \delCP < 360^\circ$. For $\stheta \lesssim
+10^{-2}$ the sensitivity gets slightly worse if
+$\thetatt^\mathrm{true} > \pi/4$ compared to $\thetatt^\mathrm{true} <
+\pi/4$.
+
+The dashed curves in Fig.~\ref{fig:deltacp} are computed without
+taking into account the degeneracies, i.e., for each choice of true
+\sigdm\ and \thetatt-octant the data are fitted only with this
+particular choice. The effect of the degeneracies becomes visible for
+large values of \thetaot. Note that this is just the region where they
+can be reduced by a combined analysis with atmospheric neutrinos (see
+Sec.~\ref{sec:atmospherics} or Ref.~\cite{Huber:2005ep}).
+ 
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Synergies provided by the CERN--MEMPHYS facilities}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:synergies}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{Combining Beta Beam and Super Beam}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:synergies-beams}
+
+In this section we discuss synergies which emerge if both \BB\ and SPL
+are available. The main difference between these two beams is the
+different initial neutrino flavor,
+$\stackrel{\scriptscriptstyle(-)}{\nu}_e$ for \BB\ and
+$\stackrel{\scriptscriptstyle (-)}{\nu}_\mu$ for SPL. This implies
+that at near detectors all relevant cross sections can be measured. In
+particular, the near detector of the \BB\ will measure the cross
+section for the SPL appearance search, and vice versa.
+%
+If both experiments run with neutrinos and antineutrinos all possible
+transition probabilities are covered: $P_{\nu_e\to\nu_\mu}$,
+$P_{\bar\nu_e\to\bar\nu_\mu}$, $P_{\nu_\mu\to\nu_e}$, and
+$P_{\bar\nu_\mu\to\bar\nu_e}$. Together with the fact that matter
+effects are very small because of the relatively short baseline, this
+means that in addition to CP also direct tests of the T and CPT
+symmetries are possible.
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.9\textwidth]{./fig14.eps}
+%   
+   \mycaption{Discovery potential of a finite value of $\stheta$ at
+   $3\sigma$ $(\Delta\chi^2>9)$ for 5~yrs neutrino data from
+   \BB, SPL, and the combination of \BB\ + SPL compared to
+   10~yrs data from T2HK (2~yrs neutrinos + 8~yrs antineutrinos).
+   \label{fig:th13-5yrs}}
+\end{figure}
+
+However, if the CPT symmetry is assumed in principle all information
+can be obtained just from neutrino data because of the relations
+$P_{\bar\nu_e\to\bar\nu_\mu} = P_{\nu_\mu\to\nu_e}$ and
+$P_{\bar\nu_\mu\to\bar\nu_e} = P_{\nu_e\to\nu_\mu}$. As mentioned
+already in Sec.~\ref{sec:degeneracies} this implies that (time
+consuming) antineutrino running can be avoided. We illustrate this
+synergy in Figs.~\ref{fig:th13-5yrs} and \ref{fig:CP-5yrs}. In
+Fig.~\ref{fig:th13-5yrs} we show the $\theta_{13}$ discovery potential
+of 5 years of neutrino data from \BB\ and SPL. From the left panel the
+complementarity of the two experiments is obvious, since each of them
+is most sensitive in a different region of \delCP. (As expected from
+general properties of the oscillation probabilities the sensitivity
+curves of \BB\ and SPL are approximately related by the transformation
+$\delCP \to 2\pi - \delCP$.) Combining these two data sets results in
+a sensitivity slightly better than from 10 years (2$\nu$+8$\bar\nu$)
+of T2HK data.
+%
+As visible in Fig.~\ref{fig:CP-5yrs} also for the CPV discovery this
+synergy works and 5 years of neutrino data from \BB\ and SPL lead to a
+similar sensitivity as 10 years of T2HK.
+
+\begin{figure}[!t]
+  \centering
+   \includegraphics[width=0.6\textwidth]{./fig15.eps}
+%   
+   \mycaption{Sensitivity to CPV at $3\sigma$ $(\Delta\chi^2>9)$ for
+   combining 5~yrs neutrino data from \BB\ and SPL compared to
+   10~yrs data from T2HK (2~yrs neutrinos + 8~yrs antineutrinos).
+   \label{fig:CP-5yrs}}
+\end{figure}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\subsection{Resolving degeneracies with atmospheric neutrinos}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:atmospherics}
+
+It was pointed out in Ref.~\cite{Huber:2005ep} that for LBL
+experiments based on mega ton scale water \v{C}erenkov detectors data
+from atmospheric neutrinos (ATM) provide an attractive method to
+resolve degeneracies. Atmospheric neutrinos are sensitive to the
+neutrino mass hierarchy if $\theta_{13}$ is sufficiently large due to
+Earth matter effects, mainly in multi-GeV $e$-like
+events~\cite{Petcov:1998su,Akhmedov:1998ui,Bernabeu:2003yp}. Moreover,
+sub-GeV $e$-like events provide sensitivity to the octant of
+$\theta_{23}$~\cite{Kim:1998bv,Peres:2003wd,Gonzalez-Garcia:2004cu}
+due to oscillations with $\Delta m^2_{21}$ (see also
+Ref.~\cite{Kajita} for a discussion of atmospheric neutrinos in the
+context of Hyper-K). 
+%
+Following Ref.~\cite{Huber:2005ep} we investigate here the synergy
+from a combination of LBL data from \BB\ and SPL with ATM data in the
+MEMPHYS detector. Technical details are given in
+Sec.~\ref{sec:atm-details}. 
+ 
+The effect of degeneracies in LBL data has been discussed in
+Sec.~\ref{sec:degeneracies}, see Figs.~\ref{fig:degeneracies} and
+\ref{fig:degeneracies_SPL}. As discussed there, for given true
+parameter values the data can be fitted with the wrong hierarchy
+and/or with the wrong octant of $\theta_{23}$. Hence, from LBL data
+alone the hierarchy and the octant cannot be determined and
+ambiguities exist in the determination of $\theta_{13}$ and
+$\delta_\mathrm{CP}$.
+%
+If the LBL data are combined with ATM data only the colored regions in
+Fig.~\ref{fig:degeneracies} survive, i.e., in this particular example
+for SPL and T2HK the degeneracies are completely lifted at 95\%~CL,
+the mass hierarchy and the octant of $\theta_{23}$ can be identified,
+and the ambiguities in $\theta_{13}$ and $\delta_\mathrm{CP}$ are
+resolved. For the \BB\ an island corresponding to the wrong hierarchy
+does survive at the 95\%~CL for 2~dof. Still, the solution with the
+wrong sign of $\Delta m^2_{31}$ is disfavored with $\Delta\chi^2 =
+5.1$ with respect to the true solution, which corresponds to
+2.4$\sigma$ for 1~dof.
+%
+Let us note that in Fig.~\ref{fig:degeneracies} we have chosen a
+favorable value of $\sin^2\theta_{23} = 0.6$; for values
+$\sin^2\theta_{23} < 0.5$ in general the sensitivity of ATM data is
+weaker~\cite{Huber:2005ep}.
+
+\begin{figure}[!t]
+\centering
+  \includegraphics[width=0.9\textwidth]{./fig16.eps}
+%
+  \mycaption{Sensitivity to the mass hierarchy at $2\sigma$
+  $(\Delta\chi^2 = 4)$ as a function of the true values of
+  $\sin^22\theta_{13}$ and $\delta_\mathrm{CP}$ (left), and the
+  fraction of true values of $\delCP$ (right). The solid curves are
+  the sensitivities from the combination of long-baseline and
+  atmospheric neutrino data, the dashed curves correspond to
+  long-baseline data only. The running time is ($5\nu + 5\bar\nu$)~yrs
+  for \BB\ and ($2\nu + 8\bar\nu$)~yrs for the Super Beams. For
+  comparison we show in the right panel also the sensitivities of
+  NO$\nu$A and NO$\nu$A+T2K extracted from Fig.~13.14 of
+  Ref.~\cite{Ayres:2004js}. For the curve labeled ``NO$\nu$A
+  (p.dr.)+T2K@4~MW'' a proton driver has been assumed for NO$\nu$A and
+  the T2K beam has been up-graded to 4~MW, see
+  Ref.~\cite{Ayres:2004js} for details.}
+  \label{fig:hierarchy}
+\end{figure}
+
+In Fig.~\ref{fig:hierarchy} we show how the combination of ATM+LBL
+data leads to a non-trivial sensitivity to the neutrino mass
+hierarchy, i.e.\ to the sign of $\Delta m^2_{31}$. For LBL data alone
+(dashed curves) there is practically no sensitivity for the
+CERN--MEMPHYS experiments (because of the very small matter effects
+due to the relatively short baseline), and the sensitivity of T2HK
+depends strongly on the true value of $\delta_\mathrm{CP}$. However,
+by including data from atmospheric neutrinos (solid curves) the mass
+hierarchy can be identified at $2\sigma$~CL provided
+$\sin^22\theta_{13} \gtrsim 0.02-0.03$. As an example we have chosen
+in that figure a true value of $\theta_{23} = \pi/4$. Generically the
+hierarchy sensitivity increases with increasing $\theta_{23}$, see
+Ref.~\cite{Huber:2005ep} for a detailed discussion.
+
+The sensitivity to the neutrino mass hierarchy shown in
+Fig.~\ref{fig:hierarchy} is significantly improved with respect to our
+previous results obtained in Ref.~\cite{Huber:2005ep}. There are two
+main reasons for this improved performance: First, we use now much
+more bins in charged lepton energy for fully contained single-ring
+events\footnote{The impact of energy binning on the hierarchy
+determination with atmospheric neutrinos has been discussed recently
+in Ref.~\cite{Petcov:2005rv} in the context of magnetized iron
+detectors.}  (compare Sec.~\ref{sec:atm-details}), and second, we
+implemented also information from multi-ring events. This latter point
+is important since the relative contribution of neutrinos and
+antineutrinos is different for single- and multi-ring
+events. Therefore, combining single- and multi-ring data allows to
+obtain a discrimination between neutrino and antineutrino events on a
+statistical basis. This in turn contains crucial information on the
+hierarchy, since the matter enhancement is visible either in neutrinos
+or antineutrinos, depending on the hierarchy.
+
+Although \BB\ and SPL alone have no sensitivity to the hierarchy at
+all, we find that the combination of them does provide rather good
+sensitivity even without atmospheric data. The reason for this
+interesting effect is the following. Because of the rather short
+baseline the matter effect is too small to distinguish between NH and
+IH given only neutrino and antineutrino information in one channel.
+However, the tiny matter effect suffices to move the hierarchy
+degenerate solution to slightly different locations in the ($\stheta$,
+$\delCP$) plane for the $\stackrel{\scriptscriptstyle(-)}{\nu}_e \to
+\stackrel{\scriptscriptstyle (-)}{\nu}_\mu$ (\BB) and
+$\stackrel{\scriptscriptstyle(-)}{\nu}_\mu \to
+\stackrel{\scriptscriptstyle (-)}{\nu}_e$ (SPL) channels (compare
+Fig.~\ref{fig:degeneracies}). Hence, if all four CP and T conjugate
+channels are available (as it is the case for the \BB+SPL combination)
+already the small matter effect picked up along the 130~km
+CERN--MEMPHYS distance provides sensitivity to the mass hierarchy for
+$\sin^22\theta_{13} \gtrsim 0.03$, or $\sin^22\theta_{13} \gtrsim 0.015$
+if also atmospheric neutrino data is included.
+
+For comparison we show in the right panel of Fig.~\ref{fig:hierarchy}
+also the sensitivity of the NO$\nu$A~\cite{Ayres:2004js} experiment,
+and of NO$\nu$A+T2K, where in the second case a beam upgrade by a
+proton driver has been assumed for NO$\nu$A, and for T2K the
+Super-Kamiokande detector has been used but the beam intensity has
+been increased by assuming 4~MW power. More details on these
+sensitivities can be found in Ref.~\cite{Ayres:2004js}.
+%
+Let us note that in general LBL experiments with two detectors and/or
+very long baselines ($\gtrsim 1000$~km) are a competitive method to
+atmospheric neutrinos for the hierarchy determination, see, e.g.,
+Refs.~\cite{Ishitsuka:2005qi,Kajita:2006bt,MenaRequejo:2005hn,Hagiwara:2005pe,Barger:2006vy}
+for recent analyses. In particular, in case of the T2KK extension of
+the T2HK experiment, the very long baseline to Korea allows for a
+determination of the mass hierarchy down to $\sin^22\theta_{13}
+\gtrsim 0.02$ ($2\sigma$) without using atmospheric
+neutrinos~\cite{Kajita:2006bt}.
+%
+We mention also the possibility to determine the neutrino mass
+hierarchy by using neutrino events from a galactic Super Nova
+explosion in mega ton \v{C}erenkov detectors such as MEMPHYS, see,
+e.g., Ref.~\cite{Kachelriess:2004vs}.
+
+\begin{figure}[!t]
+\centering
+  \includegraphics[width=0.55\textwidth]{./fig17.eps}
+%
+  \mycaption{$\Delta\chi^2$ of the solution with the wrong octant of
+  $\theta_{23}$ as a function of the true value of
+  $\sin^2\theta_{23}$. We have assumed a true value of $\theta_{13} =
+  0$, and the running time is ($2\nu + 8\bar\nu$)~yrs.}
+  \label{fig:octant}
+\end{figure}
+
+Fig.~\ref{fig:octant} shows the potential of ATM+LBL data to exclude
+the octant degenerate solution. Since this effect is based mainly on
+oscillations with $\Delta m^2_{21}$ there is very good sensitivity
+even for $\theta_{13} = 0$; a finite value of $\theta_{13}$ in general
+improves the sensitivity~\cite{Huber:2005ep}.  From the figure one can
+read off that atmospheric data alone can can resolve the correct
+octant at $3\sigma$ if $|\sin^2\theta_{23} - 0.5| \gtrsim 0.085$. If
+atmospheric data is combined with the LBL data from SPL or T2HK there
+is sensitivity to the octant for $|\sin^2\theta_{23} - 0.5| \gtrsim
+0.05$. The improvement of the octant sensitivity with respect to
+previous analyses~\cite{Huber:2005ep,Gonzalez-Garcia:2004cu} follows
+from changes in the analysis of sub-GeV atmospheric events, where now
+three bins in lepton momentum are used instead of one. Note that since
+in Fig.~\ref{fig:octant} we have assumed a true value of $\theta_{13}
+= 0$, combining the \BB\ with ATM does not improve the sensitivity
+with respect to atmospheric data alone. 
+%
+We note that the T2KK configuration provides also some sensitivity to
+the octant of $\theta_{23}$ without referring to atmospheric
+neutrinos. In Ref.~\cite{Kajita:2006bt} it was found that for
+$|\sin^2\theta_{23} - 0.5| \gtrsim 0.12$ the octant can be identified
+in T2KK at $3\sigma$.
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\section{Summary}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\label{sec:conclusions}
+
+In this work we have studied the physics potential of the
+CERN--MEMPHYS neutrino oscillation project. We consider a Beta Beam
+(\BB) with $\gamma = 100$ for the stored ions, where existing
+facilities at CERN can be used optimally, and a Super Beam based on an
+optimized Super Proton Linac (SPL) with a beam energy of 3.5~GeV and
+4~MW power. As target we assume the MEMPHYS detector, a 440~kt water
+\v{C}erenkov detector at Fr\'ejus, at a distance of 130~km from
+CERN. The main characteristics of the experiments are summarized in
+Tab.~\ref{tab:setups}.
+%
+The adopted neutrino fluxes are based on realistic calculations of ion
+production and storage for the \BB, and a full simulation of the beam
+line (particle production and decay of secondaries) for SPL. Special
+care has be given to the issue of backgrounds, which we include by
+means of detailed event simulations and applying Super-Kamiokande particle
+identification algorithms.
+
+The physics potential of the \BB\ and SPL experiments in terms of
+$\theta_{13}$ discovery reach and sensitivity to CP violation has been
+addressed where parameter degeneracies are fully taken into account.
+The main results on these performance indicators are summarized in
+Figs.~\ref{fig:th13} and \ref{fig:CPV}.
+%
+We obtain a guaranteed discovery reach of $\stheta \simeq 5\times
+10^{-3}$ at $3\sigma$, irrespective of the actual value of \delCP. For
+certain values of \delCP\ the sensitivity is significantly improved,
+and for \BB\ (SPL) discovery limits around $\stheta \simeq 3\,(10)
+\times 10^{-4}$ are possible for a large fraction of all possible
+values of \delCP.
+%
+Maximal CP violation (for $\delCP^\mathrm{true} = \pi/2, \, 3\pi/2$)
+can be discovered at $3\sigma$ down to $\stheta \simeq 2\, (9)\times
+10^{-4}$ for \BB\ (SPL), whereas the best sensitivity to CP violation
+is obtained for $\stheta \sim 10^{-2}$: For $\stheta = 10^{-2}$ CP
+violation can be established at $3\sigma$ for 78\% (73\%) of all
+possible true values of \delCP\ for \BB\ (SPL).
+%
+We stress that the \BB\ performance in general depends crucially on
+the number of ion decays per year.
+%
+The impact of the value of systematical uncertainties on signal and
+background on our results is discussed.
+%
+The \BB\ and SPL sensitivities are compared to the ones of the
+phase~II of the T2K experiment in Japan (T2HK), which is a competing
+proposal of similar size and timescale. In general we obtain rather
+similar sensitivities for T2HK and SPL, and hence the CERN--MEMPHYS
+experiments provide a viable alternative to T2HK. We find that \BB\
+and SPL are less sensitive to systematical errors, whereas the
+sensitivity of T2HK crucially depends on the systematical error on the
+background.\footnote{Let us note that in the present study we have not
+considered the recent ``T2KK'' proposal~\cite{Ishitsuka:2005qi}, where
+one half of the Hyper-K detector mass is at Kamioka and the second
+half in Korea. For such a setup our results do not apply and
+especially the conclusion on systematical errors may be different.}
+
+Assuming that both \BB\ and SPL experiments are available, we point
+out that one can benefit from the different oscillation channels
+$\nu_e\to\nu_\mu$ for \BB\ and $\nu_\mu\to\nu_e$ for SPL, since by the
+combination of these channels the time intensive antineutrino
+measurements can be avoided. We show that 5 years of neutrino data from
+\BB\ and SPL lead to similar results as 2 years of neutrino plus 8
+years of antineutrino data from T2HK.
+%
+Furthermore, we discuss the use of atmospheric neutrinos in the
+MEMPHYS detector to resolve parameter degeneracies in the
+long-baseline data. This effect leads to a sensitivity to the neutrino
+mass hierarchy at $2\sigma$~CL for $\sin^22\theta_{13} \gtrsim
+0.025$ for \BB\ and SPL, although these experiments alone (without
+atmospheric data) have no sensitivity at all. The optimal hierarchy
+sensitivity is obtained from combining \BB+SPL+atmospheric data.
+Furthermore, the combination of atmospheric data with a Super Beam
+provides a possibility to determine the octant of $\theta_{23}$.
+
+To conclude, we have shown that the CERN--MEMPHYS neutrino oscillation
+project based on a Beta Beam and/or a Super Beam plus a mega ton scale
+water \v{C}erenkov detector offers interesting and competitive physics
+possibilities and is worth to be considered as a serious option in
+the worldwide process of identifying future high precision neutrino
+oscillation facilities~\cite{ISSpage}.
+
+\subsection*{Acknowledgment}
+
+We thank J.~Argyriades for communication on the Super-K atmospheric
+neutrino analysis, A.~Cazes for his work on the SPL simulation, and
+P.~Huber for his patience in answering questions concerning the use of
+GLoBES. Furthermore, we thank D.~Casper for the help in installing and
+running Nuance, and E.~Couce for discussions about the \BB\
+backgrounds.  T.S.\ is supported by the $6^\mathrm{th}$~Framework
+Program of the European Community under a Marie Curie Intra-European
+Fellowship.
+
+
+%\newpage
+\begin{thebibliography}{99}
+
+\bibitem{solar}
+  B.~T.~Cleveland {\it et al.},
+  Astrophys.\ J.\  {\bf 496} (1998) 505;
+  %%CITATION = ASJOA,496,505;%%
+%
+  J.N.~Abdurashitov {\it et al.}  [SAGE],
+  J.\ Exp.\ Theor.\ Phys.\  {\bf 95} (2002) 181
+  % [Zh.\ Eksp.\ Teor.\ Fiz.\  {\bf 122} (2002) 211].
+  [astro-ph/0204245];
+  %%CITATION = ASTRO-PH 0204245;%%
+%
+  T. Kirsten {\it et al.} [GALLEX and GNO], 
+  Nucl. Phys. B (Proc. Suppl.)  {\bf 118} (2003) 33;
+%
+  S.~Fukuda {\it et al.} [Super-Kamiokande],
+  %``Determination of solar neutrino 
+  % oscillation parameters using 1496 days  of Super-Kamiokande-I data,''
+  Phys. Lett. {\bf B539} (2002) 179;
+%
+%\bibitem{ahmad:2002ka}
+  Q.R. Ahmad {\em et~al.} [SNO],
+  Phys. Rev. Lett. {\bf 89}, 011302 (2002) 
+  [nucl-ex/0204009];
+  %%CITATION = NUCL-EX 0204009;%%
+%
+%\bibitem{Aharmim:2005gt}
+  B.~Aharmim {\it et al.}  [SNO],
+  %``Electron energy spectra, fluxes, and day-night asymmetries of B-8 solar
+  %neutrinos from the 391-day salt phase SNO data set,''
+  Phys.\ Rev.\ C {\bf 72} (2005) 055502
+  [nucl-ex/0502021].
+  %%CITATION = NUCL-EX 0502021;%%
+
+\bibitem{Fukuda:1998mi}
+  Y.~Fukuda {\it et al.} [Super-Kamiokande Coll.],
+  %``Evidence for oscillation of atmospheric neutrinos,''
+  Phys.\ Rev.\ Lett.\  {\bf 81} (1998) 1562
+  [hep-ex/9807003].
+  %%CITATION = HEP-EX 9807003;%%
+
+\bibitem{Ashie:2005ik}
+  Super-Kamiokande Coll.,
+  Y.~Ashie {\it et al.},  %[Super-Kamiokande Collaboration],
+  %``A measurement of atmospheric neutrino oscillation parameters by
+  %Super-Kamiokande I,''
+  Phys.\ Rev.\ D {\bf 71}, 112005 (2005)
+  [hep-ex/0501064];
+  %%CITATION = HEP-EX 0501064;%%
+%
+%\bibitem{Hosaka:2006zd}
+  J.~Hosaka {\it et al.},% [Super-Kamiokande Collaboration],
+  %``Three flavor neutrino oscillation analysis of atmospheric neutrinos in
+  %Super-Kamiokande,''
+  Phys.\ Rev.\ D {\bf 74}, 032002 (2006)
+  [hep-ex/0604011].
+  %%CITATION = HEP-EX 0604011;%%
+
+
+\bibitem{Araki:2004mb}
+  T.~Araki {\it et al.} [KamLAND Coll.],
+  %``Measurement of neutrino oscillation with KamLAND: Evidence of spectral
+  %distortion,''
+  Phys.\ Rev.\ Lett.\  {\bf 94}, 081801 (2005)
+  [hep-ex/0406035].
+  %%CITATION = HEP-EX 0406035;%%
+
+
+\bibitem{Aliu:2004sq}
+  E.~Aliu {\it et al.}  [K2K Coll.],
+  %``Evidence for muon neutrino oscillation in an accelerator-based
+  %experiment,''
+  Phys.\ Rev.\ Lett.\  {\bf 94}, 081802 (2005)
+  [hep-ex/0411038].
+  %%CITATION = HEP-EX 0411038;%%
+
+\bibitem{MINOS} 
+  D.G.~Micheal {\it et al.} [MINOS Coll.],
+  %''Observation of muon neutrino disappearance with the {MINOS} detectors and
+  %the {NuMI} neutrino beam,''
+  hep-ex/0607088.
+
+\bibitem{OPERA}
+  D. Autiero [OPERA Coll.], 
+  Nucl.\ Phys.\ B (Proc. Suppl.) {\bf 143}, 257 (2005);
+  M. Guler  \etal, \textit{Experiment proposal}, 
+  CERN/SPSC 2000-028 SPSC/P318 LNGS P25/2000.
+
+\bibitem{CNGS}
+  G. Acquistapace \etal, CERN-98-02.
+
+\bibitem{LSND}
+  A. Athanassopoulos \etal, Phys.\ Rev.\ Lett.\ {\bf 81}, 1774  (1998);
+  A. Aguilar \etal, Phys.\ Rev.\ D {\bf 64}, 112007 (2001).
+
+\bibitem{MINIBOONE}
+  I. Stancu \etal, FERMILAB-TM-2207.
+
+\bibitem{FOGLILISI05}
+  G.~L.~Fogli, E.~Lisi, A.~Marrone and A.~Palazzo,
+  %``Global analysis of three-flavor neutrino masses and mixings,''
+  Prog.\ Part.\ Nucl.\ Phys.\  {\bf 57}, 742 (2006)
+  [hep-ph/0506083].
+  %%CITATION = HEP-PH 0506083;%%
+
+\bibitem{Maltoni:2004ei}
+  M.~Maltoni, T.~Schwetz, M.~A.~Tortola and J.~W.~F.~Valle,
+  %``Status of global fits to neutrino oscillations,''
+  New J.\ Phys.\  {\bf 6}, 122 (2004)
+  [hep-ph/0405172];
+  %%CITATION = HEP-PH 0405172;%%
+%
+%\bibitem{Schwetz:2005jr}
+  T.~Schwetz,
+  %``Neutrino oscillations: Current status and prospects,''
+  Acta Phys.\ Polon.\ B {\bf 36}, 3203 (2005)
+  [hep-ph/0510331].
+  %%CITATION = HEP-PH 0510331;%%
+
+\bibitem{PMNS}
+  B.~Pontecorvo, Sov.\ Phys.--JETP {\bf 6}, 429 (1957) 
+  [Zh.\ Eksp.\ Teor.\ Fiz.\ \textbf{33}, 549 (1957)];
+  Z.~Maki, M.~Nakagawa and S.~Sakata, 
+  Prog.\ Theor.\ Phys.\ \textbf{28}, 870 (1962);
+  B.~Pontecorvo, Sov.\ Phys.--JETP \textbf{26}, 984 (1968) 
+  [Zh. Eksp. Teor. Fiz. \textbf{53}, 1717 (1967)];
+  V.~N.~Gribov and B.~Pontecorvo, 
+  Phys.\ Lett.\ B \textbf{28}, 493 (1969). 
+
+\bibitem{CHOOZ}
+  Chooz Collaboration,
+  M. Apollonio \etal, Phys.\ Lett.\ B {\bf 466}, 415 (1999);
+%\bibitem{Apollonio:2002gd}
+  M.~Apollonio {\it et al.},
+  %``Search for neutrino oscillations on a long base-line at the CHOOZ  nuclear
+  %power station,''
+  Eur.\ Phys.\ J.\ C {\bf 27}, 331 (2003)
+  [hep-ex/0301017].
+  %%CITATION = HEP-EX 0301017;%%
+
+\bibitem{Wpaper}
+  K.~Anderson \etal, White paper report on using nuclear 
+  reactors to search for a value of $\theta_{13}$, 
+  hep-ex/0402041;
+%
+  F.~Ardellier \etal, Letter of intent for Double-Chooz, 
+  hep-ex/0405032.
+
+\bibitem{T2K}
+  Y.~Itow {\it et al.},
+  The JHF-Kamioka neutrino project,
+  hep-ex/0106019;
+  %%CITATION = HEP-EX 0106019;%%
+%
+%\bibitem{Kobayashi:2005hu}
+  T.~Kobayashi,
+  %``Super beams,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 143} (2005) 303.
+  %%CITATION = NUPHZ,143,303;%%
+
+\bibitem{Ayres:2004js}
+  D.~S.~Ayres {\it et al.} [NOvA Coll.],
+  %``NOvA proposal to build a 30-kiloton off-axis detector to study neutrino
+  %oscillations in the Fermilab NuMI beamline,''
+  hep-ex/0503053.
+  %%CITATION = HEP-EX 0503053;%%
+
+\bibitem{Huber:2003pm}
+  P.~Huber, M.~Lindner, T.~Schwetz and W.~Winter,
+  %``Reactor neutrino experiments compared to superbeams,''
+  Nucl.\ Phys.\ B {\bf 665} (2003) 487
+  [hep-ph/0303232];
+  %%CITATION = HEP-PH 0303232;%%
+%
+%\bibitem{Huber:2004ug}
+  P.~Huber, M.~Lindner, M.~Rolinec, T.~Schwetz and W.~Winter,
+  %``Prospects of accelerator and reactor neutrino oscillation experiments  for
+  %the coming ten years,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 073014
+  [hep-ph/0403068].
+  %%CITATION = HEP-PH 0403068;%%
+
+\bibitem{Albrow:2005kw}
+  M.~G.~Albrow {\it et al.},
+  Physics at a Fermilab proton driver,
+  hep-ex/0509019.
+  %%CITATION = HEP-EX 0509019;%%
+
+\bibitem{SPL}
+  M.~Baylac {\it et al.},
+  Conceptual design of the SPL II: A high-power superconducting H- linac
+  at CERN, CERN-2006-006.
+
+\bibitem{BNLHS}
+%\bibitem{Diwan:2003bp}
+  M.~V.~Diwan {\it et al.},
+  %``Very long baseline neutrino oscillation experiments for precise
+  %measurements of mixing parameters and CP violating effects,''
+  Phys.\ Rev.\ D {\bf 68} (2003) 012002
+  [hep-ph/0303081].
+  %%CITATION = HEP-PH 0303081;%%
+
+\bibitem{zucchelli}
+%\bibitem{Zucchelli:2002sa}
+  P.~Zucchelli,
+  %``A novel concept for a anti-nu/e / nu/e neutrino factory: The Beta Beam,''
+  Phys.\ Lett.\ B {\bf 532} (2002) 166.
+  %%CITATION = PHLTA,B532,166;%%
+
+\bibitem{Albright:2004iw}
+  C.~Albright {\it et al.}  [Neutrino Factory/Muon Collider Coll.],
+  %``The neutrino factory and Beta Beam experiments and development,''
+  physics/0411123.
+  %%CITATION = PHYS-ICS 0411123;%%
+
+\bibitem{Blondel:2004ae}
+  A.~Blondel {\it et al.},
+  ECFA/CERN studies of a European neutrino factory complex,
+  CERN-2004-002
+
+\bibitem{Campagne:2004wt}
+  J.~E.~Campagne and A.~Cazes,
+  %``The theta(13) and delta(CP) sensitivities of the SPL-Frejus project
+  %revisited,''
+  Eur.\ Phys.\ J.\ C {\bf 45} (2006) 643
+  [hep-ex/0411062].
+  %%CITATION = HEP-EX 0411062;%%
+
+\bibitem{Mezzetto:2003ub}
+  M.~Mezzetto,
+  %``Physics reach of the beta beam,''
+  J.\ Phys.\ G {\bf 29} (2003) 1771
+  [hep-ex/0302007];
+  %%CITATION = HEP-EX 0302007;%%
+%
+  J.~Bouchez, M.~Lindroos, M.~Mezzetto,
+  %``Beta Beams: Present design and expected performances,''
+  AIP Conf.\ Proc.\  {\bf 721} (2004) 37
+  [hep-ex/0310059].
+  %%CITATION = HEP-EX 0310059;%%
+
+\bibitem{memphys}
+  A.~de Bellefon {\it et al.}, 
+  MEMPHYS: A large scale water \v{C}erenkov detector
+  at Fr\'ejus, Contribution to the CERN strategic committee,
+  hep-ex/0607026,\\
+  \verb!http://apc-p7.org/APC_CS/Experiences/MEMPHYS/!
+
+\bibitem{UNO} 
+  C.~K.~Jung,
+  Feasibility of a next generation underground water Cherenkov detector:
+  UNO, hep-ex/0005046.
+  %%CITATION = HEP-EX 0005046;%%
+
+\bibitem{Nakamura:2003hk}
+  K.~Nakamura,
+  %``Hyper-Kamiokande: A next generation water Cherenkov detector,''
+  Int.\ J.\ Mod.\ Phys.\ A {\bf 18} (2003) 4053.
+  %%CITATION = IMPAE,A18,4053;%%
+
+\bibitem{Huber:2005ep}
+  P.~Huber, M.~Maltoni, T.~Schwetz,
+  %``Resolving parameter degeneracies in long-baseline experiments by
+  %atmospheric neutrino data,''
+  Phys.\ Rev.\ D {\bf 71} (2005) 053006
+  [hep-ph/0501037].
+  %%CITATION = HEP-PH 0501037;%%
+
+\bibitem{Globes}
+  P.~Huber, M.~Lindner and W.~Winter,
+  %``Simulation of long-baseline neutrino oscillation experiments with
+  %GLoBES,''
+  Comput.\ Phys.\ Commun.\  {\bf 167} (2005) 195
+  [hep-ph/0407333],
+  \verb!http://www.mpi-hd.mpg.de/lin/globes/!
+
+\bibitem{Huber:2002mx}
+  P.~Huber, M.~Lindner and W.~Winter,
+  %``Superbeams versus neutrino factories,''
+  Nucl.\ Phys.\ B {\bf 645} (2002) 3
+  [hep-ph/0204352].
+  %%CITATION = HEP-PH 0204352;%%
+
+\bibitem{Nuance}
+  NUANCE event generator (v3), 
+  \verb!http://nuint.ps.uci.edu/nuance/!,
+  D.~Casper,
+  %``The nuance neutrino physics simulation, and the future,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 112} (2002) 161
+  [hep-ph/0208030].
+
+
+% T2KK %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\bibitem{Ishitsuka:2005qi}
+  M.~Ishitsuka, T.~Kajita, H.~Minakata and H.~Nunokawa,
+  %``Resolving neutrino mass hierarchy and CP degeneracy by two identical
+  %detectors with different baselines,''
+  Phys.\ Rev.\ D {\bf 72} (2005) 033003
+  [hep-ph/0504026].
+  %%CITATION = HEP-PH 0504026;%%
+
+\bibitem{Kajita:2006bt}
+  T.~Kajita, H.~Minakata, S.~Nakayama and H.~Nunokawa,
+  %``Resolving eight-fold neutrino parameter degeneracy by two identical
+  %detectors with different baselines,''
+  Phys.\ Rev.\  D {\bf 75}, 013006 (2007)
+  [hep-ph/0609286].
+  %%CITATION = PHRVA,D75,013006;%%
+
+\bibitem{Hagiwara:2005pe}
+  K.~Hagiwara, N.~Okamura and K.~Senda,
+  %``Solving the neutrino parameter degeneracy by measuring the T2K off-axis
+  %beam in Korea,''
+  Phys.\ Lett.\ B {\bf 637}, 266 (2006)
+  [hep-ph/0504061].
+  %%CITATION = HEP-PH 0504061;%%
+
+
+% BB %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\bibitem{MyNufact04}
+  M.~Mezzetto,
+  %``SPL and Beta Beams to the Frejus,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 149} (2005) 179.
+
+\bibitem{Donini:2004hu}
+  A.~Donini, E.~Fernandez-Martinez, P.~Migliozzi, S.~Rigolin and L.~Scotto Lavina,
+  %``Study of the eightfold degeneracy with a standard beta-beam and a
+  %super-beam facility,''
+  Nucl.\ Phys.\ B {\bf 710}, 402 (2005)
+  [hep-ph/0406132].
+  %%CITATION = HEP-PH 0406132;%%
+
+\bibitem{JJHigh2} 
+%\bibitem{Burguet-Castell:2005pa}
+  J.~Burguet-Castell, D.~Casper, E.~Couce, J.~J.~Gomez-Cadenas and P.~Hernandez,
+  %``Optimal beta-beam at the CERN-SPS,''
+  Nucl.\ Phys.\ B {\bf 725} (2005) 306
+  [hep-ph/0503021].
+  %%CITATION = HEP-PH 0503021;%%
+
+\bibitem{LindnerBB}
+%\bibitem{Huber:2005jk}
+  P.~Huber, M.~Lindner, M.~Rolinec and W.~Winter,
+  %``Physics and optimization of beta-beams: From low to very high gamma,''
+  Phys.\ Rev.\ D {\bf 73}, 053002 (2006)
+  [hep-ph/0506237].
+  %%CITATION = HEP-PH 0506237;%%
+
+\bibitem{JJHigh1}
+ J.~Burguet-Castell, D.~Casper, J.~J.~Gomez-Cadenas, P.~Hernandez and F.~Sanchez,
+ Nucl.\ Phys.\ B {\bf 695} (2004) 217
+ [hep-ph/0312068].
+
+\bibitem{Terranova}
+  F.~Terranova, A.~Marotta, P.~Migliozzi and M.~Spinetti,
+  %``High energy beta beams without massive detectors,''
+  Eur.\ Phys.\ J.\ C {\bf 38}, 69 (2004)
+  [hep-ph/0405081].
+  %%CITATION = HEP-PH 0405081;%%
+
+\bibitem{BB-Reviews}
+  M.~Mezzetto, %``Beta Beams,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 143} (2005) 309
+  [hep-ex/0410083];
+%
+  C.~Volpe,
+  %``Topical review on 'beta-beams',''
+  hep-ph/0605033.
+
+\bibitem{Volpe}
+  C.~Volpe,
+  %``What about a Beta Beam facility for low energy neutrinos?,''
+  J.\ Phys.\ G {\bf 30} (2004) L1
+  [hep-ph/0303222].
+
+\bibitem{Lindroos}
+%\bibitem{Autin:2002ms}
+  B.~Autin {\it et al.},
+  %``The acceleration and storage of radioactive ions for a neutrino  factory,''
+  J.\ Phys.\ G {\bf 29}, 1785 (2003)
+  [physics/0306106];
+  %%CITATION = PHYS-ICS 0306106;%%
+% 
+  M.~Benedikt, S.~Hancock and M.~Lindroos,
+  % ``Baseline Design for a Beta-Beam Neutrino Factory'', 
+  Proceedings of EPAC, 2004,
+  \verb!http://accelconf.web.cern.ch/AccelConf/e04!;
+%
+  M.~Lindroos, EURISOL DS/TASK12/TN-05-02.
+
+\bibitem{Eurisol}
+  Eurisol Beta Beam webpage: \verb!http://beta-beam.web.cern.ch/beta-beam/!.
+
+\bibitem{Lindroos-Optimization}
+  M.~Benedikt, A.~Fabich, S.~Hancock and M.~Lindroos,
+  %``Optimization Of The Beta-Beam Baseline,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 155} (2006) 211.
+
+\bibitem{MezzettoNuFact05}
+  M.~Mezzetto,
+  %``Physics potential of the gamma = 100,100 beta beam,''
+  Nucl.\ Phys.\ Proc.\ Suppl.\  {\bf 155} (2006) 214
+  [hep-ex/0511005].
+
+% SPL %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\bibitem{Neugen}
+  The NEUGEN neutrino event generator,
+  \verb!http://minos.phy.tufts.edu/gallag/neugen/!.
+
+\bibitem{FLUKA}
+A.~Fasso \etal, Proceedings of the MonteCarlo 2000 conference, 
+Lisbon, October 26 2000, 
+A.~Kling \etal\ (eds.), Springer-Verlag Berlin (2001), 159-164 and 955-960. 
+
+\bibitem{GEANT}
+Application Software group, Computing and Network Division \etal, 
+GEANT Description and Simulation Tool, CERN Geneva, Switzerland
+
+\bibitem{HARP-MINERVA}
+  C. Catanesi \etal\ [HARP Coll.], CERN-SPSC 2002/019;
+%
+%\bibitem{Drakoulakos:2004gn}
+  D.~Drakoulakos {\it et al.}  [Minerva Coll.],
+  %``Proposal to perform a high-statistics neutrino scattering experiment  using
+  %a fine-grained detector in the NuMI beam,''
+  hep-ex/0405002.
+  %%CITATION = HEP-EX 0405002;%%
+
+\bibitem{Mezzetto:2003mm}
+  M.~Mezzetto,
+  %``Physics potential of the SPL super beam,''
+  J.\ Phys.\ G {\bf 29}, 1781 (2003)
+  [hep-ex/0302005].
+  %%CITATION = HEP-EX 0302005;%%
+
+% ATM %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\bibitem{Honda:2004yz}
+  M.~Honda, T.~Kajita, K.~Kasahara and S.~Midorikawa,
+  %``A new calculation of the atmospheric neutrino flux in a 3-dimensional
+  %scheme,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 043008
+  [astro-ph/0404457].
+  %%CITATION = ASTRO-PH 0404457;%%
+
+\bibitem{Lipari:1991ut}
+  P.~Lipari and T.~Stanev,
+  %``Propagation of multi - TeV muons,''
+  Phys.\ Rev.\ D {\bf 44} (1991) 3543.
+  %%CITATION = PHRVA,D44,3543;%%
+
+\bibitem{Gonzalez-Garcia:2004wg}
+  M.~C.~Gonzalez-Garcia and M.~Maltoni,
+  %``Atmospheric neutrino oscillations and new physics,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 033010
+  [hep-ph/0404085].
+  %%CITATION = HEP-PH 0404085;%%
+
+% DEGENERACIES %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\bibitem{Burguet-Castell:2001ez}
+  J.~Burguet-Castell, M.~B.~Gavela, J.~J.~Gomez-Cadenas, P.~Hernandez and O.~Mena,
+  %``On the measurement of leptonic CP violation,''
+  Nucl.\ Phys.\ B {\bf 608} (2001) 301
+  [hep-ph/0103258].
+  %%CITATION = HEP-PH 0103258;%%
+
+\bibitem{Minakata:2001qm}
+  H.~Minakata and H.~Nunokawa,
+  %``Exploring neutrino mixing with low energy superbeams,''
+  JHEP {\bf 0110}, 001 (2001)
+  [hep-ph/0108085].
+  %%CITATION = HEP-PH 0108085;%%
+
+\bibitem{Fogli:1996pv}
+  G.~L.~Fogli and E.~Lisi,
+  %``Tests of three-flavor mixing in long-baseline neutrino oscillation
+  %experiments,''
+  Phys.\ Rev.\ D {\bf 54}, 3667 (1996)
+  [hep-ph/9604415].
+  %%CITATION = HEP-PH 9604415;%%
+
+\bibitem{Barger:2001yr}
+  V.~Barger, D.~Marfatia and K.~Whisnant,
+  %``Breaking eight-fold degeneracies in neutrino CP violation, mixing, and
+  %mass hierarchy,''
+  Phys.\ Rev.\ D {\bf 65}, 073023 (2002)
+  [hep-ph/0112119].
+  %%CITATION = HEP-PH 0112119;%%
+
+\bibitem{Yasuda:2004gu}
+  O.~Yasuda,
+  %``New plots and parameter degeneracies in neutrino oscillations,''
+  New J.\ Phys.\  {\bf 6}, 83 (2004)
+  [hep-ph/0405005].
+  %%CITATION = HEP-PH 0405005;%%
+
+
+\bibitem{Antusch:2004yx}
+  S.~Antusch, P.~Huber, J.~Kersten, T.~Schwetz and W.~Winter,
+  %``Is there maximal mixing in the lepton sector?,''
+  Phys.\ Rev.\ D {\bf 70}, 097302 (2004)
+  [hep-ph/0404268].
+  %%CITATION = HEP-PH 0404268;%%
+
+\bibitem{Minakata:2004pg}
+  H.~Minakata, M.~Sonoyama and H.~Sugiyama,
+  %``Determination of theta(23) in long-baseline neutrino oscillation
+  %experiments with three-flavor mixing effects,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 113012
+  [hep-ph/0406073].
+  %%CITATION = HEP-PH 0406073;%%
+
+\bibitem{Donini:2005db}
+  A.~Donini, E.~Fernandez-Martinez, D.~Meloni and S.~Rigolin,
+  %``nu/mu disappearance at the SPL, T2K-I, NOnuA and the neutrino factory,''
+  Nucl.\ Phys.\ B {\bf 743}, 41 (2006)
+  [hep-ph/0512038].
+  %%CITATION = HEP-PH 0512038;%%
+
+\bibitem{Peres:2003wd}
+  O.L.G.~Peres, A.Y.~Smirnov,
+  %``Atmospheric neutrinos: LMA oscillations, U(e3) induced interference and
+  %CP-violation,''
+  Nucl.\ Phys.\ B {\bf 680} (2004) 479
+  [hep-ph/0309312].
+  %%CITATION = HEP-PH 0309312;%%
+
+\bibitem{Gonzalez-Garcia:2004cu}
+  M.C.~Gonzalez-Garcia, M.~Maltoni, A.Y. Smirnov,
+  %``Measuring the deviation of the 2-3 lepton mixing from maximal with
+  %atmospheric neutrinos,''
+  Phys.\ Rev.\ D {\bf 70} (2004) 093005
+  [hep-ph/0408170].
+  %%CITATION = HEP-PH 0408170;%%
+
+\bibitem{Petcov:1998su}
+  S.~T.~Petcov,
+  %``Diffractive-like (or parametric-resonance-like?) enhancement of the  earth
+  %(day-night) effect for solar neutrinos crossing the earth core,''
+  Phys.\ Lett.\ B {\bf 434} (1998) 321
+  [hep-ph/9805262];
+  %%CITATION = HEP-PH 9805262;%%
+%
+%\bibitem{Chizhov:1998ug}
+  M.~Chizhov, M.~Maris and S.~T.~Petcov,
+  %``On the oscillation length resonance in the transitions of solar and
+  %atmospheric neutrinos crossing the earth core,''
+  hep-ph/9810501;
+  %%CITATION = HEP-PH 9810501;%%
+%
+%\bibitem{Chizhov:1999az}
+  M.~V.~Chizhov and S.~T.~Petcov,
+  %``New conditions for a total neutrino conversion in a medium,''
+  Phys.\ Rev.\ Lett.\  {\bf 83} (1999) 1096
+  [hep-ph/9903399].
+  %%CITATION = HEP-PH 9903399;%%
+
+\bibitem{Akhmedov:1998ui}
+  E.~K.~Akhmedov,
+  %``Parametric resonance of neutrino oscillations and passage of solar and
+  %atmospheric neutrinos through the earth,''
+  Nucl.\ Phys.\ B {\bf 538}, 25 (1999)
+  [hep-ph/9805272];
+  %%CITATION = HEP-PH 9805272;%%
+%
+%\bibitem{Akhmedov:1998xq}
+  E.~K.~Akhmedov, A.~Dighe, P.~Lipari and A.~Y.~Smirnov,
+  %``Atmospheric neutrinos at Super-Kamiokande and parametric resonance in
+  %neutrino oscillations,''
+  Nucl.\ Phys.\ B {\bf 542}, 3 (1999)
+  [hep-ph/9808270].
+  %%CITATION = HEP-PH 9808270;%%
+
+\bibitem{Bernabeu:2003yp}
+  J.~Bernabeu, S.~Palomares-Ruiz and S.~T.~Petcov,
+  %``Atmospheric neutrino oscillations, theta(13) and neutrino mass
+  %hierarchy,''
+  Nucl.\ Phys.\ B {\bf 669}, 255 (2003)
+  [hep-ph/0305152].
+  %%CITATION = HEP-PH 0305152;%%
+
+\bibitem{Kim:1998bv}
+  C.~W.~Kim and U.~W.~Lee,
+  %``Comment on the possible electron-neutrino excess in the  Super-Kamiokande
+  %atmospheric neutrino experiment,''
+  Phys.\ Lett.\ B {\bf 444}, 204 (1998)
+  [hep-ph/9809491].
+  %%CITATION = HEP-PH 9809491;%%
+
+\bibitem{Kajita}
+  T.~Kajita, Talk at NNN05, 7--9 April 2005, Aussois, Savoie, France,\\
+  \verb!http://nnn05.in2p3.fr/!
+
+\bibitem{Petcov:2005rv}
+  S.~T.~Petcov and T.~Schwetz,
+  %``Determining the neutrino mass hierarchy with atmospheric neutrinos,''
+  Nucl.\ Phys.\ B {\bf 740}, 1 (2006)
+  [hep-ph/0511277].
+  %%CITATION = HEP-PH 0511277;%%
+
+\bibitem{MenaRequejo:2005hn}
+  O.~Mena-Requejo, S.~Palomares-Ruiz and S.~Pascoli,
+  %``Super-NOvA: A long-baseline neutrino experiment with two off-axis
+  %detectors,''
+  Phys.\ Rev.\ D {\bf 72} (2005) 053002
+  [hep-ph/0504015];
+  %%CITATION = HEP-PH 0504015;%%
+%
+%\bibitem{Mena:2005ri}
+  %O.~Mena, S.~Palomares-Ruiz and S.~Pascoli,
+  %``Determining the neutrino mass hierarchy and CP violation in NOnuA with a
+  %second off-axis detector,''
+  Phys.\ Rev.\ D {\bf 73} (2006) 073007
+  [hep-ph/0510182].
+  %%CITATION = HEP-PH 0510182;%%
+
+\bibitem{Barger:2006vy}
+  V.~Barger {\it et al.}, 
+  % M.~Dierckxsens, M.~Diwan, P.~Huber, C.~Lewis, D.~Marfatia and B.~Viren,
+  %``Precision physics with a wide band super neutrino beam,''
+  Phys.\ Rev.\  D {\bf 74} (2006) 073004
+  [hep-ph/0607177].
+  %%CITATION = PHRVA,D74,073004;%%
+
+\bibitem{Kachelriess:2004vs}
+  M.~Kachelriess and R.~Tomas,
+  %``Identifying the neutrino mass hierarchy with supernova neutrinos,''
+  hep-ph/0412100.
+  %%CITATION = HEP-PH 0412100;%%
+
+\bibitem{ISSpage}
+  Webpage of the International Scoping Study physics working group:\\
+  \verb!http://www.hep.ph.ic.ac.uk/iss/wg1-phys-phen/index.html!
+
+\end{thebibliography}
+\end{document}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
