Changeset 4069 in Sophya for trunk/Cosmo/RadioBeam/sensfgnd21cm.tex

Timestamp:

Apr 27, 2012, 11:47:27 AM (13 years ago)

Author:

ansari

Message:

dernières corrections (proofreading) du papier avant publication par A&A, 26 Mars 2012, 27/04/2012

File:

• trunk/Cosmo/RadioBeam/sensfgnd21cm.tex (modified) (8 diffs)

trunk/Cosmo/RadioBeam/sensfgnd21cm.tex

@@ -219 +219 @@
 $1 \lesssim z \lesssim 2$, and possibly up to the reionization redshift \citep{wyithe.08}.
 
-In section 2, we  discuss the intensity mapping and its potential for measuring of the
+In section 2, we  discuss the intensity mapping and its potential for measuring the
 \HI mass distribution power spectrum. The method used in this paper to characterize 
 a radio instrument response and sensitivity for $P_{\mathrm{H_I}}(k)$ is presented in section 3.
@@ -398 +398 @@
 compared to its current value $\gHI(z=1.5) \sim 0.025$. 
 The 21 cm brightness temperature and the corresponding power spectrum can be written as 
-(\cite{madau.97}; \cite{zaldarriaga.04}); \cite{barkana.07})
+(\cite{madau.97}; \cite{zaldarriaga.04}; \cite{barkana.07})
 \begin{eqnarray}
  P_{T_{21}}(k) & = & \left( \bar{T}_{21}(z)  \right)^2 \, P(k)    \label{eq:pk21z} \\
@@ -628 +628 @@
 { \changemark
 \begin{eqnarray}
-\alpha , \beta & \rightarrow &  \ell_\perp = l_x, l_y = (1+z) \, \dang(z) \,  \alpha,\beta  \\
+\alpha , \beta & \rightarrow &  \ell_\perp = \ell_x, \ell_y = (1+z) \, \dang(z) \,  \alpha,\beta  \\
 \uv & \rightarrow & k_\perp = k_x, k_y = 2 \pi \frac{ \uvu , \uvv }{  (1+z) \, \dang(z)  }   \label{eq:uvkxky} \\
 \delta \nu & \rightarrow & \delta \ell_\parallel = (1+z) \frac{c}{H(z)} \frac{\delta \nu}{\nu} 
@@ -672 +672 @@
 to a 3D white noise, with a uniform noise spectral density:}
 \begin{equation}
-P_{noise}(k_\perp, l_\parallel(\nu) ) = P_{noise} = 2 \, \frac{\Tsys^2}{t_{int} \, \nu_{21} } \, \frac{\lambda^2}{D^2}  \, \dang^2(z) \frac{c}{H(z)} \, (1+z)^4  
+P_{noise}(k_\perp, \ell_\parallel(\nu) ) = P_{noise} = 2 \, \frac{\Tsys^2}{t_{int} \, \nu_{21} } \, \frac{\lambda^2}{D^2}  \, \dang^2(z) \frac{c}{H(z)} \, (1+z)^4  
 \label{ctepnoisek}
 \end{equation} 
@@ -980 +980 @@
  
 \subsection{ Synchrotron and radio sources }
-We modeled the radio sky in the form of three 3D maps (data cubes) of sky temperature 
+We modeled the radio sky in the form of 3D maps (data cubes) of sky temperature 
 brightness $T(\alpha, \delta, \nu)$ as a function of two equatorial angular coordinates $(\alpha, \delta)$ 
 and the frequency $\nu$. Unless otherwise specified, the results presented here are based on simulations of 
@@ -1579 +1579 @@
 The \HI power spectrum is divided by an envelop curve $P(k)_{ref}$ 
 corresponding to the power spectrum without baryonic oscillations. 
-The dots represents one simulation for a "packed" array of cylinders  
+The dots represents one simulation for a "packed" array of dishes  
 with a system temperature,$T_{sys}=50$K, an observation time, 
 $T_{obs}=$ 1 year, 
@@ -1609 +1609 @@
 \includegraphics[width=8.5cm]{Figs/AveragedPk.pdf}
 \caption{1D projection of the power spectrum averaged over 100 simulations
-of the packed cylinder array $b$. 
+of the packed dish array. 
 The simulations are performed for the following conditions: a system 
 temperature $T_{sys}=50$K, an observation time $T_{obs}=1$ year, 
@@ -1809 +1809 @@
 
 \section{Conclusions}
-The 3D mapping of redshifted 21 cm emission though {\it intensity mapping} is a novel and complementary 
+The 3D mapping of redshifted 21 cm emission through {\it intensity mapping} is a novel and complementary 
 approach to optical surveys for studying the statistical properties of the LSS in the universe
 up to redshifts $z \lesssim 3$. A radio instrument with a large instantaneous field of view