\documentclass[twoside,11pt]{article} % Definition pour Documentation L2 \usepackage{defdocl2} % Package standard : Utilisation de caracteres accentues, mode francais et graphique \usepackage[latin1]{inputenc} \usepackage[T1]{fontenc} \usepackage{babel} % \usepackage{graphicx} % package a mettre pour faire du pdf % \usepackage{palatino} % Extension de symboles mathematiques \usepackage{amssymb} \usepackage{amstex} % Definition de taille de page (c'est ds defdocl2.sty) \newcommand{\bul}{$\bullet \ $} \newcommand{\gph}[1]{ {\bf GPH#1} } \newcommand{\ngph}[1]{ GPH#1 } % Symboles en bold \newcommand{\bnu}{\boldsymbol{\nu}} \newcommand{\bbold}{\boldsymbol{b}} \newcommand{\dbold}{\boldsymbol{d}} \begin{document} \begin{titlepage} \titleph{ Planck HFI L2 \\ Work Breakdown Structure \\ Package Breakdown Structure } % Authors list \authors{ R. Ansari & LAL, Orsay \\ % & {\tt ansari@lal.in2p3.fr} \\ I.J. Grivell & ICSTM, London \\ G. Le Meur & LAL, Orsay \\ R.G. Mann & IfA, Edinburgh \\ M. Rowan-Robinson & ICSTM, London \\ S. Serjeant & ICSTM \\ J.F. Sygnet & IAS, Orsay \\ % {\tt Jean-Francois.Sygnet@ias.fr} \\ } \titlepfd{PL-HFI-LAL-PW-L2001}{2.0} \end{titlepage} % -------- Revision history \revisionhistory \begin{itemize} \item Version 1.0 (February 2000 - CVS version 1.1) \\ Draft version presented at the HFI consortium meeting \item Version 1.1 (April 2000 - CVS version 1.2) \\ Draft updated using the document prepared at ISCTM and IfA (Edinburgh) \item Version 2.0 (August 2000 - CVS version 1.3) \\ Inclusion of a section describing notation and conventions, flow charts. A more detailed description of deliverables is also included. \end{itemize} % -------- Table of content \newpage \tableofcontents \newpage \section{Introduction} This document contains a preliminary version a the Work Breakdown Structure (WBS), Package Breakdown Structure (PBS) for Planck-HFI Level 2 data processing. The Level 2 activity of the HFI Data Processing Centre (DPC) is divided between the Paris-Orsay-Saclay Data Analysis Centre (POSDAC) and the London Planck Analysis Centre (LPAC). POSDAC will run the Level 2 data processing pipeline and have overall responsibility for the collaborative work involved in its design and implementation. LPAC will a major role for in the activities that iterate and overlap between Level 2 and Level 3 (for which the Cambridge Planck Analysis Centre, CPAC, plays the role analogous to POSDAC at Level 2) \section{HFI L2 processing software packages} The Level 2 workpackages are listed below, with a numbering scheme derived from that in the {\it HFI Science Implementation Plan (SIP: draft of 19/11/99) }. All packages should be compliant with the general software architecture and use the services of the corresponding support modules (\gph{428}). \begin{itemize} \item[]\gph{421} RTA/QLA : Real Time Assesment, Quick Look Analysis. \item[]\gph{422} TOI processing \item[]\gph{423} Polarised TOI processing \item[]\gph{424} Basic 2-D map reconstruction from TOI's \item[]\gph{425} Optimal 2-D map reconstruction \item[]\gph{426} Optimal 2-D polarised map reconstruction \item[]\gph{427} Early Compact Source Catalogue \item[]\gph{428} General software architecture and support modules \item[]\gph{429} Integration and Validation \end{itemize} The package \gph424 should provide a resonably fast and simple method for reconstructing 2-D maps from cleaned TOI's (from \gph422 and \gph423), removing systematic effects (destriping) and deconvolving the antenna beam pattern. An iterative method is foreseen, capable of dealing with partial knowledge of instrument caracteristics. The optimal 2-D map reconstruction packages (\gph425 and \gph426) will implement the best feasible method for analysing the whole data set from the HFI instrument and building the full sky frequency maps. \begin{itemize} \item[]\gph{320} infrastructure procurement and maintenance (POSDAC) \item[]\gph{360} infrastructure procurement and maintenance (LPAC) \item[]\gph{140} Project management (POSDAC) \item[]\gph{180} Project management (LPAC) \end{itemize} The table below shows a very preliminary cost estimate in FTE-MY (Full Time Equivalent Man Years) for each package. \\ \begin{table} \begin{center} \begin{tabular}[h]{|c|c||c|c|} \hline \makebox[2.5cm][c]{Package} & \makebox[2.5cm][c]{Cost} & \makebox[2.5cm][c]{Package} & \makebox[2.5cm][c]{Cost} \\ \hline % & & & \\ \ngph{421} & 5 & \ngph{426} & ? \\ % \ngph{422} & 15 & \ngph{427} & 5 \\ % \ngph{423} & 15 & \ngph{428} & 30 \\ % \ngph{424} & 20 & \ngph{429} & 10 \\ % \ngph{425} & ? & & \\ % & & & \\ % \hline \ngph{320} & 3 & \ngph{140} & 4 \\ \ngph{360} & 2 & \ngph{180} & 1 \\ \hline \hline \multicolumn{2}{c}{\bf Total} & \multicolumn{2}{c}{\bf 110 + ?} \\ \hline \end{tabular} \end{center} \caption{Preliminary estimate of staff effort (in Full Time Equivalent Man-Years FTE-MY)} \end{table} \section{HFI data processing steps} The major steps for processing Planck-HFI data are briefly described here. For the sake of clarity, we define here the notation and conventions used throughout this document for referring to the different data components in planck HFI. Most of these data components are also defined in \cite{datamodel}. \subsection{Notation and conventions} \begin{itemize} \item[] {\bf Coordinates:} The spacecraft attitude is defined by the spin axis direction $SA (\theta, \phi)$. $\psi$ is the third angle defining the position of the spacecraft and thus a given detectors view direction and beam pattern orientation. A given sky direction is denoted $(\alpha,\delta)$ in equatorial coordinates, $(l,b)$ in Galactic coordinates or $(\lambda,\beta)$ in ecliptic coordinate. \item[] {\bf Detector:} A given HFI bolometer read-out channel. The corresponding signal is denoted $\dbold(t)$ or $\bbold(t)$ $\dbold^j(t)$ or $\bbold^j(t)$ where $j$ is the bolometer number. \item[] {\bf Frequency channel:} The set of detectors working in the same frequency range. This information is only obtained by combining information from several detectors in the corresponding frequency band. The subscript $\bnu$ is used to denote a frequency channel. The sky map in a given frequency band would be written as $Sky (\theta,\phi) \vert ^{\bnu}$. \item[] {\bf Scan:} The time interval corresponding to a nominal spin axis direction \end{itemize} \subsection{Processing steps} \section{GPH421: RTA/QLA Real Time Assesment, Quick Look Analysis} \begin{itemize} \item[]\gph{421.1} Quick look analysis \item[]\gph{421.2} Evaluation of instrument health \item[]\gph{421.1} Exchange of information with LFI of mission/spacecraft/payload-dependent effects common to both instruments \end{itemize} \section{GPH422: TOI processing} This package contains all the processing which has to be perfomed on TOI's (Time Ordered Information ) for either a single-detector or multpile-detector, single-frequency set of TOI's. A very rough sketch of data flow and processing steps for GPH422 is given in figure \ref{fig422}. \begin{figure}[htbp] \mbox{\hspace*{1cm} \includegraphics[width=7cm]{gph422_1.eps} \includegraphics[width=7cm]{gph422_2.eps} } \caption{Data flow and processing steps for GPH422} \label{fig422} \end{figure} \begin{itemize} \item[]\gph{422.1} TOI statistical characterisation \begin{itemize} \item[]422.1.1 Raw time-line statistical checks \item[]422.1.2 Evaluation of noise components in TOI \\ (including use of redundancy to produce independent coadds) \item[]422.1.3 Low frequency drifts \item[]422.1.4 Correlation of TOI with housekeeping data and various coordinate systems to look for systematic trends \item[]422.1.5 correlation of TOI between channels to identify cross-talk \end{itemize} \item[]\gph{422.2} TOI filters \begin{itemize} \item[]422.2.1 Time domain filtering \item[]422.2.2 Fourier filtering \end{itemize} \item[]\gph{422.3} Deglitching and source extraction \begin{itemize} \item[]422.3.1 production of deglitched TOI, flagged to indicate cosmic ray hits etc. \item[]422.3.2 Point source detectors \item[]422.3.3 Galaxy crossing detector \item[]422.3.4 CMB dipole finder \end{itemize} \item[]\gph{422.4} Astrometric calibration \\ Astrometric calibration using known point sources, bright sources from the ECSC and galaxy crossing in TOI. \item[]\gph{422.5} Photometric calibration \begin{itemize} \item[]422.5.1 extended-source photometric calibration using known sources (Galaxy) and COBE/FIRAS data \item[]422.5.2 point-source photometric calibration using known sources \item[]422.5.3 reconstruction of beam pattern seen by each detector from observations of bright \end{itemize} \item[]\gph{422.6} reconstruction of beam pattern seen by each detector from observations of bright point sources \gph{422.3.2} and galaxy crossing \gph{422.3.3} \item[]\gph{422.7} Production of single pointing co-added rings \item[]\gph{422.9} Deliverables: Cleaned, calibrated TOI's : \begin{itemize} \item $(\alpha, \delta)$, roll angle, calibrated signal \item Noise statistics \item Offset/drifts \item Co-added rings \end{itemize} \end{itemize} \section{GPH423: Polarised TOI processing} \gph{423.1} Additional TOI processing, as required to reconstruct Stokes I,Q,U parameters from detector signals in polarised channels. \section{GPH424: Simple 2-D map reconstruction} This package contains all the necessary modules for single frequency 2-D map reconstruction using the cleaned TOI's from \gph{422} and \gph{423}. However \gph{424} should only implement simple versions of 2-D map making and systematic removal algorithms, as opposed to \gph{424} which must provide a global, optimal 2-D map reconstruction with systematic effects assessment. \begin{itemize} \item[]\gph{424.1} 1D $\rightarrow$ 2D Projector \item[]\gph{424.2} Estimation and subtraction of systematic effects \begin{itemize} \item[]424.2.1 Low frequency noise estimation \item[]424.2.2 far side determination using moon/earth during commissioning phases. \item[]424.2.3 far side lobe subtraction \item[]424.2.4 use of redundancy to produce independent maps for assessment of noise contributions \end{itemize} \item[]\gph{424.3} Main lobe \begin{itemize} \item[]424.3.1 supplementing source extraction from TOI with use of sources selected from frequency maps \item[]424.3.2 reconstruction of beam pattern from maps using known point and bright ECSC sources. \end{itemize} \item[]\gph{424.4} Astrometric calibration using known and bright ECSC sources. \item[]\gph{424.5} Photometric calibration \item[]\gph{424.6} Postage stamp maps for compact sources \item[]\gph{424.9} Deliverables: Full sky maps \\ \begin{itemize} \item Sky maps per frequency channels $map_\nu (\alpha, \delta) $ \item Reprocessed TOI's \end{itemize} \end{itemize} \section{GPH425: Global 2-D map reconstruction} Implementation of an optimal 2-D full sky map reconstruction, with systematics (low frequency drifts, side lobes, \ldots) estimation and removal. This package definition and breakdown structure can only be refined at a later stage, after preliminary studies of applicable methods. \begin{itemize} \item[]\gph{425.9} Deliverables: Full sky maps \\ \begin{itemize} \item Full sky maps for each frequency channels $map_\nu (\alpha, \delta) $ \item Reprocessed, cleanead TOI's \item Beam patterns per detector and per frequency channel \item Estimation of systematics \end{itemize} \end{itemize} \section{GPH426: Global polarised 2-D map reconstruction} This module, a extended version of \gph{425} has to take into account specific constraints related to polarised TOI's and sky map reconstruction \begin{itemize} \item[]\gph{426.9} Deliverables: full sky maps for each polarisation component (I,Q,U) \\ \begin{itemize} \item Full sky maps for each frequency channels $map_\nu (\alpha, \delta) $ for each component (I,Q,U) \item Reprocessed, cleanead TOI's for I,Q,U \item Noise and systematic effect maps and characteristics \end{itemize} \end{itemize} \section{GPH427: Early Compact Source Catalogue} \begin{itemize} \item[]\gph{427.9} Deliverables: Source catalogue \\ \begin{itemize} \item Astrometrically calibrated source positions and photometrically calibrated flux in each frequency band \\ $$(\alpha, \delta)_i , F_i^\nu, i=1,..,N$$ \item Llocal sky maps in each frequency bands for areas around all source positions. \item Related software and documentation \end{itemize} \end{itemize} \section{GPH428: General software architecture and support modules} This package defines the general architecture for the level 2 processing software and insures the compliance with IDIS framework. It provides also the support modules for the different level 2 packages (\gph{42x}) and their interfaces with IDIS components. \begin{itemize} \item[]\gph{428.1} Definition and construction of the software architecture \item[]\gph{428.2} Development and maintenance of TOI manipulation module (including diagnostics and display) \item[]\gph{428.3} Development and maintenance of maps manipulation module (including diagnostics and display of both full and local sky maps) \item[]\gph{428.4} Instrument and satellite representation \begin{itemize} \item[]428.4.1 Focal plane geometry \item[]428.4.2 Detector's frequency response \item[]428.4.3 Main and secondary lobes \item[]428.4.4 Sampling and noise characteristics \item[]428.4.5 Orbit and attitude \item[]428.4.6 Thermal model \end{itemize} \item[]\gph{428.5} Development/supply and maintenence of standard numerical analysis tools \begin{itemize} \item[]428.5.1 Arrays (Matrix, Vectors, \ldots) and linear algebra \item[]428.5.2 Fourier analysis, Wavelet analysis \item[]428.5.3 Minimisation, optimisation \item[]428.5.4 Statistical analysis \end{itemize} \item[]\gph{428.6} Interface with DMC \item[]\gph{428.7} Interface with the process coordinator \end{itemize} \section{GPH429: Integration and Validation} The assembly of the different L2 processing modules and integration in the pipeline, as well as the assessment of the overall quality of the delivered data products is the responsibility of \gph{429}. The data quality validation activity includes iterative work using Level 2 and 3 data products, and comparison of HFI and LFI data for the common 100 GHz channel: for example, activity in this workpackage may influence the details of how the Global polarised 2D map reconstruction of \gph{426} is performed, leading to the changes in the deliverables from that workpackage. \begin{itemize} \item[]\gph{429.1} Pipeline management \begin{itemize} \item[]429.1.1 management and construction of pipeline modules and their interfaces \item[]429.1.2 IDIS and DMC interface \item[]429.1.2 Management of pipeline operations \end{itemize} \item[]\gph{429.2} Iterative study of systematic effects (e.g. map striping, etc) involving both level 2 and level 3 products \item[]\gph{429.3} Combination, comparison and validation of source catalogues derived from Levels 2 and 3 source extraction \item[]\gph{429.4} Comparison of TOI data and maps between HFI and LFI for common 100GHz channel \item[]\gph{429.9} Deliverables: Full sky maps for each polarisation component (I,Q,U) \\ \begin{itemize} \item Sky maps per frequency channels $map_\nu (\alpha, \delta) $ for each component (I,Q,U) \item Reprocessed, cleanead TOI's for I,Q,U \item Noise and systematic effect maps and characteristics \item Photometric and Astrometric calibration \item Associated software and documentation \end{itemize} \end{itemize} \begin{thebibliography}{10} \bibitem{datamodel} \newblock {\bf PL-COM-OAT-TN-003} \newblock {Planck IDIS Data Model Description Document} \end{thebibliography} \end{document}