Index: trunk/doc/design/ippSRS.tex =================================================================== --- trunk/doc/design/ippSRS.tex (revision 2241) +++ trunk/doc/design/ippSRS.tex (revision 2544) @@ -1,7 +1,7 @@ - %%% $Id: ippSRS.tex,v 1.12 2004-10-29 22:00:08 eugene Exp $ + %%% $Id: ippSRS.tex,v 1.13 2004-11-30 23:16:03 eugene Exp $ \documentclass[panstarrs,spec]{panstarrs} % basic document variables -\title{Pan-STARRS Image Processing Pipeline} +\title{Pan-STARRS PS-1 Image Processing Pipeline} \subtitle{Software Requirements Specification} \shorttitle{IPP SRS} @@ -11,5 +11,5 @@ \project{Pan-STARRS Image Processing Pipeline} \organization{Institute for Astronomy} -\version{DR} +\version{01} \docnumber{PSDC-430-005} @@ -34,11 +34,11 @@ \RevisionsStart % version Date Description -DR.01 & 2004.01.01 & First draft \\ \hline -DR.02 & 2004.03.10 & Second draft \\ \hline -DR.03 & 2004.04.13 & Most paragraphs fleshed out \\ \hline -DR.04 & 2004.04.27 & Basic text frozen for internal review \\ \hline -DR.05 & 2004.05.24 & Incorporating comments from internal review \\ \hline -DR.06 & 2004.08.06 & Revisions in prep of SRR \\ \hline -DR.06 & 2004.10.22 & Revisions based on SRR \\ \hline +% DR.01 & 2004.01.01 & First draft \\ \hline +% DR.02 & 2004.03.10 & Second draft \\ \hline +% DR.03 & 2004.04.13 & Most paragraphs fleshed out \\ \hline +% DR.04 & 2004.04.27 & Basic text frozen for internal review \\ \hline +% DR.05 & 2004.05.24 & Incorporating comments from internal review \\ \hline +00 & 2004.08.06 & Revisions in prep of SRR \\ \hline +01 & 2004.10.29 & Revisions based on SRR \\ \hline \RevisionsEnd @@ -121,8 +121,9 @@ that series is implied. -Open issues (TBDs) in this document are marked \tbd{in bold red}. - -Quantities which should be reviewed (TBRs) are marked \tbr{in bold -blue}. +Open issues (TBDs) in this document are marked {\bf \color{red} in +bold red}. + +Quantities which should be reviewed (TBRs) are marked {\bf +\color{blue} in bold blue}. \subsubsection{``Shall''} When used in this specification, the word @@ -141,10 +142,13 @@ \DocumentsInternalSection -PSDC-130-001 & PS-1 Design Reference Mission \\ \hline -PSDC-130-xxx & PS-1 SCD \\ \hline -PSDC-430-004 & Pan-STARRS IPP C Code Conventions \\ \hline -PSDC-430-006 & Pan-STARRS IPP ADD \\ \hline -PSDC-430-006 & Pan-STARRS IPP SDRS \\ \hline -PSDC-430-007 & Pan-STARRS IPP PSLib SDRS \\ \hline +PSDC-230-001 & PS-1 Design Reference Mission \\ \hline +PSDC-230-002 & PS-1 System Concept Definition \\ \hline +PSDC-400-006 & The Pan-STARRS IPP Computational Challenge \\ \hline +PSDC-430-004 & Pan-STARRS PS-1 IPP C Code Conventions \\ \hline +PSDC-430-006 & Pan-STARRS PS-1 IPP Algorithm Design Document \\ \hline +PSDC-430-007 & Pan-STARRS PS-1 IPP PSLib Supplementary Design Requirements Specification \\ \hline +PSDC-430-010 & Pan-STARRS PS-1 IPP Perl Code Conventions \\ \hline +PSDC-430-011 & Pan-STARRS PS-1 IPP System/Subsystem Design Description \\ \hline +PSDC-430-012 & Pan-STARRS PS-1 IPP Modules Supplementary Design Requirements Specification \\ \hline \DocumentsExternalSection Posix Standard & Open Group Based Specifications Issue 6, IEEE Std 1003.1, 2003 \\ @@ -179,5 +183,5 @@ The Pan-STARRS System Concept Definition (SCD) specifies the derived top-level requirements for the IPP, which we reproduce here (with -numbering consistent with this document): +numbering consistent within this document): \begin{enumerate} @@ -261,6 +265,6 @@ \label{TLR:15} -\item The IPP shall degrade the stacked image by no more than \tbr{10 - milliarcseconds (FWHM added in quadrature)} over the theoretical +\item The IPP shall degrade the stacked image by no more than 150 + milliarcseconds (FWHM added in quadrature) over the theoretical limit for the stack under infinite sampling.\VER{ANALYSIS}{SCD:3.5.2} @@ -269,6 +273,6 @@ \item The IPP shall perform the processing of science images to the level of transient detection and static sky inclusion at a rate such - that exposures taken at an \tbr{average cadence of 40 seconds} do - not accumulate in the processing buffer (average throughput + that exposures taken at an average cadence of 40 seconds do not + accumulate in the processing buffer (average throughput requirement).\VER{TEST}{SCD:3.2.2.3} \label{TLR:17} @@ -281,5 +285,5 @@ \item The IPP shall perform transient detection to a completeness of - 99\% at the completeness for transient detections with a significant + 99\% at the completeness for transient detections with a significance $> 5\sigma$.\VER{ANALYSIS}{SCD:xxx} @@ -300,6 +304,7 @@ \label{TLR:21} -\item The IPP shall provide access to preferred Pan-STARRS science clients to the - detected transient objects within \tbr{5 minutes}.\VER{TEST}{SCD:3.5.10} +\item The IPP shall provide access to preferred Pan-STARRS science + clients to the detected transient objects within 15 minutes with at + least 85\% reliability.\VER{TEST}{SCD:3.5.10} \label{TLR:22} @@ -375,6 +380,6 @@ \item Because the delivered code is required to run on UNIX machines, the delivered code shall be in compliance with the language-independent UNIX operating system standard POSIX (Open Group Based Specifications Issue 6, IEEE Std 1003.1, 2004).\VER{INSPECT}{allocated} \item Source code files shall use the UNIX line-break convention (line-feed only). \VER{INSPECT}{allocated} -\item C coding style shall adhere to the standard defined in the document `Pan-STARRS C-coding standard' (PSDC-430-004). \VER{INSPECT}{allocated} -\item Perl coding shall follow the standard defined in the document \tbd{`Pan-STARRS Perl-coding standard' (PSDC-430-0XX)}.\VER{INSPECT}{allocated} +\item C coding style shall adhere to the standard defined in the document `Pan-STARRS IPP C-coding standard' (PSDC-430-004). \VER{INSPECT}{allocated} +\item Perl coding shall follow the standard defined in the document `Pan-STARRS IPP Perl-coding standard' (PSDC-430-010).\VER{INSPECT}{allocated} \end{enumerate} @@ -501,17 +506,7 @@ \subsubsection{Software Configuration} -\paragraph{Version Management} - -The IPP software configuration management system shall ensure that -validated versions of both internal and external software are used -when the software is compiled.\VER{TEST}{allocated} - -\paragraph{Optional Modes} - -The IPP software configuration management system shall provide -optionally selected software version sets under compilation -conditions. For example, compilation of the software for test -purposes with a non-standard FFT tool shall be an -option.\VER{TEST}{allocated} +The IPP software configuration management system shall follow the +processes outlined by the Pan-STARRS IPP Software Configuration +Management Place (PSDC-430-003).\VER{INSPECT}{allocated} \subsection{Architectural Components} @@ -525,12 +520,11 @@ As discussed in the Pan-STARRS System Concept Definition -(PSDC-250-002), the IPP is organized into a number of clearly-defined -software elements. The SCD provides a detailed description of the -roles and responsibilities of these subsystems. In brief, the IPP -consists of: a collection of science analysis programs which perform -the stages of the data analysis; a set of architectural components -which provide the infrastructure needed to run the analysis programs; -and a collection of hardware on which all of the software elements -exist and operate. +(PSDC-230-002), the IPP is organized into a number of clearly-defined +software elements. The SCD provides a detailed description of these +subsystems. In brief, the IPP consists of: a collection of science +analysis programs which perform the stages of the data analysis; a set +of architectural components which provide the infrastructure needed to +run the analysis programs; and a collection of hardware on which all +of the software elements exist and operate. The architectural components consist of: @@ -546,4 +540,10 @@ it is no longer needed by other portions of the IPP. +\item {\bf IPP Metadata Database:} This component is used to store all + other data which are neither image files nor astronomical object + data. The Metadata Database is the authoritative source for all + metadata data, including metadata which may be duplicated elsewhere, + such as in the headers of images in the image database. + \item {\bf Astrometry \& Photometry Database (AP):} This component is used to store and manipulate astronomical objects detected in images @@ -554,10 +554,4 @@ needed to interpret the object data. -\item {\bf IPP Metadata Database:} This component is used to store all - other data which are neither image files nor astronomical object - data. The Metadata Database is the authoritative source for all - metadata data, including metadata which may be duplicated elsewhere, - such as in the headers of images in the image database. - \item {\bf IPP Controller:} In order to perform the analysis stages required by the IPP, it is necessary to use distributed computing @@ -588,5 +582,5 @@ \begin{enumerate} \item The IPP Image Server shall accept raw images from the summit at - a sustained rate of 1 exposure (2~GB) per \tbr{40 seconds.} + a sustained rate of 1 exposure (2~GB) per 40 seconds. \VER{TEST}{TLR:17, TLR:23} @@ -597,6 +591,6 @@ reference to the specified image.\VER{TEST}{allocated} -\item The IPP Image Server shall provide a total data capacity of 300 - TB after the first year of PS-1 operations and 900 TB after the +\item The IPP Image Server shall provide a total data capacity of 400 + TB after the first year of PS-1 operations and 750 TB after the second year of operations.\VER{INSPECT}{} @@ -607,73 +601,28 @@ \end{enumerate} -\subsubsection{AP Database} - -%%% Table: AP DB parameters -\begin{table} -\begin{center} -\caption{AP Detection Classes \& Object Parameters\label{APdetections}} -\begin{tabular}{lrrrr} -\hline -\hline -Object Parameter & P2 & P4$\Sigma$ & P4$\Delta$ & SS \\ -\hline -PSF x,y, covar, $\alpha,\delta$ & + & + & + & + \\ -PSF mag, $\sigma_{\rm mag}$ & + & + & + & + \\ -star/gal sep & + & + & + & + \\ -$\sigma_x$, $\sigma_y$, $\theta$ & + & + & + & + \\ -local sky data & + & + & + & + \\ -Petrosian R, M, $R_{50}$, $R_{90}$ & - & + & - & + \\ -S\'ersic R, M, AB, $\phi$, $\nu$ & - & + & - & + \\ -W.L. $\gamma_1$, $\gamma_2$, pol. terms & - & - & - & + \\ -exp. spaced aps., Poisson noise, variance & - & - & - & + \\ -\hline -\end{tabular} -\end{center} -\end{table} - -%%% Table: AP DB Throughput -\begin{table} -\begin{center} -\caption{AP Data Volume and Throughput Requirements\label{APrates}} -\begin{tabular}{lrrr} -\hline -\hline -Quantity & P2 & P4$\Sigma$ & P4$\Delta$ \\ -\hline -detection limit & $20 \sigma$ & $5 \sigma$ & $3 \sigma$ \\ -depth (r') & 21.8 & 24.0 & 24.5 \\ -bytes star$^{-1}$ & 64 & 100 & 64 \\ -stars deg$^{-2}$ ($|b|>10$) & $2.0 \times 10^5$ & $8.0 \times 10^5$ & $2.0 \times 10^5$ \\ -stars FPA$^{-1}$ ($|b|>10$) & $1.4 \times 10^6$ & $5.6 \times 10^6$ & $1.4 \times 10^6$ \\ -stars sec$^{-1}$ ($|b|>10$) & $3.5 \times 10^4$ & $3.5 \times 10^4$ & $8.8 \times 10^3$ \\ -MB sec$^{-1}$ & 2.3 & 3.5 & 0.6 \\ -AP total TB & 7.7 & - & - \\ -IVP total TB & 13 & 20 & 3 \\ -MOPS total TB & 4 & 6 & 1 \\ -PS-1 total TB & 25 & 26 & 4 \\ -\hline -\end{tabular} -\end{center} -\end{table} - -%% IPP AP DB Requirements -The IPP AP Database has the following performance requirements: - -\begin{enumerate} -\item The AP Database shall accept new detections at the rate - generated by the telescope from the Phase 2 and Phase 4 analysis. - Except within 10 degrees of the galactic plane, the AP Database - shall keep up with the incoming rates. The expected rates are - listed in Table~\ref{APrates}, along with the total data volume - required for storage space over the PS-1 lifetime.\VER{TEST}{TLR:2, - TLR:3, TLR:22} - -\item The AP Database shall provide access to external Pan-STARRS - clients to the detected objects within \tbr{5 minute} after the - image is obtained.\VER{TEST}{TLR:22} - \label{IPP:DeReq:29c} -\end{enumerate} - \subsubsection{Metadata Database} + +%% Metadata DB Requirements + +The Metadata Database has the following requirements: + +\begin{enumerate} +\item The IPP Metadata Database shall accept metadata from the summit + at a nightly average rate of 1 MB per 40 second.\VER{TEST}{TLR:17, + TLR:21, TLR:25} + +\item The Metadata Database queries shall have a latency of $< 0.1$ + seconds.\VER{TEST}{TLR:17} + +\item The Metadata Database shall be capable of at least 100 queries + per second.\VER{TEST}{TLR:17} + +\item The Metadata Database shall be capable of accepting a total data + volume after 2 years of operation of 280 GB. \VER{INSPECT}{TLR:25} + +\item The Metadata Database shall restrict write access of the + scientific parameters to a different group from the software and + hardware configuration parameters.\VER{TEST}{allocated} +\end{enumerate} %% Table: Metadata data classes @@ -702,26 +651,71 @@ \end{table} -%% Metadata DB Requirements - -The Metadata Database has the following requirements: - -\begin{enumerate} -\item The IPP Metadata Database shall accept metadata from the summit - at a sustained rate of \tbr{1 MB per 40 second.}\VER{TEST}{TLR:17, - TLR:21, TLR:25} - -\item The Metadata Database queries shall have a latency of $< 0.1$ - seconds.\VER{TEST}{TLR:17} - -\item The Metadata Database shall be capable of at least 100 queries - per second.\VER{TEST}{TLR:17} - -\item The Metadata Database shall be capable of accepting a total data - volume after 2 years of operation of 280 GB. \VER{INSPECT}{TLR:25} - -\item The Metadata Database shall restrict write access of the - scientific parameters to a different group from the software and - hardware configuration parameters.\VER{TEST}{allocated} -\end{enumerate} +\subsubsection{AP Database} + +%% IPP AP DB Requirements +The IPP AP Database has the following performance requirements: + +\begin{enumerate} +\item The AP Database shall accept new detections at the rate + generated by the telescope from the Phase 2 and Phase 4 analysis. + Except within 10 degrees of the galactic plane, the AP Database + shall keep up with the incoming rates. The expected rates are + listed in Table~\ref{APrates}, along with the total data volume + required for storage space over the PS-1 lifetime.\VER{TEST}{TLR:2, + TLR:3, TLR:22} + +\item The AP Database shall provide access to external Pan-STARRS + clients to the detected transient objects within 15 minutes after + the image is obtained with an 85\% reliability.\VER{TEST}{TLR:22} + \label{IPP:DeReq:29c} +\end{enumerate} + +%%% Table: AP DB parameters +\begin{table}[hb] +\begin{center} +\caption{AP Detection Classes \& Object Parameters\label{APdetections}} +\begin{tabular}{lrrrr} +\hline +\hline +Object Parameter & P2 & P4$\Sigma$ & P4$\Delta$ & SS \\ +\hline +PSF x,y, covar, $\alpha,\delta$ & + & + & + & + \\ +PSF mag, $\sigma_{\rm mag}$ & + & + & + & + \\ +star/gal sep & + & + & + & + \\ +$\sigma_x$, $\sigma_y$, $\theta$ & + & + & + & + \\ +local sky data & + & + & + & + \\ +Petrosian R, M, $R_{50}$, $R_{90}$ & - & + & - & + \\ +S\'ersic R, M, AB, $\phi$, $\nu$ & - & + & - & + \\ +W.L. $\gamma_1$, $\gamma_2$, pol. terms & - & - & - & + \\ +exp. spaced aps., Poisson noise, variance & - & - & - & + \\ +\hline +\end{tabular} +\end{center} +\end{table} + +%%% Table: AP DB Throughput +\begin{table} +\begin{center} +\caption{AP Data Volume and Throughput Requirements\label{APrates}} +\begin{tabular}{lrrr} +\hline +\hline +Quantity & P2 & P4$\Sigma$ & P4$\Delta$ \\ +\hline +detection limit & $20 \sigma$ & $5 \sigma$ & $3 \sigma$ \\ +depth (r') & 21.8 & 24.0 & 24.5 \\ +bytes star$^{-1}$ & 64 & 100 & 64 \\ +stars deg$^{-2}$ ($|b|>10$) & $2.0 \times 10^5$ & $8.0 \times 10^5$ & $2.0 \times 10^5$ \\ +stars FPA$^{-1}$ ($|b|>10$) & $1.4 \times 10^6$ & $5.6 \times 10^6$ & $1.4 \times 10^6$ \\ +stars sec$^{-1}$ ($|b|>10$) & $3.5 \times 10^4$ & $3.5 \times 10^4$ & $8.8 \times 10^3$ \\ +MB sec$^{-1}$ & 2.3 & 3.5 & 0.6 \\ +AP total TB & 7.7 & - & - \\ +IVP total TB & 13 & 20 & 3 \\ +MOPS total TB & 4 & 6 & 1 \\ +PS-1 total TB & 25 & 26 & 4 \\ +\hline +\end{tabular} +\end{center} +\end{table} \subsubsection{Controller} @@ -810,10 +804,11 @@ \begin{enumerate} \item The IPP Science Analysis shall pre-process the science images - with the master calibration images at a sustained rate of 1 exposure - (2~GB) per \tbr{40 seconds}.\VER{TEST}{TLR:17} + with the master calibration images at a nightly average rate of 1 + exposure (2~GB) per 40 seconds.\VER{TEST}{TLR:17} \item The IPP Science Analysis shall merge multiple pre-processed science images into stacked images with corresponding signal-to-noise - maps at a sustained rate of 1 exposure (2~GB) per \tbr{40 seconds}.\VER{TEST}{TLR:17} + maps at a nightly average rate of 1 exposure (2~GB) per 40 + seconds.\VER{TEST}{TLR:17} \item The IPP Science Analysis shall excise pixels from the input @@ -823,11 +818,13 @@ \item The IPP Science Analysis shall merge the cleaned images into the static sky image, and update the corresponding exposure (S/N) maps, - at a sustained rate of 1 exposure (2~GB) per \tbr{40 seconds}.\VER{TEST}{TLR:17} + at a nightly average rate of 1 exposure (2~GB) per 40 + seconds.\VER{TEST}{TLR:17} \item The maximum latency between the acquisition of an image and the completion of the science image analysis is set by the science requirements of the fast transient recovery programs. The science - image analysis shall process images to detection transients within - \tbr{5 min} of their acquisition.\VER{TEST}{TLR:22} + image analysis shall process images to the detection of transients + within 15 min of their acquisition with an 85\% + reliability.\VER{TEST}{TLR:22} \item The science image analysis stages shall processes up to 1000 @@ -905,6 +902,4 @@ images which are not undersampled. \VER{TEST}{TLR:18} -\item The resulting astrometric solution shall be consistent across the - OTA field to within \tbr{100 milli-arcsec}.\VER{TEST}{TLR:4} \end{enumerate} @@ -926,15 +921,15 @@ resulting astrometric solution shall have a residual scatter of $< 30$ milliarcseconds when calibrated with the AP Survey reference - catalog and $< 100$ milliarcseconds when calibrated with the USNO-B - catalog.\VER{ANALYSIS}{TLR:} + catalog and $< 200$ milliarcseconds when calibrated with the USNO-B + catalog.\VER{ANALYSIS}{TLR:4} \item For images obtained under normal observing conditions, the - resulting astrometric solution shall have a precision relative to - ICRS of better than 100 milliarcseconds.\VER{ANALYSIS}{TLR:} + resulting astrometric solution shall have systematic errors relative + to ICRS of $< 100 milliarcseconds$.\VER{ANALYSIS}{TLR:3} \item For images obtained under photometric conditions or minimal cirrus conditions ($< 0.1$ mag total extinction), the resulting photometric calibration shall have a relative accuracy of 5 - millimagnitudes.\VER{ANALYSIS}{TLR:} + millimagnitudes.\VER{ANALYSIS}{TLR:1} \item For images obtained under photometric conditions or minimal @@ -942,5 +937,5 @@ photometric calibration shall have an absolution photometric accuracy of 10 millimagnitudes when calibrated relative to the AP - Survey reference catalog.\VER{ANALYSIS}{TLR:} + Survey reference catalog.\VER{ANALYSIS}{TLR:1} \item For images obtained under photometric conditions or minimal @@ -948,5 +943,5 @@ conditions listed in Table~\ref{moonconditions}, the resulting sky background subtraction shall leave behind peak-to-peak residuals $< - 1$\% of the input sky flux.\VER{ANALYSIS}{TLR:} + 1$\% of the input sky flux.\VER{ANALYSIS}{TLR:1} \end{enumerate} @@ -968,5 +963,5 @@ \item The sky representation shall degrade the image quality by less - than 10 milliarcseconds added in quadrature to the input image + than 150 milliarcseconds added in quadrature to the input image quality.\VER{TEST}{TLR:1} @@ -975,7 +970,9 @@ time. \VER{TEST}{TLR:17} -\item \tbd{completeness} - -\item \tbd{contamination} +\item The Phase 4 analysis shall have a transient detection + completeness of 99\% for detections with a significance $> 5\sigma$. + +\item The Phase 4 analysis shall have a false detection rate of $< + 5\%$ for transients detections with a significance $> 5\sigma$. \end{enumerate} @@ -1025,5 +1022,5 @@ The required set of Pan-STARRS modules and their functionality is specified in the document `Pan-STARRS Image Processing Pipeline Modules -Supplementary Design Requirements' (PSDC-430-xxx), and details of +Supplementary Design Requirements' (PSDC-430-012), and details of specific algorithms are specified in the document `Pan-STARRS Image Processing Pipeline Algorithm Design Document' (PSDC-430-006). @@ -1072,4 +1069,41 @@ \subsubsection{External Catalogs} +\begin{table} +\begin{center} +\caption{Astrometric Reference Catalogs\label{AstroRefs}} +\begin{tabular}{lrrrrl} +\hline +\hline +Name & scatter limit & proper & depth & Nstars & filters \\ + & (milliarcsec) & motion &(mag) & (millions) & \\ +\hline +Hipparcos & 1 & 2 & 7.3 & 0.1 & {\em V} \\ +Tycho2 & 10 & 1 & 11.5 & 2.5 & {\em B,V} \\ +UCAC-2 & 20 & 1 & 16.0 & 48.0 & {\em R} \\ +USNO-A2.0 & 250 & N/A & 19.0 & 526.2 & {\em B,R} \\ +USNO-B1.0 & 200 & 20 & 21.0 & 1042.6 & {\em B,R} \\ +2MASS & 70 & N/A & 16.0 & 470.0 & {\em J,H,K} \\ +\hline +\end{tabular} +\end{center} +\end{table} + +\begin{table} +\begin{center} +\caption{Photometric Reference Catalogs\label{PhotoRefs}} +\begin{tabular}{lrrr} +\hline +\hline +Name & scatter & depth & filters \\ + & mmag & mag & \\ +\hline +SDSS & 15 & 16 & {\em u,g,r,i,z} \\ +CFHT-LS & 10 & 18 & {\em u,g,r,i,z} \\ +Landolt & 10-20 & 15 & {\em U,B,V,R,I} \\ +\hline +\end{tabular} +\end{center} +\end{table} + The IPP AP Database shall be able to interact with the externally provided reference catalogs listed in Table~\ref{AstroRefs} and @@ -1078,5 +1112,6 @@ \subsubsection{Static Sky Pixel Size} -The IPP static sky shall have a pixel scale of \tbr{0.2\arcsec}. +The IPP static sky shall have a pixel scale of +0.2\arcsec.\VER{ANALYSIS}{TLR:16} \subsection{External Interfaces} @@ -1182,5 +1217,5 @@ \hline \hline -Raw data & 200 TB \\ +Raw data & 400 TB \\ static sky & 350 TB \\ calibration frames & 2.8 TB \\ @@ -1188,5 +1223,5 @@ AP db & 55 TB \\ \hline -total & 610 TB \\ +total & 810 TB \\ \hline \end{tabular} @@ -1204,10 +1239,9 @@ \begin{enumerate} \item The IPP shall store all raw images from the first year from the - AP and IVP surveys. This corresponds to 175,000 images, or 175 TB, - assuming 1 GB per image with compression. The IPP will require - space for 200 TB of raw imagery to store the data from these two - survey components along with raw calibration, test, and short-term - storage of other raw images not in the AP and IVP - surveys.\VER{INSPECT}{TLR:23} + AP and IVP surveys. This corresponds to 180,000 images, or 360 TB, + assuming 2 GB per image. The IPP will require space for 400 TB of + raw imagery to store the data from these two survey components along + with raw calibration, test, and short-term storage of other raw + images not in the AP and IVP surveys.\VER{INSPECT}{TLR:23} \item The IPP shall store a single copy of the complete static sky in @@ -1226,5 +1260,6 @@ represent at most 2 terabytes. \VER{INSPECT}{TLR:25} -\item The IPP shall have storage capacity for a total of 610 TB of data. +\item The IPP shall have storage capacity for a total of 810 TB of + data by the end of PS-1. \end{enumerate} @@ -1353,5 +1388,6 @@ %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% -\section{Appendices} +\clearpage +\appendix \bibliographystyle{plain}