Index: trunk/doc/design/ippSRS.tex =================================================================== --- trunk/doc/design/ippSRS.tex (revision 2186) +++ trunk/doc/design/ippSRS.tex (revision 2192) @@ -1,3 +1,3 @@ - %%% $Id: ippSRS.tex,v 1.10 2004-10-21 03:55:59 eugene Exp $ + %%% $Id: ippSRS.tex,v 1.11 2004-10-22 04:43:35 eugene Exp $ \documentclass[panstarrs,spec]{panstarrs} @@ -180,78 +180,84 @@ \begin{enumerate} -\item For images obtained in photometric weather, produce reduced - science images for each full camera exposure with photometric - zero-point scatter less than 1\% across the full - field. \VER{ANALYSIS}{SCD:3.2.2.5} +\item For images obtained in photometric weather with normal detector + characteristics and providing appropriate flat-field images and + correction data have been obtained, the IPP shall produce reduced + science images for each full camera exposure with relative + photometric zero-point scatter less than 1\% ($1 \sigma$) across the + full field. \VER{ANALYSIS}{SCD:3.2.2.5} \label{TLR:1} -\item For images obtained in photometric weather, produce reduced - science images for each full camera exposure which are - photometrically calibrated with respect to the Pan-STARRS filter - system with a 1$\sigma$ accuracy of 1\%.\VER{ANALYSIS}{SCD:3.2.2.5} +\item For images of reference fields calibrated for the IPP filter set + and obtained in photometric weather with normal detector + characteristics and providing appropriate flat-field images and + correction data have been obtained, the IPP shall determine and + track zero-points for these exposures with a 1$\sigma$ accuracy of + 1\%.\VER{ANALYSIS}{SCD:3.2.2.5} \label{TLR:2} \item For images obtained under normal seeing conditions and optical - distortion, produce reduced science images for each full camera - exposure with an astrometric calibration providing $< 30$ - milliarcsecond scatter (1$\sigma$) for sequential images of the same - location.\VER{ANALYSIS}{SCD:3.2.2.7} + distortion, the IPP shall produce reduced science images for each + full camera exposure with an astrometric calibration providing $< + 30$ milliarcsecond scatter (1$\sigma$) for sequential images of the + same location.\VER{ANALYSIS}{SCD:3.2.2.7} \label{TLR:4} \item For images obtained under normal seeing conditions and optical - distortion, produce reduced science images for each full camera - exposure with an astrometric calibration providing $< 100$ - milliarcsecond scatter (1$\sigma$) relative to the ICRS reference - system.\VER{ANALYSIS}{SCD:3.2.2.6} + distortion, the IPP shall produce reduced science images for each + full camera exposure with an astrometric calibration providing $< + 100$ milliarcsecond scatter (1$\sigma$) relative to the ICRS + reference system.\VER{ANALYSIS}{SCD:3.2.2.6} \label{TLR:3} \item In photometric weather and under moon conditions listed in - Table~\ref{moonconditions}, produce reduced science images for each - full camera exposure which have background variations of less than - 1\% in regions free of large ($> 30$ pixels diameter) astronomical - structures.\VER{ANALYSIS}{SCD:3.5.12} + Table~\ref{moonconditions}, the IPP shall produce reduced science + images for each full camera exposure which have background + variations of less than 1\% in regions free of large ($> 30$ pixels + diameter) astronomical structures.\VER{ANALYSIS}{SCD:3.5.12} \label{TLR:5} -\item In photometric weather, produce reduced science images for each - full camera exposure which have background deviations from the - static sky in the same filter of less than 1\% for the median in - large ($> 30$ pixels diameter) regions.\VER{ANALYSIS}{SCD:3.5.12} +\item In photometric weather, the IPP shall produce reduced science + images for each full camera exposure which have background + deviations from the static sky in the same filter of less than 1\% + for the median in large ($> 30$ pixels diameter) + regions.\VER{ANALYSIS}{SCD:3.5.12} \label{TLR:5a} -\item Merge all $g$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} +\item The IPP shall merge all $g$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} \label{TLR:6} -\item Merge all $r$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} +\item The IPP shall merge all $r$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} \label{TLR:7} -\item Merge all $i$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} +\item The IPP shall merge all $i$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} \label{TLR:8} -\item Merge all $z$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} +\item The IPP shall merge all $z$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} \label{TLR:9} -\item Merge all $y$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} +\item The IPP shall merge all $y$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} \label{TLR:10} -\item Merge all $w$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} +\item The IPP shall merge all $w$ filter science images into a static sky image.\VER{TASK}{SCD:3.2.2.10} \label{TLR:11} -\item Detect and classify objects on the individual processed science +\item The IPP shall detect and classify objects on the individual processed science images.\VER{TASK}{SCD:3.2.2.16} \label{TLR:12} -\item Detect and classify objects on the stacked groups of science - images.\VER{TASK}{SCD:3.2.2.16} +\item The IPP shall detect and classify objects on the stacked groups + of science images.\VER{TASK}{SCD:3.2.2.16} \label{TLR:13} -\item Detect and classify objects on the static sky image.\VER{TASK}{SCD:3.2.2.16} +\item The IPP shall detect and classify objects on the static sky + image.\VER{TASK}{SCD:3.2.2.16} \label{TLR:14} -\item Detect transients with significance $>3\sigma$ in the individual - science images relative to the static sky +\item The IPP shall detect transients with significance $>3\sigma$ in + the individual science images relative to the static sky image.\VER{ANALYSIS}{SCD:3.2.2.16} \label{TLR:15} -\item Degrade the stacked image by no more than \tbr{10 +\item The IPP shall degrade the stacked image by no more than \tbr{10 milliarcseconds (FWHM added in quadrature)} over the theoretical limit for the stack under infinite @@ -259,50 +265,52 @@ \label{TLR:16} -\item 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 +\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 requirement).\VER{TEST}{SCD:3.2.2.3} \label{TLR:17} -\item Limit the \tbr{false alarm rate (FAR) to less than 5\%} for - transient detections $> 5\sigma$ sent to the preferred client +\item The IPP shall limit the false alarm rate (FAR) to less than 5\% + for transient detections $> 5\sigma$ sent to the preferred client science pipelines.\footnote{note difference with PS-4: 1\%} \VER{ANALYSIS}{SCD:3.2.2.13} \label{TLR:18} -\item Perform \tbr{transient detection to a completeness of 99\%} at - the completeness for transient detections with a significant $> - 5\sigma$.\VER{ANALYSIS}{SCD:xxx} - -\item Publish the static sky images to the Pan-STARRS Published - Science Products Subsystem (PSPS) once per \tbr{6 - months}.\VER{TASK}{SCD:3.2.2.18} +\item The IPP shall perform transient detection to a completeness of + 99\% at the completeness for transient detections with a significant + $> 5\sigma$.\VER{ANALYSIS}{SCD:xxx} + +\item The IPP shall publish the static sky images to the Pan-STARRS + Published Science Products Subsystem (PSPS) at a rate so the full + sky is transmitted once per year.\VER{TASK}{SCD:3.2.2.18} \label{TLR:19} -\item Publish the detected objects to the Pan-STARRS Published Science - Products Subsystem (PSPS) once per month.\VER{TASK}{SCD:3.2.2.18} +\item The IPP shall publish the detected objects to the Pan-STARRS + Published Science Products Subsystem (PSPS) at a rate such that the + objects from the full sky are transmitted once per + year.\VER{TASK}{SCD:3.2.2.18} \label{TLR:20} -\item Send the IPP metadata and received OTIS metadata to the - Pan-STARRS Published Science Products Subsystem (PSPS) +\item The IPP shall send the IPP metadata and received OTIS metadata + to the Pan-STARRS Published Science Products Subsystem (PSPS) weekly.\VER{TASK}{SCD:3.2.2.18} \label{TLR:21} -\item Provide access to preferred Pan-STARRS science clients to the +\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} \label{TLR:22} -\item Provide sufficent storage volume for raw images from the AP and +\item The IPP shall provide sufficent storage volume for raw images from the AP and IVP Surveys and the \grizy\ Static Sky.\footnote{note difference with PS-4: 1 month of raw images} \VER{INSPECT}{allocated} \label{TLR:23} -\item Provide sufficient storage volume for all detections from the +\item The IPP shall provide sufficient storage volume for all detections from the AP, IVP, and MVP Surveys.\footnote{note difference with PS-4: 1 year of detections}\VER{INSPECT}{allocated} \label{TLR:24} -\item Provide sufficient storage volume for 2 years of +\item The IPP shall provide sufficient storage volume for 2 years of metadata.\footnote{note difference with PS-4: 10 years of metadata}\VER{INSPECT}{allocated} @@ -787,8 +795,9 @@ \item The AP Database shall accept new detections at the rate generated by the telescope from the Phase 2 and Phase 4 analysis. - \tbr{Except within 10 degrees of the galactic plane, the AP Database - shall keep up with the incoming rates.} The expected rates are + 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} + 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 @@ -940,13 +949,13 @@ computers.\VER{TEST}{TLR:17} -\item The IPP Controller shall limit command latency to \tbr{$< 0.1$} seconds.\VER{TEST}{TLR:17} - -\item The IPP Controller shall be capable of performing up to \tbr{10 tasks per second}.\VER{TEST}{TLR:17} - -\item The IPP Controller shall be capable of buffering up to a total of \tbr{64 MB} of messages.\VER{TEST}{TLR:17} - -\item The IPP Controller shall be capable of executing up to \tbr{6 million tasks per month}.\VER{TEST}{TLR:17} - -\item The IPP Controller shall be capable of interacting with up to \tbr{256} client processes.\VER{TEST}{TLR:17} +\item The IPP Controller shall limit command latency to $< 0.1$ seconds.\VER{TEST}{TLR:17} + +\item The IPP Controller shall be capable of performing up to 10 tasks per second.\VER{TEST}{TLR:17} + +\item The IPP Controller shall be capable of buffering up to a total of 64 MB of messages.\VER{TEST}{TLR:17} + +\item The IPP Controller shall be capable of executing up to 6 million tasks per month.\VER{TEST}{TLR:17} + +\item The IPP Controller shall be capable of interacting with up to 256 client processes.\VER{TEST}{TLR:17} \item The IPP Controller shall be capable of accepting up to 2 non-client (external) requests per second.\VER{TEST}{TLR:17} @@ -987,9 +996,10 @@ \begin{enumerate} \item The IPP Scheduler shall publish the static sky images to the - Pan-STARRS PSPS on a time-scale of \tbr{6 month}.\VER{TEST}{TLR:19} + Pan-STARRS PSPS at a rate so that the full sky is transmitted once + per year.\VER{TEST}{TLR:19} \item The IPP Scheduler shall query the Databases on a regular basis to check for new input information. These queries shall take place - at least once every \tbr{1 seconds}.\VER{TEST}{TLR:17} + at least once every second.\VER{TEST}{TLR:17} \item The IPP Scheduler shall accept new User input in real-time: @@ -997,8 +1007,9 @@ \item The IPP Scheduler shall publish the detected objects to the - Pan-STARRS PSPS on a time-scale of \tbr{1 month}.\VER{TEST}{TLR:20} + Pan-STARRS PSPS at a rate so that the objects from the full sky are + transmitted once per year.\VER{TEST}{TLR:20} \item The IPP Scheduler shall publish the IPP and OTIS metadata to the - Pan-STARRS PSPS on a time-scale of \tbr{1 week}.\VER{TEST}{TLR:21} + Pan-STARRS PSPS on a time-scale of 1 week.\VER{TEST}{TLR:21} \item The IPP Scheduler shall send the detected single-occurance @@ -1085,6 +1096,6 @@ \item Calculate the Image cell / Sky cell overlaps for each image. - Sky cells which do not have sufficient science image overlap \tbr{$< - 5\%$} are excluded from the overlap table. + Sky cells which do not have sufficient science image overlap $< 5\%$ + are excluded from the overlap table. \end{itemize} @@ -1101,10 +1112,10 @@ \item Bright-star extraction from the image data shall be performed in - less than \tbr{1 second}.\VER{TEST}{TLR:17} + less than 1 second.\VER{TEST}{TLR:17} \item In order for blind astrometry of an image to succeed, it is necessary that approximate image coordinates be known. The Phase 1 analysis shall succeed despite initial coordinate errors as large as - \tbr{20\arcsec}.\VER{TEST}{TLR:3} + 20\arcsec.\VER{TEST}{TLR:3} \end{enumerate} @@ -1128,5 +1139,5 @@ \item Mask ghosts of bright stars which introduce residual feature - more significant than \tbr{1\%} of the background. + more significant than 1\% of the background. \item Bias subtract the image. @@ -1188,6 +1199,6 @@ time. \VER{TEST}{TLR:17} -\item The bias subtraction shall leave no residuals greater than - \tbr{1 DN} peak-to-peak for images within the normal range of bias +\item The bias subtraction shall leave no residuals greater than 1 DN + peak-to-peak for images within the normal range of bias variations.\VER{TEST}{TLR:1} @@ -1206,9 +1217,10 @@ \item The background residuals shall have peak-to-peak variations of - less than \tbr{1\%} of the input background amplitude.\VER{ANALYSIS}{TLR:5} - -\item The background residuals shall have a scatter of less than - \tbr{1\%} of the input background amplitude for apertures of less - than \tbr{10 arcsec}.\VER{ANALYSIS}{TLR:1} + less than 1\% of the input background + amplitude.\VER{ANALYSIS}{TLR:5} + +\item The background residuals shall have a scatter of less than 1\% + of the input background amplitude for apertures of less than 10 + arcsec.\VER{ANALYSIS}{TLR:1} \item The Phase 2 analysis shall detect cosmic rays with flux $> 5\sigma$ by @@ -1235,6 +1247,6 @@ photometric zero point and zero-point variations across the field. -\item If zero-point variations are significant (\tbr{$> 0.01$ mag - peak-to-peak}), the zero-point variations are modeled with a +\item If zero-point variations are significant ($> 0.01$ mag + peak-to-peak), the zero-point variations are modeled with a polynomial correction of order 3 or less. @@ -1437,9 +1449,10 @@ \begin{enumerate} -\item The IPP Calibration Analysis shall produce master calibration images -from the raw calibration images in less \tbr{2 hours}.\VER{TEST}{TLR:17, TLR:22} +\item The IPP Calibration Analysis shall produce master calibration + images from the raw calibration images in less 2 + hours.\VER{TEST}{TLR:17, TLR:22} \item Master calibration images shall not introduce systematic - uncertainties in the photometry greater than \tbr{0.2\%}.\VER{TEST}{TLR:1} + uncertainties in the photometry greater than 0.2\%.\VER{TEST}{TLR:1} \end{enumerate} @@ -1477,6 +1490,5 @@ \item The Dark calibration stage raises an error if the input images - have exposure times which deviate by more than - \tbr{2\%}. + have exposure times which deviate by more than 2\%. \item The Dark calibration stage corrects the input dark images for @@ -1538,10 +1550,10 @@ \item The Mask calibration stage masks the pixels which are - inconsistent in the input flats by more than \tbr{1\%}, given - sufficient signal-to-noise in the input flats. + inconsistent in the input flats by more than 1\%, given sufficient + signal-to-noise in the input flats. \item The Mask calibration stage mask the pixels which are consistently low or high in the input flats by more than a factor of - \tbr{3} beyond the typical pixel. + 3 beyond the typical pixel. \item The Mask calibration stage masks the pixels identified in a @@ -1660,5 +1672,5 @@ \item The IPP Calibration system monitors changes in the telescope astrometry parameters and issue a warning if the parameters change - by more than \tbr{2\%}. + by more than 2\%. \end{itemize}