Changeset 2192 for trunk/doc/design/ippSRS.tex

Timestamp:

Oct 21, 2004, 6:43:35 PM (22 years ago)

Author:

eugene

Message:

finished major revisions

File:

• trunk/doc/design/ippSRS.tex (modified) (17 diffs)

trunk/doc/design/ippSRS.tex

@@ -1 @@
- %%% $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 +180 @@
 
 \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 +265 @@
   \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 +795 @@
 \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 +949 @@
   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 +996 @@
 \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 +1007 @@
 
 \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 +1096 @@
 
 \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 +1112 @@
 
 \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 +1139 @@
 
 \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 +1199 @@
   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 +1217 @@
 
 \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 +1247 @@
   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 +1449 @@
 
 \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 +1490 @@
 
 \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 +1550 @@
 
 \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 +1672 @@
 \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}