\documentclass[panstarrs,spec]{panstarrs}

\title{IPP Commissioning Plan for PS-1} % put in your title
%\subtitle{Specification}
\author{Eugene Magnier}
\audience{Pan-STARRS Science}
\shorttitle{AP Survey Requirements}
\group{Pan-STARRS IPP}
\project{Pan-STARRS IPP}
\organization{Institute for Astronomy}
\version{DR}
\docnumber{PSDC-xxx-xxx}

\newcommand\ugriz{$u^\prime g^\prime r^\prime i^\prime z^\prime$}
\newcommand\grizy{$g r i z y$}

\begin{document}
\maketitle

\section{Overview}

The Pan-STARRS Image Processing Pipeline will undergo extensive
commissioning tests in the period September - December, 2006.  With
the staged arrival of the telescope, the first camera (TC-3) and
optics, and the main camera (GPC), the commissioning will take place
in a series of steps.  Initially, basic operating functionality will
be demonstrated along with analysis throughput, without specific focus
on achieving the final astrometric and photometric precision goals.
Eventually, with the arrival of the GPC, the complete system
requirements will be used as the commissioning criteria.

\section{Pipeline / Infrastructure tests with Megacam data}

Before actual camera hardware is delivered, the IPP will begin
commissioning tests related to the infrastructure and interfaces.
These commissioning tests may be performed with only a few IPP cluster
nodes in the IfA computer room before hardware is deployed to Maui.
Below, we list the commissioning tasks required to demonstrate the
working infrastructure of the IPP.

\begin{itemize}
\item {\bf PanTasks / ippTools / Analysis Programs interactions :
  Detrend Creation} The complete IPP pipelines for Phase 0 and the
  Detrend Creation steps should be installed and set up on the test
  cluster.  A complete megacam dataset must be run through the
  pipeline.  This dataset will consist of raw bias, dark, flat-field,
  and fringe images.  This commissioning task will demonstrate the
  creation of master detrend images from raw detrend images.

\item {\bf PanTasks / ippTools / Analysis Programs interactions :
  Phase 2} The complete IPP pipelines for Phase 2 should be installed
  and set up on the test cluster.  A complete megacam dataset must be
  run through the pipeline.  This dataset will consist of science
  images along with the master detrend images generated by the
  previous task.  This commissioning task will demonstrate the
  application of master detrend images to the raw science images and
  the analysis up to object detection and photometry. (Phase 1 - guide
  star analysis - is irrelevant to the Megacam test data).

\item {\bf PanTasks / ippTools / Analysis Programs interactions :
  Phase 3} The complete IPP pipelines for Phase 3 should be installed
  and set up on the test cluster.  A complete megacam dataset must be
  run through the pipeline.  This dataset will consist of science
  images along with the master detrend images generated by the
  previous task.  This commissioning task will extend the previous
  test to include astrometric calibration relative to the installed
  DVO database.  It will also demonstrate the operation of the
  photometric calibration relative to the DVO database, though the
  reference data will not be appropriate to judge the photometric
  results at this stage.

\item {\bf Camera - IPP Image transfer} Test GPC-1 images will be
  injected into the test IPP system using the Data Store mechanism.

\item {\bf Otis - IPP Images} Test ISP images will be injected into
  the test IPP system using the Data Store mechanism.

\item {\bf Otis - IPP Metadata} Test metadata tables will be passed to
the test IPP system using the Data Store mechanism.
\end{itemize}

\section{Camera in lab : Detrend Image Tests}

Before either camera is mounted on the telescope, as set of Camera-IPP
commissioning tasks may be performed using biases, darks, and
(depending on camera lab options) rough flat-field tests.  These
initial commissioning tests are performed before a bad pixel mask is
generated.  The tests are conditional on the bad pixels not
overwhelming the statistics.  The same tests should be re-performed
after the bad pixel mask has been built with data obtained on the
telescope.  When the mask is available, the success criteria can be
set to more stringent limits.

\subsection{Bias construction / application}

Obtain a stack of ($N > 10$) bias images.  Build a master bias and
generate residual images (automatically part of the detrend creation
system).  Examine the detrend creation Q/A statistics: residuals per
chip, residuals per frame, number of 5 sigma outlier pixels.

\subsection{Dark construction / application}

Obtain a stack of ($N > 10$) dark images for each of a range of
exposure times (15, 30, 60, 120, 240 seconds).  Build master darks and
generate residual images (automatically part of the detrend creation
system).  Examine the detrend creation Q/A statistics: residuals per
chip, residuals per frame, number of 5 sigma outlier pixels.  Model
the trend of average dark current vs exposure time.

\subsection{Rough Flat-field construction / application}

Obtain a stack of ($N > 10$) flat images for each of the filters with
a range of count levels.  Build master flats and generate residual
images (automatically part of the detrend creation system).  Examine
the detrend creation Q/A statistics: residuals per chip, residuals per
frame, number of 5 sigma outlier pixels.  Examine the amplitude of the
flat-field residual as a function of count level (accuracy of shutter
ballistics model, non-linearity).

\section{Camera on telescope : Detrend Image Tests}

\subsection{Bad Pixel Mask Construction}

Supply a series of flat-field images to the mask creation
tool. Examine the statistics of the flagged pixels, and examine the
coverage by eye.

\subsection{Basic Detrend Construction}

Rerun the tests above (bias, dark, flat) using data obtained on the
telescope, and applying the mask created above.

\subsection{Fringe master construction / application}

Obtain a stack of many potential input fringe images: night-time
images in the appropriate filters over a range of airmass and time of
night.  Build master fringe images and generate residual images
(automatically part of the detrend creation system).  Examine the
detrend creation Q/A statistics: residuals per chip, residuals per
frame, number of 5 sigma outlier pixels.  Examine the amplitude of the
fringe residual as a function of count level, airmass, etc.

\subsection{Non-linearity}

Measure the non-linearity by obtaining flat-field images with a range
of exposure times and flux levels.  Measure the non-linearity by
observing star fields with bright stars with a range of exposure times
from short to long exposures.

\subsection{additional detrend characterization tests}

\begin{itemize}

\item bias levels as a function of detector \& dome temperature

\item dark level as a function of dome light level

\item flat-field consistency as a function of illumination level:
   obtain a sequence of input flats for each filter over the entire
   twilight period.

\item flat-field consistency as a function of internal vs external
   illumination: obtain a sequence of input flats with dome shutters
   opened different amounts

\item flat-field consistency as a function of time: repeat the
   flat-field construction process over N (> 5) photometric nights

\item flat-field consistency as a function of solar angle: obtain a
   series of flat-field sequences at a range of Alt/Az positions (Az =
   0, 90, 180, 270; Alt = 45, 60, 80).

\end{itemize}

\subsection{Fringe construction tests}

\subsection{Fringe consistency tests}

\begin{itemize}
\item fringe as a function of time-of-night

\item fringe as a function of airmass

\item fringe as a function of lunation

\item fringe evolution twilight-to-nighttime
\end{itemize}

\subsection{Skyflat vs Domeflat comparison}

Build master detrend images using both dome and sky flats.  a 

input data: stack of N (5 - 10) skyflat images

process: build a master flat, generate residual images (automatically
part of the detrend creation system)

test: residuals per chip, residuals per frame < limit, number of
5 sigma outlier pixels.

\section{Astrometry and Photometry}

\subsection{Phase 2 / Phase 3 Astrometry solution tests}

\begin{itemize}
\item observe a high-quality astrometry field

\item astrometry convergence for a range of stellar densities

\item astrometry accuracy: perform a series of dithers and demonstrate
   the astrometry solution
\end{itemize}

\subsection{Build the Flat Correction Frames}

\begin{itemize}
\item dither sequence in dense stellar field

\item demonstrate photometric consistency within the dither pattern
\end{itemize}

\subsection{Photometry Calibration (Zero-Point) Checks}

measure zero-points (using photflat) on megacam standards fields

\section{Phase 4 Tests}

\section{AP Survey Preparation Tests / Research}

\subsection{Skyprobe Pre-AP Survey}

Skyprobe observations in all 5 filters over 6x8 patch takes 30 minutes
(45 seconds per point, one sweep in all filters).  The observable sky
in one night is $\sim 25,000$ square degrees (ie 15\% less than 3pi),
taking roughly 4500 pointings using the base overlaps.  The entire
observable sky can be observed in 47 hours, or about 5 x 9 hour
nights.

In the pre-TC-3 / TC-3 era, we can perform a complete sweep of the
observable sky every month. \note{dark half of the lunation only?}
Between Feb-Jun, we can obtain 5 complete passes, including at least 3
on even the portions which are in conjunction with the sun at some
point in these 5 months.  The cost would be 25 photometric nights
between Feb-Jun (16\% of the available nights).  This dataset will
allow us to:

\begin{itemize}
\item build a complete skyprobe photometry dataset for the full 3pi.

\item test the static sky construction process before GPC arrives.

\item study the transparency stability of the sky at Haleakala.
\end{itemize}

\section{Transparency / Airmass Tests}

we need to understand the stability of the atmosphere on Haleakala.
Two effects which must be distinguished are variations in the airmass
slope and the stochastic variations in the absolute transparency.

we can follow a single spot on the sky (eg, Dec = 0 or 35) from the
beginning of the night to the end of the night, for 9 - 11 full hours
of transit.  we can obtain a 30-second image continuously (expose,
readout, expose).  We need to do this on a photometric night (if the
weather deteriorates, break and do some other tests).  More than one
of these would be nice, at least one per filter.  the resulting
photometry will illustrate the transparency of the sky versus the
consistency of the airmass slope (thus, more than one night would be
good, esp for g').  The measurement does not need the best possible
flat-field image: keeping the position stationary reduces the
sensitivity to the flat-fielding.

To measure the stability of the atmosphere at high zenith angles, we
can sit on the north pole field for several hours on a photometric
night, performing 30 second continuous exposures.

These two experiments would cost 5-10 photometric nights.  They can
also be used to demonstrate the astrometric stability across a range
of image qualities (high-to-low airmass).

\end{document}
