Index: trunk/doc/release.2015/ps1.detrend/detrend.tex
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--- trunk/doc/release.2015/ps1.detrend/detrend.tex	(revision 40600)
+++ trunk/doc/release.2015/ps1.detrend/detrend.tex	(revision 40601)
@@ -133,39 +133,95 @@
 %% * check on total size vs arxiv limits
 
-\section{Introduction and Survey Description}
-
-This is the third in a series of seven papers describing the Pan-STARRS1
-Surveys,
-the data reduction techniques and the resulting data products. This paper (Paper III)
-describes the details of the pixel processing algorithms, including
-detrending, warping, adding (to create stacked images), and subtracting
-(to create difference images), along with the resulting image products and their
-properties.
-\citet[][Paper I]{chambers2017} provide an overview of the Pan-STARRS System, the
-design and execution of the Surveys, the resulting image and catalog data
-products, a discussion of the overall data quality and basic
-characteristics, and a brief summary of important results.
+\section{Introduction}
+
+The 1.8m Pan-STARRS\,1 telescope is located on the summit of Haleakala
+on the Hawaiian island of Maui.  The wide-field optical design of the
+telescope \citep{2004SPIE.5489..667H} produces a 3.3 degree field of view with
+low distortion and minimal vignetting even at the edges of the
+illuminated region.  The optics and natural seeing combine to yield
+good image quality: 75\% of the images have full-width half-max values
+less than (1.51, 1.39, 1.34, 1.27, 1.21) arcseconds for (\grizy), with
+a floor of $\sim 0.7$ arcseconds.
+
+The \PSONE\ camera \citep{2009amos.confE..40T}, known as GPC1, consists of a
+mosaic of 60 back-illuminated CCDs manufactured by Lincoln Laboratory.
+The CCDs each consist of an $8\times8$ grid of $590 \times 598$
+pixel readout regions, yielding an effective $4846 \times 4868$
+detector.  Initial performance assessments are presented in
+\cite{2008SPIE.7014E..0DO}.  Routine observations are conducted remotely from the
+Advanced Technology Research Center in Kula, the main facility of the
+University of Hawaii's Institute for Astronomy (IfA) operations on Maui.
+The Pan-STARRS1 filters and photometric system have already been
+described in detail in \cite{2012ApJ...750...99T}.
+
+For nearly 4 years, from 2010 May through 2014 March, this telescope
+was used to perform a collection of astronomical surveys under the
+aegis of the Pan-STARRS Science Consortium.  The majority of the time
+(56\%) was spent on surveying the $\frac{3}{4}$ of the sky north of
+$-30$ Declination with \grizy\ filters in the so-called $3\pi$ Survey.
+Another $\sim 25\%$ of the time was concentrated on repeated deep
+observations of 10 specific fields in the Medium-Deep Survey.  The
+rest of the time was used for several other surveys, including a
+search for potentially hazardous asteroids in our solar system.  The
+details of the telescope, surveys, and resulting science publications
+are described by \cite{chambers2017}.  The Pan-STARRS1 filters and
+photometric system has already been described in detail in
+\cite{2012ApJ...750...99T}.
+
+Pan-STARRS produced its first large-scale public data release, Data
+Release 1 (DR1) on 16 December 2016.  DR1 contains the results of the
+third full reduction of the Pan-STARRS $3\pi$ Survey archival data,
+identified as PV3.  Previous reductions \citep[PV0, PV1, PV2;
+  see][]{magnier2017.datasystem} were used internally for pipeline
+optimization and the development of the initial photometric and
+astrometric reference catalog \citep{magnier2017.calibration}.  The
+products from these reductions were not publicly released, but have
+been used to produce a wide range of scientific papers from the
+Pan-STARRS 1 Science Consortium members \citep{chambers2017}.  DR1
+contained only average information resulting from the many individual
+images obtained by the $3\pi$ Survey observations.  A second data
+release, DR2, was made available \note{20 January 2019}.  DR2 provides
+measurements from all of the individual exposures, and include an
+improved calibration of the PV3 processing of that dataset.
+
+This is the third in a series of seven papers describing the
+Pan-STARRS1 Surveys, the data reduction techniques and the resulting
+data products. This paper (Paper III) describes the details of the
+pixel processing algorithms, including detrending, warping, adding (to
+create stacked images), and subtracting (to create difference images),
+along with the resulting image products and their properties.
+
+%Chambers et al. 2017 (Paper I)
+%The Pan-STARRS\,1 Surveys
+\citet[][Paper I]{chambers2017} provide an overview of the Pan-STARRS
+System, the design and execution of the Surveys, the resulting image
+and catalog data products, a discussion of the overall data quality
+and basic characteristics, and a brief summary of important results.
+
 %Magnier et al. 2017 (Paper II)
 %Pan-STARRS Data Processing Stages
-\citet[][Paper II]{magnier2017.datasystem}
-describe how the various data processing stages are organized and
-implemented
-in the Imaging Processing Pipeline (IPP), including details of the
-the processing database which is a critical element in the IPP
-infrastructure.
+\citet[][Paper II]{magnier2017.datasystem} describe how the various
+data processing stages are organized and implemented in the Imaging
+Processing Pipeline (IPP), including details of the the processing
+database which is a critical element in the IPP infrastructure.
+
 %Waters et al. 2017 (Paper III)
 %Pan-STARRS Pixel Processing : Detrending, Warping, Stacking
 %\citet[][Paper III]{waters2017}
+% THIS PAPER
+
 %Magnier et al. 2017 (Paper IV)
 %Pan-STARRS Pixel Analysis : Source Detection
-\citet[][Paper IV]{magnier2017.analysis}
-describe the details of the source detection and photometry, including
-point-spread-function and extended source fitting models, and the
-techniques for ``forced'' photometry measurements.
+\citet[][Paper IV]{magnier2017.analysis} describe the details of the
+source detection and photometry, including point-spread-function and
+extended source fitting models, and the techniques for ``forced''
+photometry measurements.
+
 %Magnier et al. 2017 (Paper V)
 %Pan-STARRS Photometric and Astrometric Calibration
-\citet[][Paper V]{magnier2017.calibration}
-describe the final calibration process, and the resulting photometric and
-astrometric quality.
+\citet[][Paper V]{magnier2017.calibration} describe the final
+calibration process, and the resulting photometric and astrometric
+quality.
+
 %Flewelling et al. 2017 (Paper VI)
 %Pan-STARRS 1 Database and Data Products
@@ -173,15 +229,16 @@
 describe the details of the resulting catalog data and its organization
 in the Pan-STARRS database.
-%
-%
-\citet[][Paper VII]{huber2017}
+
 %Huber et al. 2017 (Paper VII)
-describe the Medium Deep Survey in detail, including the unique issues and
-data products specific to that survey. The Medium Deep Survey is not part
-of Data Release 1. (DR1)
-The Pan-STARRS1 filters and photometric system has already been described
-in detail in \cite{2012ApJ...750...99T}.
-
-The Pan-STARRS 1 Science Survey uses the 1.4 gigapixel GPC1 camera
+\citet[][Paper VII]{huber2017} describe the Medium Deep Survey in
+detail, including the unique issues and data products specific to that
+survey. The Medium Deep Survey is not part of Data Releases 1 or 2 and
+will be made available in a future data release.
+
+% \note{DS notes fonts are not consistent for keywords, etc}
+
+\section{Background}
+
+The Pan-STARRS 1 Science Survey used the 1.4 gigapixel GPC1 camera
 with the PS1 telescope on Haleakala Maui to image the sky north of
 $-30^\circ$ declination.  The GPC1 camera is composed of 60 orthogonal
@@ -193,17 +250,4 @@
 needed to ensure the response is consistent across the entire seven
 square degree field of view.
-
-\note{DS notes fonts are not consistent for keywords, etc}
-
-%The Processing Version 3 (PV3) reduction represents the third full
-DR1 contains the results of the third full reduction of the Pan-STARRS
-archival data, idenfied as PV3.  Previous reductions \citep[PV0, PV1,
-  PV2; see][]{magnier2017.datasystem}
-were used internally for pipeline optimization and the development of
-the initial photometric and astrometric reference catalog
-\citep{magnier2017.calibration}.  The products from these reductions
-were not publicly released, but have been used to produce a wide range
-of scientific papers from the Pan-STARRS 1 Science Consortium members
-\citep{chambers2017}.
 
 The Pan-STARRS image processing pipeline (IPP) is described elsewhere