Index: trunk/doc/release.2015/ps1.detrend/detrend.tex
===================================================================
--- trunk/doc/release.2015/ps1.detrend/detrend.tex	(revision 39850)
+++ trunk/doc/release.2015/ps1.detrend/detrend.tex	(revision 39852)
@@ -9,7 +9,11 @@
 %\documentclass[preprint2]{aastex}
 %\documentclass[preprint2,longabstract]{aastex}
+
 \RequirePackage{color}
 \input{astro.sty}
 %\usepackage{subcaption}
+%\usepackage{natbib}
+%\bibliographystyle{apj}
+%\bibliographystyle{plain}
 
 % online version may use color, but print version needs b/w
@@ -135,5 +139,5 @@
 reduction of the Pan-STARRS archival data.  The first two reductions
 were used internally for pipeline optimization and the development of
-the initial photometric and astrometric reference catalog \citep{ps1_reference_catalog}.  The
+the initial photometric and astrometric reference catalog \citep{magnier2017c}.  The
 products from these reductions were not publicly released, but have
 been used to produce a wide range of scientific papers from the
@@ -151,5 +155,5 @@
 
 The Pan-STARRS image processing pipeline (IPP) is described elsewhere
-\citep{MagnierKaiserChambers2006}, but a short summary follows.  The
+\citep{magnier2017a}, but a short summary follows.  The
 archive of raw exposures is stored on disk, with a database storing
 the metadata of exposure parameters.  For the PV3 processing, large
@@ -158,5 +162,5 @@
 This stage performs the image detrending (described below in section
 \ref{sec:detrending}), as well as the single epoch photometry
-\citep{MagnierXXY}, in parallel on the individual OTA device data.
+\citep{magnier2017b}, in parallel on the individual OTA device data.
 Following the \ippstage{chip} stage is the \ippstage{camera} stage, in
 which the astrometry and photometry for the entire exposure is
@@ -184,5 +188,5 @@
 objects detected in that to perform forced photometry on the
 individual \ippstage{warp} stage images.  The details of these stages
-are provided in \citet{MagnierXXY}.
+are provided in \citet{magnier2017b}.
 
 The same reduction procedure described above is also performed in real
@@ -195,5 +199,5 @@
 \ippstage{diff} stage.  This allows the ongoing solar system moving
 object search to identify candidates for follow up observations within
-24 hours of the initial set of observations \citep{WainscoatXXX}.
+24 hours of the initial set of observations \citep{2015IAUGA..2251124W}.
 
 Section \ref{sec:detrending} provides an overview of the detrending
@@ -753,10 +757,10 @@
 In addition to this flat field applied to the individual images, the
 ubercal process used to calibrate the database of all detections
-\citep{ubercal} constructs internal ``flat field'' corrections.
+\citep{2012ApJ...756..158S} constructs internal ``flat field'' corrections.
 Although a single set of image flat fields was used for the entire PV3
 survey, five separate ``seasons'' of database flat fields were needed
 to ensure proper calibration.  This indicates that the flat field
 response is not completely fixed in time.  More details on this
-process are contained in \citet{calibration}.
+process are contained in \citet{magnier2017c}.
 
 \subsection{Pattern correction}
@@ -1836,9 +1840,9 @@
 individual input exposures against the reference catalog.  Upon the
 conclusion of the survey, the entire set of detection catalogs is
-further re-calibrated in the ``ubercal'' process \citep{ubercal}.
+further re-calibrated in the ``ubercal'' process \citep{2012ApJ...756..158S}.
 This produces a more consistent calibration of each exposure across
 the entire region of the sky imaged.  This further calibration is not
 available at the time of stacking, and so there may be small residuals
-in the transparency values as a result of this \citet{calibration}.
+in the transparency values as a result of this \citet{magnier2017c}.
 
 %% \czwdraft{Nigel: 5. ``The ouput exposure time is set to the sum of the input exposure times.''
@@ -1885,5 +1889,5 @@
 With the flux normalization factors and target PSF chosen, the
 convolution kernels can be calculated for each image.  ISIS kernels
-\citep{ISIS_kernels} are used with FWHM values of 1.5, 3.0, and 6.0
+\citep{1998ApJ...503..325A} are used with FWHM values of 1.5, 3.0, and 6.0
 pixels and polynomial orders of 6, 4, and 2.  Regions around the
 sources identified in the input images are extracted, convolved with
@@ -2188,5 +2192,5 @@
 data values must first be made positive, which then sets the highest
 quantization sampling near the lowest values in the image.  Following
-techniques used by SDSS \citep{sdss}, we have instead opted to use the
+techniques used by SDSS \citep{2000AJ....120.1579Y}, we have instead opted to use the
 inverse hyperbolic sine function to transform the data.  The domain of
 this function allows any input value to be converted.  In addition,
@@ -2309,5 +2313,5 @@
 sources that are not static between the two images leave a significant
 remnant.  More information on the difference image construction is
-contained in \citet{pauls_diff_paper}.  The follow section contains a
+contained in \citet{price2017}.  The follow section contains a
 overview of the difference image construction used for the data in
 DR2.
@@ -2332,5 +2336,5 @@
 
 For warp-warp differences, such as those used for the ongoing Solar
-System moving object search in nightly observations \citep{MOPS}, the
+System moving object search in nightly observations \citep{2013PASP..125..357D}, the
 warp that was taken first is used as the template.  As there is less
 certainty in which of the two input images will have better seeing, a
@@ -2351,5 +2355,5 @@
 on ensuring that the telescope pointings are as close to identical as
 possible.  The observing strategy to enable this is discussed in more
-detail in \citet{paper1}.
+detail in \citet{chambers2017}.
 
 
@@ -2465,4 +2469,6 @@
 University (ELTE), and the Los Alamos National Laboratory.
 
+%\bibliography{lib}{}
+
 
 \end{document}