Index: trunk/doc/release.2015/ps1.analysis/analysis.tex
===================================================================
--- trunk/doc/release.2015/ps1.analysis/analysis.tex	(revision 39974)
+++ trunk/doc/release.2015/ps1.analysis/analysis.tex	(revision 40069)
@@ -1,3 +1,4 @@
 \documentclass[iop,floatfix]{emulateapj}
+% \documentclass[10pt,preprint]{aastex}
 % \pdfoutput=1
 
@@ -5,8 +6,7 @@
 \RequirePackage{color}
 \RequirePackage{code}
-\RequirePackage{url}
 \input{astro.sty}
 
-\DeclareUrlCommand\email{\urlstyle{rm}}
+\usepackage[T1]{fontenc}% (2) specify encoding
 
 % online version may use color, but print version needs b/w
@@ -106,17 +106,17 @@
 \section{INTRODUCTION}\label{sec:intro}
 
-\begin{verbatim}
-here is a list of things to do:
-* clear out \note entries
-  * explain use of covariance
-  * add example for sky model
-  * Kaiser optimal detection reference
-  * find a brighter-fatter reference
-* define more tests and generate examples
-  * simulation example of background subtraction
-    at different densities
-  * real example of oversubtracted galaxy
-* check all references
-\end{verbatim}
+% \begin{verbatim}
+% here is a list of things to do:
+% * clear out \note entries
+%   * explain use of covariance
+%   * add example for sky model
+%   * Kaiser optimal detection reference
+%   * find a brighter-fatter reference
+% * define more tests and generate examples
+%   * simulation example of background subtraction
+%     at different densities
+%   * real example of oversubtracted galaxy
+% * check all references
+% \end{verbatim}
 
 This is the fourth in a series of seven papers describing the
@@ -126,8 +126,4 @@
 extended source model fitting, and the techniques for ``forced''
 photometry measurements.
-
-\url{http://eugene@ifa.hawaii.edu}
-
-\end{document}
 
 %Chambers et al. 2017 (Paper I)
@@ -141,5 +137,5 @@
 %Magnier et al. 2017 (Paper II)
 %Pan-STARRS Data Processing Stages
-\citet[][Paper II]{magnier2017c}
+\citet[][Paper II]{magnier2017.datasystem}
 describes how the various data processing stages are organised and implemented
 in the Imaging Processing Pipeline (IPP), including details of the 
@@ -154,10 +150,10 @@
 %Magnier et al. 2017 (Paper IV) 
 %Pan-STARRS Pixel Analysis : Source Detection 
-%\citet[][Paper IV]{magnier2017a}
+%\citet[][Paper IV]{magnier2017.analysis}
 %describes 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]{magnier2017b}
+\citet[][Paper V]{magnier2017.calibration}
 describes the final calibration process, and the resulting photometric and astrometric quality.  
 
@@ -446,5 +442,5 @@
 keyword which in turn specifies the value in the image header.  In the
 case of PS1 PV3, the header keyword \code{MAXLIN} specifies the
-saturation level for each chip (see \cite{waters2017}). 2) Pixels
+saturation level for each chip \citep[see][]{waters2017}. 2) Pixels
 which are below a user-defined value are considered unresponsive and
 masked as dead.  (camera format keyword \code{CELL.BAD} = 0 for PS1
@@ -453,6 +449,6 @@
 invalid.  (\code{psphot} recipe keywords \code{XMIN}, \code{XMAX},
 \code{YMIN}, \code{YMAX}, all set to 0 for PS1 PV3 -- invalid pixels
-were specified for PS1 PV3 with a supplied mask image, see
-\cite{waters2017}.
+were specified for PS1 PV3 with a supplied mask image
+\citep[see][]{waters2017}.
 
 The library functions used by \code{psphot} understand two types of
@@ -469,6 +465,6 @@
 
 \begin{table*}
-\caption{\label{tab:mask_values} \nocode{psphot} / GPC1 Mask Image Pixel Values}\vspace{-0.5cm}
 \begin{center}
+\caption{\label{tab:mask_values} \nocode{psphot} / GPC1 Mask Image Pixel Values} % \vspace{-0.5cm}
 \begin{tabular}{lcl}
 \hline