Changeset 41401

Timestamp:

Aug 15, 2020, 10:41:44 AM (6 years ago)

Author:

eugene

Message:

finished revisions for referee

Location:

trunk/doc/release.2015/ps1.dataproducts

Files:

• dataproducts.bib (modified) (1 diff)
• dataproducts.tex (modified) (157 diffs)
• fundamentalipp.tex (modified) (1 diff)
• objid.pdf (modified) ( previous)
• objid.tex (modified) (1 diff)
• pspstables.tex (modified) (1 diff)
• report.v0.txt (modified) (10 diffs)

trunk/doc/release.2015/ps1.dataproducts/dataproducts.bib

@@ -629 +629 @@
 address = {Los Alamitos, CA, USA},
 }
+
+@ARTICLE{Szalay2002,
+       author = {{Szalay}, Alexander S. and {Gray}, Jim and {Thakar}, Ani R. and
+         {Kunszt}, Peter Z. and {Malik}, Tanu and {Raddick}, Jordan and
+         {Stoughton}, Christopher and {vandenBerg}, Jan},
+        title = "{The SDSS SkyServer: Public Access to the Sloan Digital Sky Server Data}",
+      journal = {arXiv e-prints},
+     keywords = {Computer Science - Digital Libraries, Computer Science - Databases, H.3.7, H.3.5, H.2, H.3, H.4, H.5},
+         year = 2002,
+        month = feb,
+          eid = {cs/0202013},
+        pages = {cs/0202013},
+archivePrefix = {arXiv},
+       eprint = {cs/0202013},
+ primaryClass = {cs.DL},
+       adsurl = {https://ui.adsabs.harvard.edu/abs/2002cs........2013S},
+      adsnote = {Provided by the SAO/NASA Astrophysics Data System}
+}
+
+@ARTICLE{Gray2002,
+       author = {{Gray}, Jim and {Szalay}, Alex S. and {Thakar}, Ani R. and
+         {Kunszt}, Peter Z. and {Stoughton}, Christopher and {Slutz}, Don and {vand
+        enBerg}, Jan},
+        title = "{Data Mining the SDSS SkyServer Database}",
+      journal = {arXiv e-prints},
+     keywords = {Computer Science - Databases, Computer Science - Digital Libraries, H.2.8, H.3.3, H.3.5, h.3.7, H.4.2},
+         year = 2002,
+        month = feb,
+          eid = {cs/0202014},
+        pages = {cs/0202014},
+archivePrefix = {arXiv},
+       eprint = {cs/0202014},
+ primaryClass = {cs.DB},
+       adsurl = {https://ui.adsabs.harvard.edu/abs/2002cs........2014G},
+      adsnote = {Provided by the SAO/NASA Astrophysics Data System}
+}
+
+                  
+
+
+
+
+
+
+
+
+
+

trunk/doc/release.2015/ps1.dataproducts/dataproducts.tex

@@ -50 +50 @@
 \newcommand\showfigure[1]{\input{#1}}
 %\newcommand\showfigure[1]{}
+
+\newcommand\Sersic{S{\'e}rsic}
 
 \def\Ha{H{$\alpha$}}
@@ -110 +112 @@
 \shortauthors{H. A. Flewelling}
 
+\def\IfA{1}
+\def\CFHT{2}
+\def\BackYard{3}
+\def\STSCI{4}
+\def\Google{5}
+\def\MPE{6}
+\def\SpireGlobal{7}
+\def\DUR{8}
+\def\DurComp{9}
+\def\DurCEA{10}
+\def\JHU{11}
+\def\Princeton{12}
 
 \begin{document}
 \title{The Pan-STARRS1 Database and Data Products}
 \author{
-H.~A.~Flewelling\altaffilmark{1}, 
-E.~A.~Magnier\altaffilmark{1}, 
-K.~C.~Chambers\altaffilmark{1},
-J.~N.~Heasley\altaffilmark{8},
-C.~Holmberg\altaffilmark{1},
-M.~E.~Huber\altaffilmark{1},
-W.~Sweeney\altaffilmark{1}, 
-C.~Z.~Waters\altaffilmark{1},
-A.~Calamida\altaffilmark{4},
-S.~Casertano\altaffilmark{4},
-X.~Chen\altaffilmark{10},
-D.~Farrow\altaffilmark{5}
-G.~Hasinger\altaffilmark{1},
-R.~Henderson\altaffilmark{11},
-K.~S.~Long\altaffilmark{4},
-N.~Metcalfe\altaffilmark{2},
-G.~Narayan\altaffilmark{4},
-M.~A.~Nieto-Santisteban\altaffilmark{4},
-P.~Norberg\altaffilmark{6,7},
-A.~Rest\altaffilmark{4},
-R.~P.~Saglia\altaffilmark{5},
-A.~Szalay\altaffilmark{3},
-A.~R.~Thakar\altaffilmark{3},
-J.~L.~Tonry\altaffilmark{1}, 
-J.~Valenti\altaffilmark{4},
-S.~Werner\altaffilmark{3},
-R.~White\altaffilmark{4},
+H.~A.~Flewelling\altaffilmark{\IfA,\CFHT}, 
+E.~A.~Magnier\altaffilmark{\IfA}, 
+K.~C.~Chambers\altaffilmark{\IfA},
+J.~N.~Heasley\altaffilmark{\BackYard},
+C.~Holmberg\altaffilmark{\IfA},
+M.~E.~Huber\altaffilmark{\IfA},
+W.~Sweeney\altaffilmark{\IfA}, 
+C.~Z.~Waters\altaffilmark{\IfA},
+A.~Calamida\altaffilmark{\STSCI},
+S.~Casertano\altaffilmark{\STSCI},
+X.~Chen\altaffilmark{\Google},
+D.~Farrow\altaffilmark{\MPE}
+G.~Hasinger\altaffilmark{\IfA},
+R.~Henderson\altaffilmark{\SpireGlobal},
+K.~S.~Long\altaffilmark{\STSCI},
+N.~Metcalfe\altaffilmark{\DUR},
+G.~Narayan\altaffilmark{\STSCI},
+M.~A.~Nieto-Santisteban\altaffilmark{\STSCI},
+P.~Norberg\altaffilmark{\DurComp,\DurCEA},
+A.~Rest\altaffilmark{\STSCI},
+R.~P.~Saglia\altaffilmark{\MPE},
+A.~Szalay\altaffilmark{\JHU},
+A.~R.~Thakar\altaffilmark{\JHU},
+J.~L.~Tonry\altaffilmark{\IfA}, 
+J.~Valenti\altaffilmark{\STSCI},
+S.~Werner\altaffilmark{\JHU},
+R.~White\altaffilmark{\STSCI},
 %
-L.~Denneau\altaffilmark{1},
-P.~W.~Draper\altaffilmark{2},
-K.~W.~Hodapp\altaffilmark{1},
-R.~Jedicke\altaffilmark{1},
-N.~Kaiser\altaffilmark{1},
-R.~P.~Kudritzki\altaffilmark{1},
-P.~A.~Price\altaffilmark{9},
-R.~J.~Wainscoat\altaffilmark{1},
-% P.~S.~Builders\altaffilmark{PS1},
-S.~Chastel\altaffilmark{1},
-B.~McLean\altaffilmark{4},
-M.~Postman\altaffilmark{4},
-B.~Shiao\altaffilmark{4}.
+L.~Denneau\altaffilmark{\IfA},
+P.~W.~Draper\altaffilmark{\DUR},
+K.~W.~Hodapp\altaffilmark{\IfA},
+R.~Jedicke\altaffilmark{\IfA},
+N.~Kaiser\altaffilmark{\IfA},
+R.~P.~Kudritzki\altaffilmark{\IfA},
+P.~A.~Price\altaffilmark{\Princeton},
+R.~J.~Wainscoat\altaffilmark{\IfA},
+%
+S.~Chastel\altaffilmark{\IfA},
+B.~McLean\altaffilmark{\STSCI},
+M.~Postman\altaffilmark{\STSCI},
+B.~Shiao\altaffilmark{\STSCI}.
 }
 
-
-
-\altaffiltext{1}{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, Hawaii 96822, USA}
-\altaffiltext{2}{Department of Physics, Durham University, South Road, Durham DH1 3LE, UK}
-\altaffiltext{6}{Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK}
-\altaffiltext{7}{Centre for Extragalactic Astronomy,  Department of Physics, Durham University, South Road, Durham DH1 3LE, UK}
-\altaffiltext{3}{Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA}
-\altaffiltext{4}{Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA}
-\altaffiltext{5}{ Max-Planck Institut f\"ur extraterrestrische Physik, Giessenbachstra\ss e 1, D-85748 Garching, Germany}
-\altaffiltext{8}{Back Yard Observatory, P.O. BOX 68856, Tucson, AZ 85737}
-\altaffiltext{9}{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA}
-\altaffiltext{10}{Google Inc., 1600 Amphitheatre Pkwy, Mountain View, CA 94043}
-\altaffiltext{11}{Spire Global, Sky Park 5,45 Finnieston Street, Glasgow, G3 8JU, UK }
+\altaffiltext{\IfA}{Institute for Astronomy, University of Hawai`i, 2680 Woodlawn Drive, Honolulu, Hawai`i 96822, USA}
+\altaffiltext{\CFHT}{Canada-France-Hawai`i Telescope, 65-1238 Mamalahoa Hwy, Kamuela, HI  96743, USA}
+\altaffiltext{\BackYard}{Back Yard Observatory, P.O. BOX 68856, Tucson, AZ 85737}
+\altaffiltext{\STSCI}{Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA}
+\altaffiltext{\Google}{Google Inc., 1600 Amphitheatre Pkwy, Mountain View, CA 94043}
+\altaffiltext{\MPE}{Max-Planck Institut f\"ur extraterrestrische Physik, Giessenbachstra\ss e 1, D-85748 Garching, Germany}
+\altaffiltext{\SpireGlobal}{Spire Global, Sky Park 5,45 Finnieston Street, Glasgow, G3 8JU, UK }
+\altaffiltext{\DUR}{Department of Physics, Durham University, South Road, Durham DH1 3LE, UK}
+\altaffiltext{\DurComp}{Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK}
+\altaffiltext{\DurCEA}{Centre for Extragalactic Astronomy,  Department of Physics, Durham University, South Road, Durham DH1 3LE, UK}
+\altaffiltext{\JHU}{Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA}
+\altaffiltext{\Princeton}{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA}
 % \altaffiltext{PS1}{Pan-STARRS1 Builders}
 %\begin{document}
@@ -226 +239 @@
 \section{Introduction}\label{sec:introduction}
 
-For nearly four years, from 2010 May through 2014 March, the 1.8m \PS\ telescope (PS1) was used to perform as set of astronomical surveys with wide-ranging scientific goals.  The largest portion of the observing time (56\%) was used for the so-called $3\pi$ Survey, covering the $\frac{3}{4}$ of the sky north of -30 Declination, easily observable by \ps\ from its site on the summit of Haleakala on the Hawaiian island of Maui.  The wide-field optical design of the telescope \citep{2004AN....325..636H} allowed \ps\ to observe most of the $3\pi$ Survey area in each five filters (\grizy) between 10 and 15 times.  Another 25\% of the observing time was dedicated to the Medium Deep (MD) Survey, in which 10 fields were repeatedly observed over the course of the 4 year mission.  The Pan-STARRS1 Gigapixel Camera (GPC1), consisting of an $8 \times 8$ grid of $4846 \times 4868$ pixel CCDs covering roughly 7 square degrees, has a pixel scale of 0.257 arcseconds.  The telescope optics and the natural seeing of the site result in good image quality which is fully sampled by the GPC1 pixels: 75\% of the $3\pi$ Survey 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. 
+For nearly four years, from 2010 May through 2014 March, the 1.8m \PS\ telescope (PS1) was used to perform a set of astronomical surveys with wide-ranging scientific goals.  The largest portion of the observing time (56\%) was used for the so-called $3\pi$ Survey, covering the $\frac{3}{4}$ of the sky north of -30 Declination, easily observable by \ps\ from its site on the summit of Haleakala on the Hawaiian island of Maui.  The wide-field optical design of the telescope \citep{2004AN....325..636H} allowed \ps\ to observe most of the $3\pi$ Survey area in each five filters (\grizy) between 10 and 15 times.  Another 25\% of the observing time was dedicated to the Medium Deep (MD) Survey, in which 10 fields were repeatedly observed over the course of the 4 year mission.  The Pan-STARRS1 Gigapixel Camera (GPC1), consisting of an $8 \times 8$ grid of $4846 \times 4868$ pixel CCDs covering roughly 7 square degrees, has a pixel scale of 0.257\arcsec.  The telescope optics and the natural seeing of the site result in good image quality which is fully sampled by the GPC1 pixels: 75\% of the $3\pi$ Survey 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 $\sim 0.7$\arcsec. 
 
 % Operating under the aegis of the Pan-STARRS Science Consortium,
@@ -247 +260 @@
 The Pan-STARRS Project teamed with Alex Szalay's database development
 group at The Johns Hopkins University (JHU) to undertake the task of
-providing a publicly accessible hierarchical database for
+providing a publicly accessible database for
 \PS\ \citep{Heasley2008}. The JHU team was the major developer of the
 Sloan Digital Sky Survey (SDSS) public database \citep{Thakar2003},
@@ -262 +275 @@
 The system developed for \PS\ is called the {\em Published Science
   Products Subsystem}, or PSPS \citep{Heasley2006}.
-\note{define hierarchical, note relational}
-
-
-%(SDSS) public database \citep{Thakar2003}, and it is useful to reuse as much of the software developed for the SDSS as possible. However, due
-%to the Pan-STARRS's data having a larger intrinsic size and more complicated dataset, which covers a larger area of sky than SDSS and which
-%includes measurements on the stacks, single exposures, and mean properties of each, major changes were required. The system developed is
-%called the {\em Published Science Products Subsystem}, or PSPS \citep{Heasley2006}.
-
-The most significant challenge for the PSPS relative to the SDSS database implementation was the need to address the very large volume of \PS\ data.  The single monolithic database design of SDSS could not scale to the level needed for PS1 data.  While SQL Server does not have (at present) a cluster implementation, a bespoke version can be crafted using a combination of distributed partition views and data slices~\citep{Heasley2008}. Partitioning data into smaller databases spread over multiple server machines allows the information to be presented to the users as a single, unified table.
+
+\textadd{As a widely-used database engine, the Microsoft SQL Server provides a
+robust tool to define, build, and query the full database.  The engine
+implements the SQL relational database language: data within different
+tables of the database are related to data in other tables by common
+fields, or indexes.  In the PSPS implementation, the relationships are
+largely hierarchical: many measurements are linked to the images from
+which they came; associated measurements from the same astrophysical
+object are linked together to those objects.  The tables use unique
+indexes to form these relationships, as detailed throughput this article.}
+
+%(SDSS) public database \citep{Thakar2003}, and it is useful to reuse
+%as much of the software developed for the SDSS as possible. However,
+%due to the Pan-STARRS's data having a larger intrinsic size and more
+%complicated dataset, which covers a larger area of sky than SDSS and
+%which includes measurements on the stacks, single exposures, and mean
+%properties of each, major changes were required. The system developed
+%is called the {\em Published Science Products Subsystem}, or PSPS
+%\citep{Heasley2006}.
+
+The most significant challenge for the PSPS relative to the SDSS
+database implementation was the need to address the very large volume
+of \PS\ data.  The single monolithic database design of SDSS could not
+scale to the level needed for PS1 data.  While SQL Server does not
+have (at present) a cluster implementation, a bespoke version can be
+crafted using a combination of distributed partition views and data
+slices~\citep{Heasley2008}. Partitioning data into smaller databases
+spread over multiple server machines allows the information to be
+presented to the users as a single, unified table.
 
 %Our approach has been to use several features available within the Microsoft SQL Server product line to implement a system that would meet our requirements. 
@@ -316 +349 @@
 \label{sec:overview}
 
+% https://panstarrs.stsci.edu is OK (2020.08.13)
+% https://mastweb.stsci.edu/mcasjobs is OK (2020.08.13)
+
 Public access to the Pan-STARRS data is through the web server located
-at \url{http://panstarrs.stsci.edu} and is hosted by the {\em
-  Barbara A. Mikulski Archive for Space Telescopes} (MAST) at
+at \url{https://panstarrs.stsci.edu}
+% http is OK here
+and is hosted by the {\em
+Barbara A. Mikulski Archive for Space Telescopes} (MAST) at
 STScI. MAST provides the access point for downloading different pixel
 data products and their associated metadata and source catalogs. This
@@ -328 +366 @@
 Pan-STARRS tables is available through the Catalog Archive Server Jobs
 System (CasJobs) interface (see description at
-\url{http://mastweb.stsci.edu/mcasjobs}). CasJobs emulates local
+\url{https://mastweb.stsci.edu/mcasjobs}). CasJobs emulates local
 free-form SQL access in a web environment, and provides both
 synchronous and asynchronous query execution. The interface can
@@ -353 +391 @@
   preferred to making a new measurement directly from the available
   released pixel data, and care should be taken when using the
-  recalibrated astrometry with the original images (see Table
-  \ref{table:fundamentalipp}).
+  recalibrated astrometry with the original images (see Table~\ref{table:fundamentalipp}).
 
 \item Derived Data Products. These are higher order science products
@@ -383 +420 @@
 view of 32 \ippdbtable{Detection} tables, but the individual tables are hidden from
 the user. For more information on views, including the currently
-defines ones, see Table \ref{table:views}.
+defines ones, see Table~\ref{table:views}.
 
 This paper covers the data products and schema for the 3$\pi$ data
@@ -422 +459 @@
 \label{sec:chipandcamera}
 
- The \ippstage{chip} stage takes the raw images, generally 60 FITS files, one FITS file per OTA, and detrends them, one chip per computing job. Dark, flat, bias, background and other corrections, as described in Paper III, are applied to each chip image, followed by source detection and photometry using the \ippprog{psphot} program (Paper IV). Next, the \ippstage{camera} stage combines the outputs of the \ippstage{chip} stage, performs basic astrometry on the detected sources, and generates a binary FITS table, called an \smf\ file, holding the catalog information for the entire exposure. These files  are later ingested into a DVO-style database for internal use. These 2 stages are represented as the ``ipp processing" $\rightarrow$ ``camera" steps in Figure~\ref{fig:revisedipptopsps}. Camera stage products are available to the user in the PSPS `Detection' tables, starting with DR2.
+ The \ippstage{chip} stage takes the raw images, generally 60 FITS files, one FITS file per OTA, and detrends them, one chip per computing job. Dark, flat, bias, background and other corrections, as described in Paper III, are applied to each chip image, followed by source detection and photometry using the \ippprog{psphot} program (Paper IV). Next, the \ippstage{camera} stage combines the outputs of the \ippstage{chip} stage, performs basic astrometry on the detected sources, and generates a binary FITS table, called an \smf\ file, holding the catalog information for the entire exposure. These files  are later ingested into a DVO-style database for internal use. These 2 stages are represented as the ``ipp processing" $\rightarrow$ ``camera" steps in Figure~\ref{fig:revisedipptopsps}. Camera stage products are available to the user in the PSPS ``Detection'' tables, starting with DR2.
 
 
@@ -428 +465 @@
 \label{sec:fakeandwarp}
 
-The next step, the \ippstage{warp} stage, is represented as ``camera" $\rightarrow$ ``stacks" in Figure~\ref{fig:revisedipptopsps}. The \ippstage{warp} stage geometrically transforms the output images from the \ippstage{chip} stage to a common pixel grid defined on a tangential RA/Dec plane, with 0.25\arcsec\ pixels.  The output images, called ``skycells'', cover the entire sky; thus an image from a PS1 exposure can be split and projected onto a common layout for its portion of the sky. For 3$\pi$, the skycell tessellation\footnote{Note that our use of the term `tessellation' is inaccurate since the skycell sizes are variable and neighbors overlap each other.} is called \ippmisc{Rings.V3} and is described in detail in Paper II. This tessellation subdivides the sky into projections cell rings with centers at constant Declination.  Each projection cell is $\sim4.0~ \times \sim4.0$ degrees, subdivided into $10 \times 10$ skycells, each with 60\arcsec\ of overlap on a side, yielding square image with size ranging from 6240 to 6500 pixels on a side. All image data products beyond \ippstage{warp} (\ippstage{stacks}/\ippstage{forced warps}/\ippstage{diffs}/ etc.) are laid out in skycells as well.  
+The next step, the \ippstage{warp} stage, is represented as ``camera'' $\rightarrow$ ``stacks'' in Figure~\ref{fig:revisedipptopsps}. The \ippstage{warp} stage geometrically transforms the output images from the \ippstage{chip} stage to a common pixel grid defined on a tangential R.A./Dec plane, with 0.25\arcsec\ pixels.  The output images, called ``skycells'', cover the entire sky; thus an image from a PS1 exposure can be split and projected onto a common layout for its portion of the sky. For 3$\pi$, the skycell tessellation\footnote{Note that our use of the term ``tessellation'' is inaccurate since the skycell sizes are variable and neighbors overlap each other.} is called \ippmisc{Rings.V3} and is described in detail in Paper II. This tessellation subdivides the sky into projections cell rings with centers at constant Declination.  Each projection cell is $\sim4.0~ \times \sim4.0$ degrees, subdivided into $10 \times 10$ skycells, each with 60\arcsec\ of overlap on a side, yielding square image with size ranging from 6240 to 6500 pixels on a side. All image data products beyond \ippstage{warp} (\ippstage{stacks}/\ippstage{forced warps}/\ippstage{diffs}/ etc.) are laid out in skycells as well.  
 
 The warp image products are available to users via MAST for the $3\pi$ survey as part of DR2.
@@ -435 +472 @@
 \label{sec:stackstages}
 
-There are 3 stack-related stages: \ippstage{stack}, \ippstage{staticsky}, and \ippstage{skycal}. The \ippstage{stack} stage generates the stacked images, \ippstage{staticsky} generates the source catalogs files, while \ippstage{skycal} calibrates the source catalogs. All of the stack related stages are represented as ``stacks" in Figure~\ref{fig:revisedipptopsps}.
+There are 3 stack-related stages: \ippstage{stack}, \ippstage{staticsky}, and \ippstage{skycal}. The \ippstage{stack} stage generates the stacked images, \ippstage{staticsky} generates the source catalogs files, while \ippstage{skycal} calibrates the source catalogs. All of the stack related stages are represented as ``stacks'' in Figure~\ref{fig:revisedipptopsps}.
 
 \ippstage{Stacks} are generated by adding together \ippstage{warp} skycells, with bad-pixel rejection and internal calibration as described in Paper III.  Depending on the survey, stacks may be generated from different sets of raw exposures.  For the deepest possible stacks, essentially all available exposures are combined, with only weak cuts on the data quality.  Stacks may also be generated with a constraint on the image quality of the input exposures in order to yield a deep reference image with good image quality.   In order to limit contamination from on-going transient events, stacks may also be generated with constraints on the time range of the input exposures : out-of-season stacks would include only exposures {\em not} taken within a given year or period to act as a reference for transient events within that period.  The different stack types are listed in the \ippdbtable{StackType} table in the PSPS database.  For the DR1 and DR2 3$\pi$ databases, only the \ippmisc{DEEP\_STACK} \ippstage{stack} type is used, i.e., all available \ippstage{warps} of sufficiently good quality for a given skycell and filter within the 3$\pi$ survey data set are used to generate the \ippstage{stacks}, yielding one \ippstage{stack} per skycell per filter. Mask images, variance images, and related pixel images are also generated for each stack.   
@@ -441 +478 @@
 Once each \ippstage{stack} image is created, source detection and characterization, including galaxy morphological analysis, is performed by the \ippstage{staticsky} stage.  The source analysis is run on all 5 filters at once.  PSF photometry is forced for sources which are detected in at least two filter images on the other filter images for which the source was not detected above the $5\sigma$ threshold.  This forced photometry is also performed for sources detected in only the \yps-band.  
 
-Aperture photometry, for a series of circular apertures specified by SDSS \citep{Stoughton2002}, is performed on the raw stacks and also on stack images which have been convolved to a common 6 pixel FWHM, and again to a common 8 pixel FWHM.  These latter seeing-matched images are only kept in memory for the analysis and are not written to disk.  Up to 9 of the SDSS apertures are used for this measurement: R3 ($r = 1.03$ arcsec), R4 ($r = 1.76$ arcsec), R5 ($r = 3.00$ arcsec), R6 ($r = 4.63$ arcsec), R7 ($r = 7.43$ arcsec), R8 ($r = 11.42$ arcsec), R9 ($r = 18.20$ arcsec), R10 ($r = 28.20$ arcsec), and R11 ($r = 44.21$ arcsec).  Note that the measurement is performed in apertures with the same angular diameter as used for SDSS, which necessarily results in different radii in pixels from those used by SDSS apertures \citep[see Table 7 in ][]{Stoughton2002}.  For more details on the photometric analysis of the stack images, see Paper IV.
-
-Catalog files, one per filter, are generated with sources spatially-matched between filters using a 5 pixel (1.25\arcsec) correlation radius. Sources matched as across filters are linked in the output catalog by the detection ID.  The \ippstage{skycal} stage calibrates the \ippstage{staticsky} catalogs relative to the reference catalog. The calibrated catalog files are later ingested into the DVO database and then into the PSPS database. Due to the overlap between skycells, sources that land in the overlaps can be reported 2, 3, or 4 times in the DVO and PSPS database.  See the discussion in Section~\ref{sec:schemast} regarding the `primary' and `best' stack measurements.
+Aperture photometry, for a series of circular apertures specified by SDSS \citep{Stoughton2002}, is performed on the raw stacks and also on stack images which have been convolved to a common 6 pixel FWHM, and again to a common 8 pixel FWHM.  These latter seeing-matched images are only kept in memory for the analysis and are not written to disk.  Up to 9 of the SDSS apertures are used for this measurement: R3 ($r = 1.03$\arcsec), R4 ($r = 1.76$\arcsec), R5 ($r = 3.00$\arcsec), R6 ($r = 4.63$\arcsec), R7 ($r = 7.43$\arcsec), R8 ($r = 11.42$\arcsec), R9 ($r = 18.20$\arcsec), R10 ($r = 28.20$\arcsec), and R11 ($r = 44.21$\arcsec).  Note that the measurement is performed in apertures with the same angular diameter as used for SDSS, which necessarily results in different radii in pixels from those used by SDSS apertures \citep[see Table~7 in ][]{Stoughton2002}.  For more details on the photometric analysis of the stack images, see Paper IV.
+
+Catalog files, one per filter, are generated with sources spatially-matched between filters using a 5 pixel (1.25\arcsec) correlation radius. Sources matched as across filters are linked in the output catalog by the detection ID.  The \ippstage{skycal} stage calibrates the \ippstage{staticsky} catalogs relative to the reference catalog. The calibrated catalog files are later ingested into the DVO database and then into the PSPS database. Due to the overlap between skycells, sources that land in the overlaps can be reported 2, 3, or 4 times in the DVO and PSPS database.  See the discussion in Section~\ref{sec:schemast} regarding the ``primary'' and ``best'' stack measurements.
 
 Stack data products are available for the $3\pi$ survey as part of DR1 and DR2. Stack image products are available to users via MAST, and Stack-related tables are available in the PSPS database.
@@ -454 +491 @@
 In the forced warp photometry stage, the positions of sources located in the deep \ippstage{stacks} are used to fix the position in the warp images.  The software then measures the PSF model flux at those positions on each of the individual warps.  This measurement also yields the Kron and aperture fluxes for the warp image at that location.  The catalogs generated by this process are ingested into the DVO database and average values are then calculated.  Note that the fluxes on the warps for faint objects may be insignificant or even negative; the average values are calculated using all flux values (both positive and negative) properly weighted by the detection flux errors.  Only measurements for which the warp pixels were excessively masked are rejected in this average flux calculation.  The individual measurements and the averages are translated by the \ippstage{IppToPsps} stage into the \ippdbtable{ForcedWarp*} tables for the PSPS.  For the $3\pi$ survey, these tables are available starting with DR2. 
 
-For extended sources, galaxy models are fitted on the \ippstage{stack} images. These models are then used as a seed to determine galaxy models for each warp image. The position, aspect ratio, and (where appropriate) Sersic radius are kept fixed to the values determined for the stack image.  A grid of major and minor axis values are tested around the values from the stack fit for each warp image, with the galaxy model convolved with the PSF appropriate to the specific warp image.  The software reports the model normalization and $\chi^2$ value at each grid point; these are combined together across all warp exposures and the interpolated minimum $\chi^2$ value is used to determine a best-fit galaxy model.  Due to size constraints, only the average galaxy model results are propagated to the PSPS database.  These are later ingested into the PSPS database as the \ippdbtable{ForcedGalaxy*} tables. 
+For extended sources, galaxy models are fitted on the \ippstage{stack} images. These models are then used as a seed to determine galaxy models for each warp image. The position, aspect ratio, and (where appropriate) \Sersic\ radius are kept fixed to the values determined for the stack image.  A grid of major and minor axis values are tested around the values from the stack fit for each warp image, with the galaxy model convolved with the PSF appropriate to the specific warp image.  The software reports the model normalization and $\chi^2$ value at each grid point; these are combined together across all warp exposures and the interpolated minimum $\chi^2$ value is used to determine a best-fit galaxy model.  Due to size constraints, only the average galaxy model results are propagated to the PSPS database.  These are later ingested into the PSPS database as the \ippdbtable{ForcedGalaxy*} tables. 
 
 The extended source (galaxy) models described above are not applied to all sources.  Galaxy models are only applied if the measured Kron magnitudes are brighter than the following limits for at least one filter: (\grizy) = (21.5, 21.5, 21.5, 20.5, 19.5).  In addition, galaxy models and Petrosian fluxes are only measured for skycells with centers outside of a Galactic plane exclusion zone defined for the $3\pi$ Survey as:
@@ -475 +512 @@
 Difference images are generated by the IPP in order to detect transient and moving objects.  Several types of difference images may be generated by the IPP depending on the type of images which are involved in the subtraction.  The \ippmisc{WARP\_WARP} diffs are generated by subtracting warps from a pair of exposures, usually taken within a short period of time; these are primarily used by the nightly science processing and the MOPS analysis for inner solar system sources and for transient detections from the $3\pi$ survey data. \ippmisc{STACK\_STACK} diffs are generated by subtracting a deep reference stack from a stack of multiple exposure taken over a shorter period. The \ippmisc{STACK\_STACK} diffs are used for supernova discovery in the MD survey fields with 8 exposures taken in sequence and stacked to make a more sensitive single-epoch observation. The \ippmisc{WARP\_STACK} diffs were generated for the $3\pi$ survey by combining warps from single exposures with a deep reference stack.  These diffs are also used for MOPS and transient discoveries, and will be provided for the full $3\pi$ Survey as a temporal reference.  There is one \ippstage{diff} image for each single exposure within the 3$\pi$ survey. Finally, \ippmisc{STACK\_WARP} diffs could be made in principal but are not in practice used by the IPP. 
 
-For the difference image analysis, the input images (\ippstage{stack} or \ippstage{warp}) are convolved to have similar PSFs \citep{Waters2017} and one subtracted from the other. Sources are detected on the difference image, basic photometry is performed on the sources, and \ippstage{diff} catalog files are created.  The \ippstage{diff} catalog files are then ingested into the \ippstage{diff} DVO, and later ingested into the PSPS.  
-The results from this stage of processing include diff catalog files, which will be available in a future release (nominally DR3). The diff images can be reconstructed from available data products hosted at STScI, but at this time we anticipate they will not be stored there due to space constraints.
+For the difference image analysis, the input images (\ippstage{stack}
+or \ippstage{warp}) are convolved to have similar PSFs
+\citep{Waters2017} and one subtracted from the other. Sources are
+detected on the difference image, basic photometry is performed on the
+sources, and \ippstage{diff} catalog files are created.  The
+\ippstage{diff} catalog files are then ingested into the
+\ippstage{diff} DVO, and later ingested into the PSPS.  The results
+from this stage of processing include diff catalog files, which will
+be available in a future release (nominally DR3). \textmod{At this
+  time, it is undecided if, as part of DR3, the complete collection of
+  PV3 difference images will be
+  stored at MAST or if they will be generated on demand.  Within the
+  IPP, difference images are generally stored on disk only for a short
+  period of time (days to weeks) in order to save on storage space.
+  When needed, historical difference images are regularly regenerated based on stored
+  results (difference kernels and PSF models).  MAST may rely on this
+  process for DR3.}
 
 \subsection{DVO Database Steps}
@@ -492 +544 @@
 Catalog files from several stages of IPP processing are ingested into the DVO database via the IPP program \ippprog{addstar}.  The relevant stages are \ippstage{camera} (all measurements from the individual exposures), \ippstage{skycal} (measurements from the stacks), and \ippstage{forced warp} (forced photometry and the forced galaxy model fits from the warps).  Difference image catalogs are ingested into the separate diff DVO database. 
 
-Measurements from 2MASS, WISE, and Gaia are also merged into the DVO database; flags within the DVO database, and inherited by the PSPS database, note the presence of data from these surveys. Gaia DR1 \citep{Gaia2016} was released before the Pan-STARRS DR1 was complete, but after all of the object tables were already ingested into the PSPS database.  We used the Gaia DR1 data to recalibrate the DVO object positions, which improved the astrometry significantly. Rather than regenerate the database and start over (with corrected RA and Dec positions), we arranged for the \ippstage{IppToPsps} system to export just the newly calibrated positions along with minimal metadata to link the new coordinates with the existing objects.  See Section~\ref{sec:ipptopsps} on the special table which carries the Gaia DR1 calibration into the $3\pi$ Survey DR1 release.  For the $3\pi$ Survey DR2, the calibration is tied directly to the Gaia DR1 astrometric system (Paper V).  
-
-The DVO databasing system uses a collection of binary FITS tables as the backend.  These files define a spatial partition of the database, divided on lines of constant RA and Dec.  For a given file type, the database contains several thousand such files.  Several categories of DVO files are used by \ippstage{IppToPsps} to populate the PSPS database.  Here we give a short summary of the subset of DVO files that are most relevant for \ippstage{IppToPsps} (see Paper II for more details).
-
-\parheading{.cpt} Object information - each .cpt table has one entry for each object in that region of the sky. It summarizes the average properties of that object as long as those properties can be derived independently of the filter used. Information such as mean RA and Dec are listed in these files.  
+Measurements from 2MASS, WISE, and Gaia are also merged into the DVO database; flags within the DVO database, and inherited by the PSPS database, note the presence of data from these surveys. Gaia DR1 \citep{Gaia2016} was released before the Pan-STARRS DR1 was complete, but after all of the object tables were already ingested into the PSPS database.  We used the Gaia DR1 data to recalibrate the DVO object positions, which improved the astrometry significantly. Rather than regenerate the database and start over (with corrected R.A. and Dec positions), we arranged for the \ippstage{IppToPsps} system to export just the newly calibrated positions along with minimal metadata to link the new coordinates with the existing objects.  See Section~\ref{sec:ipptopsps} on the special table which carries the Gaia DR1 calibration into the $3\pi$ Survey DR1 release.  For the $3\pi$ Survey DR2, the calibration is tied directly to the Gaia DR1 astrometric system (Paper V).  
+
+The DVO databasing system uses a collection of binary FITS tables as the backend.  These files define a spatial partition of the database, divided on lines of constant R.A. and Dec.  For a given file type, the database contains several thousand such files.  Several categories of DVO files are used by \ippstage{IppToPsps} to populate the PSPS database.  Here we give a short summary of the subset of DVO files that are most relevant for \ippstage{IppToPsps} (see Paper II for more details).
+
+\parheading{.cpt} Object information - each .cpt table has one entry for each object in that region of the sky. It summarizes the average properties of that object as long as those properties can be derived independently of the filter used. Information such as mean R.A. and Dec are listed in these files.  
 
 \parheading{.cpm} Measurements - each .cpm table contains all of the measurement information for each object in the .cpt file. Contains measurement information for detections from the stack/skycal cmf, camera smfs, and forced warp smfs.
@@ -568 +620 @@
 \parheading{Diff detection batches (DF)} Populate the \ippdbtable{DiffDetection} table, described in more detail in Section~\ref{sec:schemadiff}.  Each batch corresponds to a difference image catalog file created in the \ippstage{diff} stage, and contains all of the skycells for a given exposure.  Columns are filled from the DVO database ({\em cpt} and {\em cpm} files), and from the corresponding \ippstage{diff} catalog file (\cmf). 
 
-\parheading{Gaia object batches (GO)} Populate the \ippdbtable{GaiaFrameCoordinate} table, linking the Gaia DR1 calibrated positions to the \ippdbtable{ObjectThin} entries by \ippdbcolumn{objID}.  It is based on exactly the same DVO files as OB batches, has updated RA and Dec calibrated to Gaia, and ignores the rest of the DVO columns.  These batches, and this table, are only present for DR1.  For DR2, additional calibration improvements were made within the DVO database (see Paper V).  The average property batches were regenerated, making the GO batch irrelevant for that release.
+\parheading{Gaia object batches (GO)} Populate the \ippdbtable{GaiaFrameCoordinate} table, linking the Gaia DR1 calibrated positions to the \ippdbtable{ObjectThin} entries by \ippdbcolumn{objID}.  It is based on exactly the same DVO files as OB batches, has updated R.A. and Dec calibrated to Gaia, and ignores the rest of the DVO columns.  These batches, and this table, are only present for DR1.  For DR2, additional calibration improvements were made within the DVO database (see Paper V).  The average property batches were regenerated, making the GO batch irrelevant for that release.
 
 Within \ippstage{IppToPsps} it is possible to verify that the expected batches were generated, and to re-queue and regenerate batches that failed.  Batches fail for a variety of reasons, but none of the failures are terminal.  Batches can fail if any of the associated {\em mysql} databases time out or are unavailable, if there are disk or network I/O glitches or other disk/network problems.  The DVO database sets the expected number of batches to generate, and failures are investigated and retried until they are resolved. Within \ippstage{IppToPsps} it is also possible to poll the PSPS to verify if batches have been ingested, thus closing the loop.  %This allows for easy removal of batches that have been loaded to PSPS in order to regain disk space. 
@@ -587 +639 @@
 %\subsection{Introduction}
 
-The PSPS consists of several parts: the data transformation layer (DXLayer), the Object Database Manager (ODM), the Workflow Manager Database (WMD), and the data retrieval layer (DRL).  The user accesses the data through the DRL, using either scripts, the STScI CasJobs interface, or if the user is a \PS\ Consortium member, the Published Science Interface (PSI). The DXLayer polls the \ippstage{IppToPsps} datastores for new batches and prepares them for loading.  The ODM is the software used to load, merge, copy and publish the PSPS databases.  The WMD is the database containing all the logs about the PSPS databases.  The DRL is the intermediate layer between the client and the PSPS database.  The PSI is the web based interface for PS1 consortium members, for interacting with the DRL. Each of these components is described in more detail below, and a diagram of the process is shown in Fig~\ref{fig:odm_data_flow}
+The PSPS consists of several parts: the data transformation layer (DXLayer), the Object Database Manager (ODM), the Workflow Manager Database (WMD), and the data retrieval layer (DRL).  The user accesses the data through the DRL, using either scripts, the STScI CasJobs interface, or if the user is a \PS\ Consortium member, the Published Science Interface (PSI). The DXLayer polls the \ippstage{IppToPsps} datastores for new batches and prepares them for loading.  The ODM is the software used to load, merge, copy and publish the PSPS databases.  The WMD is the database containing all the logs about the PSPS databases.  The DRL is the intermediate layer between the client and the PSPS database.  The PSI is the web based interface for PS1 consortium members, for interacting with the DRL. Each of these components is described in more detail below, and a diagram of the process is shown in Figure~\ref{fig:odm_data_flow}
 
 % \showfigure{pspsslices.tex}
@@ -599 +651 @@
 % Figure~\ref{fig:pspsslices} shows the different database slices, and Table~\ref{table:pspsslices} describes the names of the slices and the declination ranges for each slice.  
 
-\subsection{The Data Transformation Layer (DXLayer)} The DXLayer is the first stage in the PSPS to receive data from \ippstage{IppToPsps}. This stage polls the IPP datastore interface for new batches to load and prepares them for the next step (ODM). Fig~\ref{fig:dxlayerprocess} shows the flowchart of the DXLayer process, and Fig~\ref{fig:psps_loadprocess} shows a more detailed flowchart of how batches are loaded and verified within the DXLayer and ODM. PSPS loads batches created by the \ippstage{IppToPsps} (Section~\ref{sec:ipptopsps}).  Batches contain a manifest file that describes the batch information such as type of batch, min/max \ippdbcolumn{objID}, MD5 checksum, and the tables to load. Batch data is stored in FITS files, which are transformed into comma-separated value (csv) files in the DXLayer. As noted above, the batch area cannot exceed two PSPS slices or it will fail to load.  The PSPS slices are constructed so that this does not happen.
+\subsection{The Data Transformation Layer (DXLayer)} The DXLayer is the first stage in the PSPS to receive data from \ippstage{IppToPsps}. This stage polls the IPP datastore interface for new batches to load and prepares them for the next step (ODM). Figure~\ref{fig:dxlayerprocess} shows the flowchart of the DXLayer process, and Figure~\ref{fig:psps_loadprocess} shows a more detailed flowchart of how batches are loaded and verified within the DXLayer and ODM. PSPS loads batches created by the \ippstage{IppToPsps} (Section~\ref{sec:ipptopsps}).  Batches contain a manifest file that describes the batch information such as type of batch, min/max \ippdbcolumn{objID}, MD5 checksum, and the tables to load. Batch data is stored in FITS files, which are transformed into comma-separated value (CSV) files in the DXLayer. As noted above, the batch area cannot exceed two PSPS slices or it will fail to load.  The PSPS slices are constructed so that this does not happen.
 
 \input{pspsslicetable.tex}
@@ -609 +661 @@
 \showfigure{psps_loadprocess.tex}
 
-\subsection{The Data Retrieval Layer (DRL)} The DRL is the layer between the user and the PSPS database.  The DRL is responsible for management of queries that the user submits via the DRL API.  The DRL is based on CasJobs \citep{Szalay2007}, and has many similar features. It primarily keeps track of all user queries and provides progress updates of those queries in a secure way. It also kills queries that use too many resources or take too long. The DRL API is accessed via Simple Access Object Protocol (SOAP), allowing users multiple ways to access the database.  Before the public releases, Pan-STARRS science consortium members used the Published Science Interface (PSI, a web-based user interface) initially based at the IfA and later at STScI.  For the general public, the MAST server provides access via the CasJobs interface (\url{https://mastweb.stsci.edu/ps1casjobs/}), as well as a simple object search form which implements a basic cone search (\url{https://catalogs.mast.stsci.edu/panstarrs}).  It is also possible for the consortium users to query the database via SOAP calls from command line scripts.  
+% https://mastweb.stsci.edu/ps1casjobs is OK (2020.08.13)
+% https://catalogs.mast.stsci.edu/panstarrs is OK (2020.08.13)
+
+\subsection{The Data Retrieval Layer (DRL)}
+The DRL is the layer between the user and the PSPS database.  The DRL
+is responsible for management of queries that the user submits via the
+DRL API.  The DRL is based on CasJobs \citep{Szalay2007}, and has many
+similar features. It primarily keeps track of all user queries and
+provides progress updates of those queries in a secure way. It also
+kills queries that use too many resources or take too long. The DRL
+API is accessed via \textmod{Simple Object Access Protocol (SOAP, \url{w3.org/TR/soap})},
+allowing users multiple ways to access the database.  Before the
+public releases, Pan-STARRS science consortium members used the
+Published Science Interface (PSI, a web-based user interface)
+initially based at the IfA and later at STScI.  For the general
+public, the MAST server provides access via the CasJobs interface
+(\url{https://mastweb.stsci.edu/ps1casjobs/}), as well as a simple
+object search form which implements a basic cone search
+(\url{https://catalogs.mast.stsci.edu/panstarrs}).  It is also
+possible for the consortium users to query the database via SOAP calls
+from command line scripts.
 
 %A flowchart of the DRL can be seen in Figure~\ref{fig:psps_drl}.
@@ -617 +689 @@
 % Bernie says 'no'
 
-\subsection{Published Science Interface (PSI)} The PSI is the web user interface provided to the Pan-STARRS Science Consortium members. This interface provides many useful features including a query request page, information on query progress, MyDB management tools, graphing tools, access to the pixel data products, and interactive help.  The query request page allows for the user to easily submit queries to a variety of databases (3pi/MD/MyDB), to upload query files or to check the syntax, to name MyDB results tables and to select the queue to submit to. The MyDB management tools allow the user to easily select which MyDB tables to purge as well as well as methods to extract to csv, FITS or xml files to download.  Some of the interactive features include an interactive schema browser, a query builder to easily create a query with multiple joins and conditions, and a flag generator to create bitmasks for the different types of flag tables. 
+\subsection{Published Science Interface (PSI)} The PSI is the web user interface provided to the Pan-STARRS Science Consortium members. This interface provides many useful features including a query request page, information on query progress, MyDB management tools, graphing tools, access to the pixel data products, and interactive help.  The query request page allows for the user to easily submit queries to a variety of databases (3pi/MD/MyDB), to upload query files or to check the syntax, to name MyDB results tables and to select the queue to submit to. The MyDB management tools allow the user to easily select which MyDB tables to purge as well as well as methods to extract to CSV, FITS or XML files to download.  Some of the interactive features include an interactive schema browser, a query builder to easily create a query with multiple joins and conditions, and a flag generator to create bitmasks for the different types of flag tables. 
 % SC: consider removing most of the PSI content.  The last sentence mostly replicates previous content.
 
@@ -652 +724 @@
 \ippdbtable{Detection} table, using \ippdbcolumn{objID}, in order to get the
 individual photometric attributes for all the detections of that
-object within the single exposures (at a given RA and Dec).
+object within the single exposures (at a given R.A. and Dec).
 
 % \subsection{\ippdbcolumn{objID} and its relation to R.A. and Dec.} 
@@ -659 +731 @@
 The index \ippdbcolumn{objID} (and \ippdbcolumn{diffObjID} for difference
 tables) is derived from right ascension and declination.  While it is
-possible to calculate the RA and Dec from the \ippdbcolumn{objID}, this is
+possible to calculate the R.A. and Dec from the \ippdbcolumn{objID}, this is
 not recommended. The \ippdbcolumn{objID} value is determined when an object
 is initially instantiated in the DVO database, and is based on the
@@ -903 +975 @@
 detection.  These bits include information specific to difference
 imaging, as well as quality issues such as if source is near
-diffraction spikes, star core, affected by the `burntool' analysis of
+diffraction spikes, star core, affected by the ``burntool'' analysis of
 persistence features (see Paper III), along with other analysis
 issues.  See also Paper IV.
@@ -972 +1044 @@
 DR2 version of the database, the astrometry was recalibrated against
 Gaia DR1; the coordinates reported in the \ippdbtable{ObjectThin} table should be
-used as the best RA and Dec.  Use \ippdbcolumn{objID} to join to most
+used as the best R.A. and Dec.  Use \ippdbcolumn{objID} to join to most
 tables.
 
@@ -984 +1056 @@
 %There are several metadata tables specific to different stages of data ingested (i.e., metadata for individual exposures, \ippstage{stacked} skycells, \ippstage{difference} skycells, \ippstage{forced warp} skycells).  Basic information about indivudual exposures, \ippstage{stack} skycells, \ippstage{difference} skycells, such as the filter, exposure time, observation time, basic metrics, etc. can be found in these tables: \ippdbtable{DiffMeta}, \ippdbtable{ForcedWarpMeta}, \ippdbtable{StackMeta}, \ippdbtable{ImageMeta}. The metadata tables linking \ippstage{stacks}/\ippstage{diffs}/\ippstage{forcedwarps} to individual exposures are \ippdbtable{DiffToImage}, \ippdbtable{ForcedWarpToImage}, \ippdbtable{StackToImage}, and \ippdbtable{StackToFrame}.  There is metadata available on the detection efficiency for difference images and single exposures in \ippdbtable{DiffDetEffMeta} and \ippdbtable{ImageDetEffMeta}. \ippdbtable{ImageMeta} has metadata for a single exposure, while \ippdbtable{FrameMeta} has metadata for each of the 60 OTAs that make up an image. Further information about these tables are described in sections below.
 
-\subsubsection{Tables based on the `camera' stage of IPP}
+\subsubsection{Tables based on the ``camera'' stage of IPP}
 \label{sec:schemap2}
 
-Images processed through the \ippstage{camera} stage of the IPP have been detrended, and have had astrometry and photometry calculated.  Basic information from the images are then merged into the DVO database.  The core tables based on the \ippstage{camera} stage are \ippdbtable{FrameMeta}, \ippdbtable{ImageMeta}, \ippdbtable{Detection}, and \ippdbtable{ImageDetEffMeta}. Each image ingested into the PSPS database has a unique \ippdbcolumn{imageID}; this can be used to find out, via the \ippdbtable{FrameMeta}, \ippdbtable{ImageMeta}, and \ippdbtable{ImageDetEffMeta} tables, information about each image such as the filter, RA and Dec, exposure time, etc.  All of the detections measured in the image are ingested into the Detection table, which also has the \ippdbcolumn{imageID}, allowing for single detections to be traced back to the OTA on which it was imaged.  
-
-\parheading{FrameMeta} Contains metadata related to an individual exposure. A {\em Frame} refers to the collection of all images obtained by the 60 OTA devices in the camera in a single exposure. The camera configuration, telescope pointing, observation time, and astrometric solution from the detector focal plane (L,M) to the sky (RA,Dec) is provided.
+Images processed through the \ippstage{camera} stage of the IPP have been detrended, and have had astrometry and photometry calculated.  Basic information from the images are then merged into the DVO database.  The core tables based on the \ippstage{camera} stage are \ippdbtable{FrameMeta}, \ippdbtable{ImageMeta}, \ippdbtable{Detection}, and \ippdbtable{ImageDetEffMeta}. Each image ingested into the PSPS database has a unique \ippdbcolumn{imageID}; this can be used to find out, via the \ippdbtable{FrameMeta}, \ippdbtable{ImageMeta}, and \ippdbtable{ImageDetEffMeta} tables, information about each image such as the filter, R.A. and Dec, exposure time, etc.  All of the detections measured in the image are ingested into the Detection table, which also has the \ippdbcolumn{imageID}, allowing for single detections to be traced back to the OTA on which it was imaged.  
+
+\parheading{FrameMeta} Contains metadata related to an individual exposure. A {\em Frame} refers to the collection of all images obtained by the 60 OTA devices in the camera in a single exposure. The camera configuration, telescope pointing, observation time, and astrometric solution from the detector focal plane (L,M) to the sky (R.A.,Dec) is provided.
 
 \parheading{ImageMeta} Contains metadata related to an individual OTA (chip) image that comprises a portion of the full exposure. The characterization of the image quality, the detrends applied, and the astrometric solution from the raw pixels (X,Y) to the detector focal plane (L,M) is provided.
@@ -997 +1069 @@
 \parheading{ImageDetEffMeta} Contains the detection efficiency information for a given individual OTA image. Provides the number of recovered sources out of 500 injected fake source and statistics about the magnitudes of the recovered sources for a range of magnitude offsets.
 
-\subsubsection{Tables based on the `stack' stage of IPP}
+\subsubsection{Tables based on the ``stack'' stage of IPP}
 \label{sec:schemast}
 
@@ -1021 +1093 @@
 independent.  Only one set of such measurements should be used for
 valid population statistics.  To aid in such analysis, we define a
-`primary' detection for all stack measurements (from a single filter)
-of the same astronomical object.  The `primary' detection is that
+``primary'' detection for all stack measurements (from a single filter)
+of the same astronomical object.  The ``primary'' detection is that
 detection for which the stack pixels are closest to the center of the
 skycell. Since the definition is purely geometric, in theory no
@@ -1029 +1101 @@
 split a source into multiple detections within the image.  For the
 primary skycells, these detections will each be identified as
-`primary', though they come from the same astrophysical object.
+``primary'', though they come from the same astrophysical object.
 However, this is due to the analysis process, not the overlap of the
 stack boundaries.
@@ -1039 +1111 @@
 object.  Users who prefer a high-quality measurement of a particular
 object may choose to use these secondary measurements rather than the
-primary.  We attempt to identify the `best' stack measurement for each
+primary.  We attempt to identify the ``best'' stack measurement for each
 filter by examining the signal-to-noise of the measurements and the
 {\tt PSF\_QF\_PERFECT} values, a measurement of the masked-fraction
@@ -1058 +1130 @@
   STACK\_PRIMARY} bit set in the \ipptable{StackObjectThin.XinfoFlag3}
 field for the appropriate filter while stack measurements which are
-identified as the `best' measurement for an object within a given
+identified as the ``best'' measurement for an object within a given
 filter have the {\tt STACK\_PHOT\_SRC} bit set in the same field (see
 Tables~\ref{table:detectionflags3} and \ref{table:StackObjectThin}).
@@ -1067 +1139 @@
 %% (this field is identical for all filters).
 
-If all of the `best' measurements for a stack object (across all 5
+If all of the ``best'' measurements for a stack object (across all 5
 filters) are also primary measurements, then the {\tt BEST\_STACK} bit
 is set in the \ipptable{ObjectThin.objInfoFlag} entry for the
@@ -1074 +1146 @@
 
 Several bits in the \ipptable{StackObjectThin.XinfoFlag4} field for
-each filter may be set based on the `primary' and `best' detections
+each filter may be set based on the ``primary'' and ``best'' detections
 (see Tables~\ref{table:detectionflags3} and
-\ref{table:StackObjectThin}).  If a `primary' measurement exists for a
+\ref{table:StackObjectThin}).  If a ``primary'' measurement exists for a
 given filter, then the {\tt SECF\_STACK\_PRIMARY} bit is set for that
 filter.  If multiple primary stack measurements exist for a given
 filter, then the {\tt SECF\_STACK\_PRIMARY\_MULTIPLE} bit is also set for
-that filter (not set in DR1).  If the `best' measurement for a filter
+that filter (not set in DR1).  If the ``best'' measurement for a filter
 is a significant detection (not forced from another band), then the
-{\tt SECF\_STACK\_BESTDET} bit is set. If any of the `primary' measurements
+{\tt SECF\_STACK\_BESTDET} bit is set. If any of the ``primary'' measurements
 for a filter is a significant detection (not forced from another
 band), then the {\tt SECF\_STACK\_PRIMDET} bit is set. If any stack
@@ -1106 +1178 @@
 joined into a single row, with metadata indicating if this stack
 object represents the primary detection.  In addition, a detection is
-flagged as `best' if it is a primary detection with a \ippdbcolumn{psfQf}
+flagged as ``best'' if it is a primary detection with a \ippdbcolumn{psfQf}
 value greater than 0.98; if that condition is not met, then the
 primary or secondary detection with the highest \ippdbcolumn{psfQf} value
@@ -1163 +1235 @@
 \parheading{StackDetEffMeta} Contains the detection efficiency information for a given stacked image.  Provides the number of recovered sources out of 500 injected sources for each magnitude bin and statistics about the magnitudes of the recovered sources for a range of magnitude offsets.
 
-\subsubsection{Tables from the `forced photometry' stage of IPP}
+\subsubsection{Tables from the ``forced photometry'' stage of IPP}
 \label{sec:schemafw}
 
@@ -1185 +1257 @@
 \parheading{ForcedMeanLensing}  Contains the mean \citet{Kaiser1995} lensing parameters measured from the forced photometry of objects detected in stacked images on the individual single epoch data. Use \ippdbcolumn{objID} to join to most tables; use \ippdbcolumn{uniquePspsFOid} to join to \ippdbtable{ForcedMeanObject}. \ippdbcolumn{objID} is not unique, but \ippdbcolumn{uniquePspsFOid} is.
 
-\parheading{ForcedGalaxyShape}  Contains the extended source galaxy shape parameters. The positions, magnitudes, fluxes, and Sersic indices are inherited from their parent measurement in the \ippdbtable{StackModelFit} tables, and are reproduced here for convenience. The major and minor axes and orientation are recalculated on a warp-by-warp basis from the best fit given these inherited properties \citep{Sersic1963}. Use \ippdbcolumn{objID} to join to most tables. \ippdbcolumn{objID} is not unique, but \ippdbcolumn{uniquePspsFGid} is.
+\parheading{ForcedGalaxyShape}  Contains the extended source galaxy shape parameters. The positions, magnitudes, fluxes, and \Sersic\ indices are inherited from their parent measurement in the \ippdbtable{StackModelFit} tables, and are reproduced here for convenience. The major and minor axes and orientation are recalculated on a warp-by-warp basis from the best fit given these inherited properties \citep{Sersic1963}. Use \ippdbcolumn{objID} to join to most tables. \ippdbcolumn{objID} is not unique, but \ippdbcolumn{uniquePspsFGid} is.
 
 \parheading{ForcedWarpMeta} Contains the metadata related to a sky-aligned distortion corrected \ippstage{warp} image, upon which forced photometry is performed. The astrometric and photometric calibration of the \ippstage{warp} image are listed. 
@@ -1203 +1275 @@
 \showfigure{objid.tex}
 
-\subsubsection{Tables based on the `diff' stage of IPP}
+\subsubsection{Tables based on the ``diff'' stage of IPP}
 \label{sec:schemadiff}
 
@@ -1228 +1300 @@
 PSPS Table & \multicolumn{2}{c}{column names} & comments \\
 \hline
-FrameMeta & raBore & decBore & RA/Dec of telescope boresite \\
+FrameMeta & raBore & decBore & R.A./Dec of telescope boresite \\
 %- where the telescope was pointed when image was taken \\
-ObjectThin & raMean & decMean & mean RA and Dec from single exposure, calibrated against 2MASS \\
-ObjectThin & raStack & decStack & mean RA and Dec calculated from \ippstage{stack} skycells \\
-Detection & RA & Dec & RA and Dec for single exposure detections \\
-StackObjectThin & (grizy)ra & (grizy)dec & RA and Dec calculated from individual \ippstage{stack} skycells \\
-DiffDetection & RA & Dec & RA and Dec for single \ippstage{diff} exposure detections  \\
-DiffDetObject & RA & Dec & similar to raMean/decMean, calculated for \ippstage{diff} objects \\
-GaiaFrameCoordinate & RA & Dec & \textbf{Best RA and Dec, recalibrated to Gaia (DR1 only).}\\%\tablenotemark{a} \\ 
+ObjectThin & raMean & decMean & mean R.A. and Dec from single exposure, calibrated against 2MASS \\
+ObjectThin & raStack & decStack & mean R.A. and Dec calculated from \ippstage{stack} skycells \\
+Detection & R.A. & Dec & R.A. and Dec for single exposure detections \\
+StackObjectThin & (grizy)ra & (grizy)dec & R.A. and Dec calculated from individual \ippstage{stack} skycells \\
+DiffDetection & R.A. & Dec & R.A. and Dec for single \ippstage{diff} exposure detections  \\
+DiffDetObject & R.A. & Dec & similar to raMean/decMean, calculated for \ippstage{diff} objects \\
+GaiaFrameCoordinate & R.A. & Dec & \textbf{Best R.A. and Dec, recalibrated to Gaia (DR1 only).}\\%\tablenotemark{a} \\ 
 \hline
 \end{tabular}
 \end{center}
-%\tablenotetext{a}{This is the best and most accurate RA and Dec to use if interested in the static sky.}
+%\tablenotetext{a}{This is the best and most accurate R.A. and Dec to use if interested in the static sky.}
 \label{table:radec}
 \end{table*}
 
 
-\subsection{Which RA and Dec to use?}
+\subsection{Which R.A. and Dec to use?}
 \label{sec:schemaradec}
 
@@ -1255 +1327 @@
 proper motion or moving objects, it is best to use coordinates from
 \ippdbtable{GaiaFrameCoordinate} if using DR1, as this is the weighted mean
-RA and Dec (similar to \ippdbtable{ObjectThin}), but tied to the Gaia system.
+R.A. and Dec (similar to \ippdbtable{ObjectThin}), but tied to the Gaia system.
 This information is in a separate table and not part of \ippdbtable{ObjectThin} because the mean properties were calculated and ingested
 into PSPS prior to Gaia's DR1.  \ippdbtable{ObjectThin}'s \ippdbcolumn{raMean} and
@@ -1276 +1348 @@
 There are multiple columns within the schema that are indexed and
 designed to be used to join tables together. Generally, if a column
-name ends in ``\ippdbcolumn{ID}", it is designed to be joined to other
+name ends in ``\ippdbcolumn{ID}'', it is designed to be joined to other
 tables, either to system metadata tables (examples include
 \ippdbcolumn{filterID}, \ippdbcolumn{surveyID}, \ippdbcolumn{ccdID}), or to
@@ -1301 +1373 @@
 different sources or objects have an index, called \ippdbcolumn{objID}.
 \ippdbcolumn{objID} is only unique for the object type of tables, and is
-loosely based on RA and Dec, see Section~\ref{sec:schemaobjid} for
+loosely based on R.A. and Dec, see Section~\ref{sec:schemaobjid} for
 more information. It is possible to use the \ippdbcolumn{objID} to get a
-rough estimate of the RA and Dec, but this should not be used for the
-definitive RA and Dec. Use \ippdbtable{ObjectThin} to get the RA and Dec
+rough estimate of the R.A. and Dec, but this should not be used for the
+definitive R.A. and Dec. Use \ippdbtable{ObjectThin} to get the R.A. and Dec
 calibrated to 2MASS, and use \ippdbtable{GaiaFrameCoordinate}(for DR1) or
-\ippdbtable{ObjectThin}(for DR2)to get the RA and Dec calibrated to Gaia
+\ippdbtable{ObjectThin}(for DR2)to get the R.A. and Dec calibrated to Gaia
 astrometry.  When available and possible, if joining 2 tables and they
 both have the same column name like \ippdbcolumn{uniquePspsXXId}, join
@@ -1364 +1436 @@
 \label{sec:schemanulls}
 
-The PSPS uses \texttt{-999} to denote \texttt{NULL} values, as PSPS is based off of CasJobs which also does not use NULL. The justification for this is  explained at the following url: \url{http://skyserver.sdss.org/edr/en/sdss/skyserver/}. Specifically, they state "We also insist that all fields are non-null. These integrity constraints are invaluable tools in detecting errors during loading and they aid tools that automatically navigate the database.", and since our own database design has in its roots many of the same parts as the SDSS database, we also adopt this convention of non-null fields.
-
+% https://skyserver.sdss.org/edr/en/sdss/skyserver is OK (2020.08.13)
+
+The PSPS uses \texttt{-999} to denote \texttt{NULL} values, as PSPS is
+based off of CasJobs which also does not use NULL. The justification
+for this is explained by \cite{Szalay2002}: 
+% at the following url: \url{https://skyserver.sdss.org/edr/en/sdss/skyserver/}. 
+% Specifically, they state
+``We also insist that all fields are non-null. These
+integrity constraints are invaluable tools in detecting errors during
+loading and they aid tools that automatically navigate the database''
+\citep[see also][]{Gray2002}.  
+Since our own database design has in its roots many of the same
+parts as the SDSS database, we also adopt this convention of non-null
+fields.
+
+% the Szalay et al (2001) reference above is a technical report only on the SDSS.  There is a possibly-related publication in :
+% https://www.springer.com/gp/book/9783540424680
+
+% Szalay, A. S., Gray, J., Kunszt, P., Thakar, A., & Slutz, D. 2001, in Mining
+% the Sky, ed. A. J. Banday, S. Zaroubi, & M. Bartelmann (Berlin:
+% Springer), 99
+
+% the paper itself is on arxiv:
+% https://arxiv.org/abs/cs/0202013
 
 %Some of the Flag tables are of type \texttt{BIGINT}.  Care should be taken when doing bitmask queries with a \texttt{BIGINT}. Specifically, the bitmask needs to be recast as a BIGINT to force it to be of a proper size. 
@@ -1416 +1510 @@
 \parheading{Camera Stage} The \ippstage{camera} stage started with these 375,573 exposures, of which 374,521 ($99.7\%$) completed processing.  The other exposures failed due to: insufficient stars for the astrometric analysis, failure of single chip astrometry to converge, or failure of mosaic astrometry, usually too many failed chips. %Of those, 374446 were ingested into the DVO. These are the number of exposures we expect to see in the PSPS after loading.
 
-\parheading{Warp Stage} The \ippstage{warp} stages started off with a larger number of exposures than expected: 379,973 instead of 374,521.  This was due from some challenges in managing the remote processing on the clusters at Los Alamos National Laboratory and the University of Hawaii computer cluster (see Paper II).  Data transfer failures between the remote clusters and the IPP main cluster required re-queuing and re-running the analysis for some warps in a way that resulted in temporary double-counting.  Of the 379,973 exposures processed, 374,339 ($98.5\%$) are unique, and 1,234 are duplicates. Of the 379,973 exposures, 379,551 ($99.9\%$) have good quality. The \ippstage{warp} stage is the first stage that repartitions the exposures into the skycell tessellation, and since all later stages process on a skycell level rather than an exposure level, we note that the \ippstage{warp} stage yields 206,177 distinct skycells, with multiple warp skycell images from the different exposures for each skycell.
+\parheading{Warp Stage} The \ippstage{warp} stages started off with a larger number of exposures than expected: 379,973 instead of 374,521.  This was due from some challenges in managing the remote processing on the clusters at Los Alamos National Laboratory and the University of Hawai`i computer cluster (see Paper II).  Data transfer failures between the remote clusters and the IPP main cluster required re-queuing and re-running the analysis for some warps in a way that resulted in temporary double-counting.  Of the 379,973 exposures processed, 374,339 ($98.5\%$) are unique, and 1,234 are duplicates. Of the 379,973 exposures, 379,551 ($99.9\%$) have good quality. The \ippstage{warp} stage is the first stage that repartitions the exposures into the skycell tessellation, and since all later stages process on a skycell level rather than an exposure level, we note that the \ippstage{warp} stage yields 206,177 distinct skycells, with multiple warp skycell images from the different exposures for each skycell.
 
 \parheading{Stack to Skycal Stages} The \ippstage{stack} stage operates on 200,730 distinct skycells with up to five filter images per skycell.  A total of 200,725 stack skycells have good quality. There are fewer stack skycells than the 206,177 warp skycells listed above because stacks are not generated for skycells with Declination $< -30\degrees$.  Stacks generated below this Declination limit would have significantly poorer coverage and are of limited utility.  A total of 200,720 distinct skycells were processed by the static sky stage and all have good quality. The \ippstage{skycal} stage processed 200,722 skycells, of which 2 were essentially duplicate \ippstage{stacks} (same inputs, same skycells), of which 200,684 completed with good quality.
@@ -1431 +1525 @@
 %{\color{red} I have the bulk of the information here, but I do not know the best way to organize what is missing}
 
-% {\em Missing from ObjectThin/MeanObject}: These were loaded via OB batches, there were 116252 batches, subdivided by individual DVO files (each DVO file covers specific RA/Dec ranges).  Of the 116252 batches, 2902 batches were only partially ingested into PSPS; this represents 2.5\% of the total number of batches, and 1.2\% of the total number of objects.  The missing batch data will be released shortly after DR1.
+% {\em Missing from ObjectThin/MeanObject}: These were loaded via OB batches, there were 116252 batches, subdivided by individual DVO files (each DVO file covers specific R.A./Dec ranges).  Of the 116252 batches, 2902 batches were only partially ingested into PSPS; this represents 2.5\% of the total number of batches, and 1.2\% of the total number of objects.  The missing batch data will be released shortly after DR1.
 
 % {\em Missing Forced Objects}: We expect 113665 \ippdbtable{Forced Object} batches.  There are 7086 batches that have been partially loaded into PSPS, the rest of the batches are fully loaded.  These missing batches will not be included in DR1, they will be added shortly after DR1.
@@ -1462 +1556 @@
 After delivery of the DR2 data to STScI, internal consistency tests
 revealed some problems for data in the vicinity of the celestial north
-pole.  This issues is described in some detail in Paper IV.  In short,
+pole.  This issue is described in some detail in Paper IV.  In short,
 the on-the-fly astrometric calibration performed during the PV3
 analysis (Section~\ref{sec:chipandcamera}) relied on an astrometric
@@ -1483 +1577 @@
 the affected images are set to {\tt NULL} as these values cannot
 be trusted.  A list of the affected skycells is provided at MAST and
-users are advised to be cautious of measurements from these regions.
+users are advised to be cautious of measurements from these regions.  
+%
+\textadd{The problem skycells are almost entirely north of Dec =
+  80\degrees, comprising roughly 21 of the 313 square degrees
+  in this region.}
+%
 A reprocessing of the polar regions north of Dec = 70\degrees\ is
-underway (Nov 2019) and will be released to users in the future.
+underway and will be released to users in the future.
 
 %{\color{red} The diff DVO database }
@@ -1599 +1698 @@
 \section{Conclusion}
 \label{sec:conclusion}
-The Pan-STARRS database contains 10,723,304,629 objects. It is the largest data release from the largest digital sky survey to date, distilling the information from 1.6 petabytes of images and tables into a form that is accessible to the astronomical community through MAST. Nevertheless, sifting through such a large database can prove daunting, and this work is intended to describe the primary tables and quantities within the database, together with example queries. Data from Pan-STARRS has been used for myriad purposes including detecting moving objects within the solar system (and in the case of ‘Oumuamua, from outside it!), the analysis of tens of thousands of high-energy transient events, mapping the 3D structure of dust within our Galaxy, and studies of the large scale structure of our Universe. Yet these only scratch the surface, and it is likely that mining the database will lead to discoveries that were missed and correlations that were overlooked. As we enter the era of multi-messenger astrophysics, the Pan-STARRS data products will be essential to identifying the host galaxies and electromagnetic counterparts of events detected by gravitational wave, high-energy particle, neutrino and radio observatories. While we have provided various tools to work with this data release, we anticipate that it will spur the development of new interfaces and ways of working with high-dimensional datasets. This work will be critical to science with future surveys such as LSST. Combining this Pan-STARRS data release with other large catalogs such as \emph{GALEX}, 2MASS and \emph{Gaia} will provide a rich, high-dimensional dataset that will enable new scientific studies, and may yield astronomical treasures that we have not even begun to imagine.
+The Pan-STARRS database contains 10,723,304,629 objects. It is the
+largest data release from the largest digital sky survey to date,
+distilling the information from 1.6 petabytes of images and tables
+into a form that is accessible to the astronomical community through
+MAST. Nevertheless, sifting through such a large database can prove
+daunting, and this work is intended to describe the primary tables and
+quantities within the database, together with example queries. Data
+from Pan-STARRS has been used for myriad purposes including detecting
+moving objects within the solar system (and in the case of 1I/2017 U1 (‘Oumuamua),
+from outside it!), the analysis of tens of thousands of high-energy
+transient events, mapping the 3D structure of dust within our Galaxy,
+and studies of the large scale structure of our Universe. Yet these
+only scratch the surface, and it is likely that mining the database
+will lead to discoveries that were missed and correlations that were
+overlooked. As we enter the era of multi-messenger astrophysics, the
+Pan-STARRS data products will be essential to identifying the host
+galaxies and electromagnetic counterparts of events detected by
+gravitational wave, high-energy particle, neutrino and radio
+observatories. While we have provided various tools to work with this
+data release, we anticipate that it will spur the development of new
+interfaces and ways of working with high-dimensional datasets. This
+work will be critical to science with future surveys such as
+LSST. Combining this Pan-STARRS data release with other large catalogs
+such as \emph{GALEX}, 2MASS and \emph{Gaia} will provide a rich,
+high-dimensional dataset that will enable new scientific studies, and
+may yield astronomical treasures that we have not even begun to
+imagine.
 
 {\color{red} }
@@ -1610 +1735 @@
 The Pan-STARRS1 Surveys (PS1) have been made possible through
 contributions of the Institute for Astronomy, the University of
-Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its
+Hawai`i, the Pan-STARRS Project Office, the Max-Planck Society and its
 participating institutes, the Max Planck Institute for Astronomy,
 Heidelberg, and the Max Planck Institute for Extraterrestrial Physics,
@@ -1625 +1750 @@
 and Betty Moore foundation.
 
+% http://www.cosmos.esa.int/gaia : OK
+% http://www.cosmos.esa.int/web/gaia/dpac/consortium : OK
+ 
 This work has made use of data from the European Space Agency (ESA)
 mission {\em Gaia} (\url{http://www.cosmos.esa.int/gaia}), processed by
@@ -1636 +1764 @@
 \bibliographystyle{apj}
 \bibliography{dataproducts}{}
-%\input{dataproducts.bbl}
+% \input{dataproducts.bbl}
 
 \appendix
@@ -1647 +1775 @@
 \label{sec:query}
 
-This section shows example queries for the \PS\ database. The
+This section shows example queries for the \PS\ DR2 database. The
 progression will be from simple queries to more complicated queries.
 SQL has no requirements on case.  We adopt the standard convention of
@@ -1653 +1781 @@
 and \texttt{CamelCase} for the tables and columns within the PSPS
 database schema.  The queries given below may all be run from the
-CasJobs tab on the MAST web site.  Note the some of the later queries
-rely on myDB tables generated in the earlier queries.
+CasJobs tab on the MAST web site \textadd{using the context
+  ``PanSTARRS\_DR2''.}  Note the some of the later queries rely on
+myDB tables generated in the earlier queries.  \textadd{The names for
+  these output tables are surrounded by square brackets in the
+  examples.  These brackets are always allowed, but are {\em required} if
+  the table name includes spaces or reserved
+  words\footnote{\url{https://docs.microsoft.com/en-us/sql/relational-databases/databases/database-identifiers}}
+  Also beware that cut-and-paste in some browsers can convert the
+  underscore characters to space.}
  
 %\noindent Unless otherwise specified, assume that these queries are run off of the PSI query page ({\color{red} arrrgh this needs to be updated because we aren't using psi, right? what do I do KCC? } \url{http:\/\/panstarrs.stsci.edu/PSI/query\_page.php} ), under 'select database' use a database that starts with 'PanSTARRS\_3PI' (this will be updated as future data releases occur), paste the query in the Query box, and select the 'slow queue'.  Set 'MyDB table for slow queue results:' to be query1, query2, etc as applicable. The progression will be from simple queries to more complicated queries, with a focus on queries for DR1 followed by queries applicable to later data releases.
@@ -1661 +1796 @@
 \item \textbf{Counting the number of rows in a large table}
 
-This is an example of a simple query, it needs to be run in the slow queue. The difference between \texttt{COUNT\_BIG()} and \texttt{COUNT()} is that \texttt{COUNT\_BIG()} returns a \texttt{BIGINT}, while \texttt{COUNT()} returns an \texttt{INT}.  The PSPS tables are so large that \texttt{COUNT()}, which goes up to 2.14 billion, is too small of a number. Users should choose the method of counting rows that is appropriate for their data ranges. Unless it involves large tables and large areas of sky, \texttt{COUNT()} is recommended.
+This is an example of a simple query, it needs to be run in the slow
+queue. The difference between \texttt{COUNT\_BIG()} and
+\texttt{COUNT()} is that \texttt{COUNT\_BIG()} returns a
+\texttt{BIGINT}, while \texttt{COUNT()} returns an \texttt{INT}.  The
+PSPS tables are so large that \texttt{COUNT()}, which goes up to 2.14
+billion, is too small of a number. Users should choose the method of
+counting rows that is appropriate for their data ranges. Unless it
+involves large tables and large areas of sky, \texttt{COUNT()} is
+recommended.  \textadd{However, if the result is too large, using
+  \texttt{COUNT()} will result in an aritmetic overflow exception.}
 
 %% careful with these: underscores from PDFs convert to spaces when copy-paste-ing
@@ -1686 +1830 @@
 AND decMean <  0.1 \\
 }
-% EAM : 2019.11.08 : OK, I get 3867 objects against DR2
-
-This returns 3867 objects. The majority of these objects have only been detected once.  
+% EAM : 2019.11.08 : OK, I get 3868 objects against DR2
+
+This returns 3868 objects. The majority of these objects have only been detected once.  
 
 \item \textbf{Make a simple text histogram of ObjectThin.nDetections for a rectangular patch of sky}
@@ -1694 +1838 @@
 It is possible to save queries into your own personal MyDB, as well as
 to make queries on your MyDB. Do the query from above, but save it to
-your MyDB as 'MyDBtest'.  Run the following query on your MyDB to make
-a histogram of \ippdbcolumn{nDetections}.
+your MyDB as 'MyDBtest'.  Run the following query on your MyDB (MyDB
+context) to make a histogram of \ippdbcolumn{nDetections}.
 
 %Verify that the query is complete from the queued jobs page.  Run the following query in the fast queue, but select the Database to be 'MyDB'
@@ -1735 +1879 @@
 AND decMean <  0.1 
 }
-% EAM : 2019.11.08 : OK, I get 747 objects from DR2
-
-This returns 747 objects, a significant reduction from the 3867 returned in query \# 2. 
+% EAM : 2019.11.08 : OK, I get 748 objects from DR2
+
+This returns 748 objects, a significant reduction from the 3867 returned in query \# 2. 
 
 \item \textbf{Select \ippstage{stack} PSF magnitudes for all filters for a rectangular patch of sky}
@@ -1754 +1898 @@
 AND decMean <  0.1 \\
 }
-% EAM : 2019.11.08 : OK, I get 1805 objects from DR2
-
-This returns 1805 objects. 
+% EAM : 2019.11.08 : OK, I get 1806 objects from DR2
+
+This returns 1806 objects. 
 
 \item \textbf{An example of finding rows with \texttt{NULL} values, using \texttt{TOP} to limit results}
@@ -1777 +1921 @@
 \item \textbf{Basic search using \texttt{BETWEEN} to limit ranges}
  
-Similar to query \# 5, except uses \texttt{BETWEEN} to limit RA and Dec ranges as well as iPSFMag ranges.
+Similar to query \# 5, except uses \texttt{BETWEEN} to limit R.A. and
+Dec ranges as well as iPSFMag ranges.
 
 % QUERY 07
@@ -1794 +1939 @@
 \item \textbf{Using built-in functions to do a box search}
 
-ObjectThin contains Hierarchical triangular mesh information, making it possible to use the built in function dbo.fGetObjFromRectEq(minra, mindec, maxra, maxdec) to do a rectangular search. Tables which have htm, cx,cy, cz can use this built in function.
+ObjectThin contains Hierarchical triangular mesh information, making
+it possible to use the built in function dbo.fGetObjFromRectEq(minra,
+mindec, maxra, maxdec) to do a rectangular search. Tables which have
+htm, cx,cy, cz can use this built in function.
 
 % QUERY 08
@@ -1808 +1956 @@
 \item \textbf{Using built in functions to do a cone search}
 
-ObjectThin contains Hierarchical triangular mesh information, making it possible to use the built in function dbo.fGetNearbyObjEq(ra, dec, conesize(deg)) to do a radial search for objects near a given ra and dec (cone search). Tables which have htm, cx,cy, cz can use this built in function.
+ObjectThin contains Hierarchical triangular mesh information, making
+it possible to use the built in function dbo.fGetNearbyObjEq(ra, dec,
+conesize(arcmin)) to do a radial search for objects near a given ra and
+dec (cone search). Tables which have htm, cx,cy, cz can use this built
+in function.  \textadd{The query below returns the objects within 0.2 arcmin of
+the coordinate 56.85, 24.12.  Note that only one of these objects was
+detected in a \gps-band image and thus has a valid value for the \gps-magnitude.}
 
 % QUERY 09
@@ -1818 +1972 @@
 ON o.objID = n.objID
 }
-% EAM : 2019.11.10 : OK, I get 40 objects from DR2
+% EAM : 2019.11.10 : OK, I get 41 objects from DR2
 
 \item \textbf{Cone search of high fidelity stellar-like objects}
 
-We want to get all objects with R degrees of a given position that are high fidelity stellar-like objects.
-We get all objects within 0.2 degree of RA=334.0 and Dec=0.0 which have mean magnitudes in griz (i.e. at least 1 detection in each band that can be used for the mean mag). In addition, we require QfPerfect $> 0.85$ in all bands. We select stars with small ($<0.05$) difference between Kron and PSF magnitudes.
+We want to get all objects with R degrees of a given position that are
+high fidelity stellar-like objects.  We get all objects within 0.2
+degrees of R.A.=334.0 and Dec=0.0 which have mean magnitudes in griz
+(i.e. at least 1 detection in each band that can be used for the mean
+mag). In addition, we require QfPerfect $> 0.85$ in all bands. We
+select stars with small ($<0.05$) difference between Kron and PSF
+magnitudes.
 
 % QUERY 10
@@ -1894 +2053 @@
 
 Star CSS J030521.9+013231 (Catalina Sky Survey), 584630948352256
-(GAIA) is an RR Lyrae with period = 0.55547 days and coordinates RA =
+(GAIA) is an RR Lyrae with period = 0.55547 days and coordinates R.A. =
 46.341468915923 and DEC = 1.54199810825252 (ref. GAIA DR2,
 2018yCat.1345....0G). In the following, we obtain the PSF and aperture
@@ -1907 +2066 @@
    ra AS RA\_GAIA, dec AS DEC\_GAIA,
    phot\_g\_mean\_mag AS Gmag
-   INTO mydb.RRL\_584630948352256
+   INTO mydb.[RRL\_584630948352256]
    FROM gaia\_source
    WHERE source\_id = 584630948352256
@@ -2048 +2207 @@
 %}
 
-%\item extracting a light curve for an object by RA and Dec using the Detection table (DR2)
-
-%If the \ippdbcolumn{objID} of the object is not know, it is necessary to do a join on \ippdbtable{ObjectThin} to search by RA and Dec.  This method is much slower than to search by the \ippdbcolumn{objID}.
+%\item extracting a light curve for an object by R.A. and Dec using the Detection table (DR2)
+
+%If the \ippdbcolumn{objID} of the object is not know, it is necessary to do a join on \ippdbtable{ObjectThin} to search by R.A. and Dec.  This method is much slower than to search by the \ippdbcolumn{objID}.
 
 %\item extracting a light curve for an object  with a known \ippdbcolumn{objID} using the \ippdbtable{ForcedWarpMeasurement} table(DR2)
 
-%\item extracting a light curve for an object by RA and Dec using the \ippdbtable{ForcedWarpMeasurement} table (DR2)
+%\item extracting a light curve for an object by R.A. and Dec using the \ippdbtable{ForcedWarpMeasurement} table (DR2)
 
 %\item extracting a light curve for an object  with a known \ippdbcolumn{objID} using the \ippdbtable{DiffDetection} table(DR2)
 
-%\item extracting a light curve for an object by RA and Dec using the \ippdbtable{DiffDetection} table (DR2)
+%\item extracting a light curve for an object by R.A. and Dec using the \ippdbtable{DiffDetection} table (DR2)
 
 \end{enumerate}
@@ -2175 +2334 @@
 %% \note{table order is a bit funny; compare with text}
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ObjectInfoFlags}
 \begin{center}
@@ -2227 +2386 @@
 
 % \FloatBarrier
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ObjectQualityFlags}
 \begin{center}
@@ -2252 +2411 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ObjectFilterFlags}
 \begin{center}
@@ -2290 +2449 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ImageFlags}
 \begin{center}
@@ -2317 +2476 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ForcedGalaxyShapeFlags}
 \begin{center}
@@ -2337 +2496 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{DetectionFlags}
 \begin{center}
@@ -2385 +2544 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{DetectionFlags2}
 \begin{center}
@@ -2425 +2584 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{DetectionFlags3}
 \begin{center}
@@ -2721 +2880 @@
 %{\color{red} needs to be added}
 
+In this section, we present the contents of all DR2 tables, along with
+the expected \ippstage{diff} tables for DR3.  These listings were
+automatically generated from the XML code used to define the PSPS
+tables, with light editing to clean up the formatting for some of the
+units and equations.
+
 \subsection{Object / Mean Object Tables}
 
-\begin{table}[b]
+\begin{table}[htb]
 
 \caption{ObjectThin: Contains the positional information for objects
@@ -2804 +2969 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{MeanObject: Contains the mean photometric information for objects based on the single epoch data, calculated as described in \citet{Magnier2013}.  To be included in this table, an object must be bright enough to have been detected at least once in an individual exposure.  PSF, Kron (1980), and aperture magnitudes and statistics are listed for all filters.}
 \begin{center}
@@ -2853 +3018 @@
 %\end{document}
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{GaiaFrameCoordinate: PSPS objects calibrated against Gaia astrometry}
 \begin{center}
@@ -2883 +3048 @@
 \subsection{Single Exposure Detection Tables}
 
-\begin{table}[b]
-\caption{FrameMeta: Contains metadata related to an individual exposure.  A "Frame" refers to the collection of all images obtained by the 60 OTA devices in the camera in a single exposure. The camera configuration, telescope pointing, observation time, and astrometric solution from the detector focal plane (L,M) to the sky (RA,Dec) is provided.}
+\begin{table}[htb]
+\caption{FrameMeta: Contains metadata related to an individual exposure.  A "Frame" refers to the collection of all images obtained by the 60 OTA devices in the camera in a single exposure. The camera configuration, telescope pointing, observation time, and astrometric solution from the detector focal plane (L,M) to the sky (R.A.,Dec) is provided.}
 \begin{center}
 \resizebox{\textwidth}{!}{%
@@ -2914 +3079 @@
 raBore & degrees & FLOAT & -999  &Right ascension of telescope boresight.\\
 decBore & degrees & FLOAT & -999  &Declination of telescope boresight.\\
-ctype1 & - & VARCHAR(100) &   &Name of astrometric projection in RA.\\
+ctype1 & - & VARCHAR(100) &   &Name of astrometric projection in R.A..\\
 ctype2 & - & VARCHAR(100) &   &Name of astrometric projection in Dec.\\
 crval1 & degrees & FLOAT & -999  &Right ascension corresponding to reference pixel.\\
 crval2 & degrees & FLOAT & -999  &Declination corresponding to reference pixel.\\
-crpix1 & pixels & FLOAT & -999  &Reference pixel for RA.\\
+crpix1 & pixels & FLOAT & -999  &Reference pixel for R.A..\\
 crpix2 & pixels & FLOAT & -999  &Reference pixel for Dec.\\
-cdelt1 & degrees/pixel & FLOAT & -999  &Pixel scale in RA.\\
+cdelt1 & degrees/pixel & FLOAT & -999  &Pixel scale in R.A..\\
 cdelt2 & degrees/pixel & FLOAT & -999  &Pixel scale in Dec.\\
-pc001001 & - & FLOAT & -999  &Linear transformation matrix element between focal plane pixel L and RA.\\
-pc001002 & - & FLOAT & -999  &Linear transformation matrix element between focal plane pixel M and RA.\\
+pc001001 & - & FLOAT & -999  &Linear transformation matrix element between focal plane pixel L and R.A..\\
+pc001002 & - & FLOAT & -999  &Linear transformation matrix element between focal plane pixel M and R.A..\\
 pc002001 & - & FLOAT & -999  &Linear transformation matrix element between focal plane pixel L and Dec.\\
 pc002002 & - & FLOAT & -999  &Linear transformation matrix element between focal plane pixel M and Dec.\\
 polyOrder & - & TINYINT & 255  &Polynomial order of astrometric fit between detector focal plane and sky.\\
-pca1x3y0 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^3$ $y^0$) for RA.\\
-pca1x2y1 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^2$ $y^1$) for RA.\\
-pca1x1y2 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^1$ $y^2$) for RA.\\
-pca1x0y3 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^0$ $y^3$) for RA.\\
-pca1x2y0 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^2$ $y^0$) for RA.\\
-pca1x1y1 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^1$ $y^1$) for RA.\\
-pca1x0y2 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^0$ $y^2$) for RA.\\
+pca1x3y0 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^3$ $y^0$) for R.A..\\
+pca1x2y1 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^2$ $y^1$) for R.A..\\
+pca1x1y2 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^1$ $y^2$) for R.A..\\
+pca1x0y3 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^0$ $y^3$) for R.A..\\
+pca1x2y0 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^2$ $y^0$) for R.A..\\
+pca1x1y1 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^1$ $y^1$) for R.A..\\
+pca1x0y2 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^0$ $y^2$) for R.A..\\
 pca2x3y0 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^3$ $y^0$) for Dec.\\
 pca2x2y1 & - & FLOAT & -999  &Polynomial coefficient for the astrometric fit component ($x^2$ $y^1$) for Dec.\\
@@ -2949 +3114 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ImageMeta: Contains metadata related to an individual OTA image that comprises a portion of the full exposure.  The characterization of the image quality, the detrends applied, and the astrometric solution from the raw pixels (X,Y) to the detector focal plane (L,M) is provided.}
 \begin{center} %cheaing here, if I do resizebox it compiles
@@ -2958 +3123 @@
 column name & units & data type & default & description\\
 \hline
-imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 * frameID + ccdID).\\
+imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 $\times$ frameID + ccdID).\\
 frameID & - & INT & NA  &Unique frame/exposure identifier.\\
 ccdID & - & SMALLINT & NA  &OTA identifier based on location in the focal plane, specific to an individual device.\\
@@ -2965 +3130 @@
 bias & adu & REAL & -999  &OTA bias level.\\
 biasScat & adu & REAL & -999  &Scatter in bias level.\\
-sky & $Jy/arcsec^2$ & REAL & -999  &Mean sky brightness.\\
-skyScat & $Jy/arcsec^2$ & REAL & -999  &Scatter in mean sky brightness.\\
+sky & Jy arcsec$^{-2}$ & REAL & -999  &Mean sky brightness.\\
+skyScat & Jy arcsec$^{-2}$ & REAL & -999  &Scatter in mean sky brightness.\\
 nDetect & - & INT & -999  &Number of detections in this image.\\
 detectionThreshold & magnitudes & REAL & -999  &Reference magnitude for detection efficiency calculation.\\
@@ -2988 +3153 @@
 momentMajor & arcsec & REAL & -999  &PSF major axis second moment.\\
 momentMinor & arcsec & REAL & -999  &PSF minor axis second moment.\\
-momentM2C & $arcsec^2$ & REAL & -999  &Moment $M2C = M_{xx} - M_{yy}$.\\
-momentM2S & $arcsec^2$ & REAL & -999  &Moment $M2S = 2 * M_{xy}$.\\
-momentM3 & $arcsec^2$ & REAL & -999  &trefoil second moment = $sqrt( (M_{xxx} - 3 * M_{xyy})^2 + (3 * M_{xxy} - M_{yyy})^2 )$.\\
-momentM4 & $arcsec^2$ & REAL & -999  &quadrupole second moment = $sqrt( (M_{xxxx} - 6 * M_{xxyy} + M_{yyyy})^2 + (4 * M_{xxxy} - 4 * M_{xyyy})^2 )$.\\
+momentM2C & arcsec$^2$ & REAL & -999  &Moment $M2C = M_{xx} - M_{yy}$.\\
+momentM2S & arcsec$^2$ & REAL & -999  &Moment $M2S = 2 M_{xy}$.\\
+momentM3 & arcsec$^2$ & REAL & -999  &trefoil second moment = $\sqrt{(M_{xxx} - 3 M_{xyy})^2 + (3 M_{xxy} - M_{yyy})^2}$.\\
+momentM4 & arcsec$^2$ & REAL & -999  &quadrupole second moment = $\sqrt{(M_{xxxx} - 6 M_{xxyy} + M_{yyyy})^2 + (4 M_{xxxy} - 4 M_{xyyy})^2}$.\\
 apResid & magnitudes & REAL & -999  &Residual of aperture corrections.\\
 dapResid & magnitudes & REAL & -999  &Scatter of aperture corrections.\\
@@ -3043 +3208 @@
 
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{Detection: Contains single epoch photometry of individual detections from a single exposure.  The identifiers connecting the detection back to the original image and to the object association are provided.  PSF, aperture, and \citet{Kron1980} photometry are included, along with sky and detector coordinate positions.}
 \begin{center}
@@ -3059 +3224 @@
 filterID & - & TINYINT & NA  &Filter identifier.  Details in the Filter table.\\
 surveyID & - & TINYINT & NA  &Survey identifier.  Details in the Survey table.\\
-imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 * frameID + ccdID).\\
+imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 $\times$ frameID + ccdID).\\
 randomDetID & - & FLOAT & NA  &Random value drawn from the interval between zero and one. \\
 dvoRegionID & - & INT & -1  &Internal DVO region identifier.\\
@@ -3093 +3258 @@
 psfChiSq & - & REAL & -999  &Reduced chi squared value of the PSF model fit.\\
 psfLikelihood & - & REAL & -999  &Likelihood that this detection is best fit by a PSF.\\
-momentXX & $arcsec^2$ & REAL & -999  &Second moment $M_{xx}$.\\
-momentXY & $arcsec^2$ & REAL & -999  &Second moment $M_{xy}$.\\
-momentYY & $arcsec^2$ & REAL & -999  &Second moment $M_{yy}$.\\
+momentXX & arcsec$^2$ & REAL & -999  &Second moment $M_{xx}$.\\
+momentXY & arcsec$^2$ & REAL & -999  &Second moment $M_{xy}$.\\
+momentYY & arcsec$^2$ & REAL & -999  &Second moment $M_{yy}$.\\
 momentR1 & arcsec & REAL & -999  &First radial moment.\\
-momentRH & $arcsec^{0.5}$ & REAL & -999  &Half radial moment ($r^{0.5}$ weighting).\\
-momentM3C & $arcsec^2$ & REAL & -999  &Cosine of trefoil second moment term: $r^2 cos(3 theta) = M_{xxx} - 3 * M_{xyy}$.\\
-momentM3S & $arcsec^2$ & REAL & -999  &Sine of trefoil second moment: $r^2 sin (3 theta) = 3 * M_{xxy} - M_{yyy}$.\\
-momentM4C & $arcsec^2$ & REAL & -999  &Cosine of quadrupole second moment: $r^2 cos (4 theta) = M_{xxxx} - 6 * M_{xxyy} + M_{yyyy}.$\\
-momentM4S & $arcsec^2$ & REAL & -999  &Sine of quadrupole second moment: $r^2 sin (4 theta) = 4 * M_{xxxy} - 4 * M_{xyyy}$.\\
+momentRH & arcsec$^{0.5}$ & REAL & -999  &Half radial moment ($r^{0.5}$ weighting).\\
+momentM3C & arcsec$^2$ & REAL & -999  &Cosine of trefoil second moment term: $r^2 \cos(3 \theta) = M_{xxx} - 3 M_{xyy}$.\\
+momentM3S & arcsec$^2$ & REAL & -999  &Sine of trefoil second moment: $r^2 \sin (3 \theta) = 3 M_{xxy} - M_{yyy}$.\\
+momentM4C & arcsec$^2$ & REAL & -999  &Cosine of quadrupole second moment: $r^2 \cos (4 \theta) = M_{xxxx} - 6 M_{xxyy} + M_{yyyy}.$\\
+momentM4S & arcsec$^2$ & REAL & -999  &Sine of quadrupole second moment: $r^2 \sin (4 \theta) = 4 M_{xxxy} - 4 M_{xyyy}$.\\
 apFlux & Jy & REAL & -999  &Flux in seeing-dependent aperture.\\
 apFluxErr & Jy & REAL & -999  &Error on flux in seeing-dependent aperture.\\
@@ -3109 +3274 @@
 kronFluxErr & Jy & REAL & -999  &Error on Kron (1980) flux.\\
 kronRad & arcsec & REAL & -999  &Kron (1980) radius.\\
-sky & $Jy/arcsec^2$ & REAL & -999  &Background sky level.\\
-skyErr & $Jy/arcsec^2$ & REAL & -999  &Error in background sky level.\\
+sky & Jy arcsec$^{-2}$ & REAL & -999  &Background sky level.\\
+skyErr & Jy arcsec$^{-2}$ & REAL & -999  &Error in background sky level.\\
 infoFlag & - & BIGINT & 0  &Information flag bitmask indicating details of the photometry.  \\
 & & & & Values listed in DetectionFlags.\\
@@ -3125 +3290 @@
 
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ImageDetEffMeta: Contains the detection efficiency information for a given individual OTA image.  Provides the number of recovered sources out of 500 injected fake source and statistics about the magnitudes of the recovered sources for a range of magnitude offsets.}
 \begin{center}
@@ -3134 +3299 @@
 column name & units & data type & default & description\\
 \hline
-imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 * frameID + ccdID).\\
+imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 $\times$ frameID + ccdID).\\
 frameID & - & INT & NA  &Unique frame/exposure identifier.\\
 magref & magnitudes & REAL & NA  &Detection efficiency reference magnitude.\\
@@ -3169 +3334 @@
 \subsection{Stack Tables}
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{StackMeta: Contains the metadata describing the stacked image produced from the combination of a set of single epoch exposures.  The nature of the \ippstage{stack} is given by the StackTypeID.  The astrometric and photometric calibration of the stacked image are listed.}
 \begin{center}
@@ -3239 +3404 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{StackObjectThin: Contains the positional and photometric information for point-source photometry of \ippstage{stack} detections.  The information for all filters are joined into a single row, with metadata indicating if this \ippstage{stack} object represents the primary detection.  Due to overlaps in the \ippstage{stack} tessellations, an object may appear in multiple \ippstage{stack} images.  The primary detection is the unique detection from the \ippstage{stack} image that provides the best coverage with minimal projection stretching.  All other detections of the object in that filter are secondary, regardless of their properties.  The detection flagged as best is the primary detection if that detection has a psfQf value greater than 0.98;  if that is not met, then any of the primary or secondary detections with the highest psfQf value is flagged as best.}
 \begin{center}
@@ -3296 +3461 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{StackObjectAttributes: Contains the PSF, \citet{Kron1980}, and aperture fluxes for all filters in a single row, along with point-source object shape parameters.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.
 }
@@ -3329 +3494 @@
 gpsfQfPerfect & - & REAL & -999  &PSF-weighted fraction of pixels totally unmasked for g filter \ippstage{stack} detection.\\
 gpsfChiSq & - & REAL & -999  &Reduced chi squared value of the PSF model fit for g filter \ippstage{stack} detection.\\
-gmomentXX & $arcsec^2$ & REAL & -999  &Second moment $M_{xx}$ for g filter \ippstage{stack} detection.\\
-gmomentXY & $arcsec^2$ & REAL & -999  &Second moment $M_{xy}$ for g filter \ippstage{stack} detection.\\
-gmomentYY & $arcsec^2$ & REAL & -999  &Second moment $M_{yy}$ for g filter \ippstage{stack} detection.\\
+gmomentXX & arcsec$^2$ & REAL & -999  &Second moment $M_{xx}$ for g filter \ippstage{stack} detection.\\
+gmomentXY & arcsec$^2$ & REAL & -999  &Second moment $M_{xy}$ for g filter \ippstage{stack} detection.\\
+gmomentYY & arcsec$^2$ & REAL & -999  &Second moment $M_{yy}$ for g filter \ippstage{stack} detection.\\
 gmomentR1 & arcsec & REAL & -999  &First radial moment for g filter \ippstage{stack} detection.\\
-gmomentRH & $arcsec^{0.5}$ & REAL & -999  &Half radial moment ($r^{0.5}$ weighting) for g filter \ippstage{stack} detection.\\
+gmomentRH & arcsec$^{0.5}$ & REAL & -999  &Half radial moment ($r^{0.5}$ weighting) for g filter \ippstage{stack} detection.\\
 gPSFFlux & Jy & REAL & -999  &PSF flux from g filter \ippstage{stack} detection.\\
 gPSFFluxErr & Jy & REAL & -999  &Error in PSF flux from g filter \ippstage{stack} detection.\\
@@ -3348 +3513 @@
 & & & & the deviation between PSF and Kron (1980) magnitudes, normalized \\
 & & & & by the PSF magnitude uncertainty.\\
-gsky & $Jy/arcsec^2$ & REAL & -999  &Residual background sky level at the g filter \ippstage{stack} detection.\\
-gskyErr & $Jy/arcsec^2$ & REAL & -999  &Error in residual background sky level at the g filter \ippstage{stack} detection.\\
+gsky & Jy arcsec$^{-2}$ & REAL & -999  &Residual background sky level at the g filter \ippstage{stack} detection.\\
+gskyErr & Jy arcsec$^{-2}$ & REAL & -999  &Error in residual background sky level at the g filter \ippstage{stack} detection.\\
 gzp & magnitudes & REAL & 0  &Photometric zeropoint for the g filter stack.  Necessary for converting\\
 & & & & listed fluxes and magnitudes back to measured ADU counts.\\
@@ -3364 +3529 @@
 \end{table}%
 
-\begin{table}[b]
-\caption{StackApFlx: Contains the unconvolved fluxes within the SDSS R5 (r = 3.00 arcsec), R6 (r = 4.63 arcsec), and R7 (r = 7.43 arcsec) apertures \citep{Stoughton2002}.  Convolved fluxes within these same apertures are also provided for images convolved to 6 sky pixels (1.5 arcsec) and 8 sky pixels (2.0 arcsec).  All filters are matched into a single row.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.}
+\begin{table}[htb]
+\caption{StackApFlx: Contains the unconvolved fluxes within the SDSS R5 (r = 3.00\arcsec), R6 (r = 4.63\arcsec), and R7 (r = 7.43\arcsec) apertures \citep{Stoughton2002}.  Convolved fluxes within these same apertures are also provided for images convolved to 6 sky pixels (1.5\arcsec) and 8 sky pixels (2.0\arcsec).  All filters are matched into a single row.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.}
 \begin{center}
 %\resizebox{\textwidth}{!}{%
@@ -3382 +3547 @@
 gstackImageID & - & BIGINT & NA  &Unique \ippstage{stack} identifier for g filter detection.\\
 gippDetectID & - & BIGINT & NA  &IPP internal detection identifier.\\
-gflxR5 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 3.00 arcsec.\\
-gflxR5Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 3.00 arcsec.\\
-gflxR5Std & Jy & REAL & -999  &Standard deviation of g filter flux within an aperture of radius r = 3.00 arcsec.\\
-gflxR5Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 3.00 arcsec.\\
-gflxR6 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 4.63 arcsec.\\
-gflxR6Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 4.63 arcsec.\\
-gflxR6Std & Jy & REAL & -999  &Standard deviation of g filter flux within an aperture of radius r = 4.63 arcsec.\\
-gflxR6Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 4.63 arcsec.\\
-gflxR7 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 7.43 arcsec.\\
-gflxR7Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 7.43 arcsec.\\
-gflxR7Std & Jy & REAL & -999  &Standard deviation of g filter flux within an aperture of radius r = 7.43 arcsec.\\
-gflxR7Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 7.43 arcsec.\\
+gflxR5 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 3.00\arcsec.\\
+gflxR5Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 3.00\arcsec.\\
+gflxR5Std & Jy & REAL & -999  &Standard deviation of g filter flux within an aperture of radius r = 3.00\arcsec.\\
+gflxR5Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 3.00\arcsec.\\
+gflxR6 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 4.63\arcsec.\\
+gflxR6Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 4.63\arcsec.\\
+gflxR6Std & Jy & REAL & -999  &Standard deviation of g filter flux within an aperture of radius r = 4.63\arcsec.\\
+gflxR6Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 4.63\arcsec.\\
+gflxR7 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 7.43\arcsec.\\
+gflxR7Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 7.43\arcsec.\\
+gflxR7Std & Jy & REAL & -999  &Standard deviation of g filter flux within an aperture of radius r = 7.43\arcsec.\\
+gflxR7Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 7.43\arcsec.\\
 gc6flxR5 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels\\
-& & & & (1.5 arcsec) within an aperture of radius r = 3.00 arcsec.\\
+& & & & (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\
 gc6flxR5Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of \\
-& & & & 6 sky pixels (1.5 arcsec) within an aperture of radius r = 3.00 arcsec.\\
+& & & & 6 sky pixels (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\
 gc6flxR5Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to \\
-& & & & a target of 6 sky pixels (1.5 arcsec) within an aperture of radius r = 3.00 arcsec.\\
+& & & & a target of 6 sky pixels (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\
 gc6flxR5Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a \\
-& & & & target of 6 sky pixels (1.5 arcsec) within an aperture of radius r = 3.00 arcsec.\\
+& & & & target of 6 sky pixels (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\
 gc6flxR6 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels\\
-& & & & (1.5 arcsec) within an aperture of radius r = 4.63 arcsec.\\
+& & & & (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\
 gc6flxR6Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of \\
-& & & & 6 sky pixels (1.5 arcsec) within an aperture of radius r = 4.63 arcsec.\\
+& & & & 6 sky pixels (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\
 gc6flxR6Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to \\
-& & & & a target of 6 sky pixels (1.5 arcsec) within an aperture of radius r = 4.63 arcsec.\\
+& & & & a target of 6 sky pixels (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\
 gc6flxR6Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of \\
-& & & & 6 sky pixels (1.5 arcsec) within an aperture of radius r = 4.63 arcsec.\\
+& & & & 6 sky pixels (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\
 gc6flxR7 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels\\
-& & & & (1.5 arcsec) within an aperture of radius r = 7.43 arcsec.\\
+& & & & (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\
 gc6flxR7Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of \\
-& & & & 6 sky pixels (1.5 arcsec) within an aperture of radius r = 7.43 arcsec.\\
+& & & & 6 sky pixels (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\
 gc6flxR7Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of \\
-& & & & 6 sky pixels (1.5 arcsec) within an aperture of radius r = 7.43 arcsec.\\
+& & & & 6 sky pixels (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\
 gc6flxR7Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 6 sky \\
-& & & & pixels (1.5 arcsec) within an aperture of radius r = 7.43 arcsec.\\
+& & & & pixels (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\
 gc8flxR5 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 8 sky pixels\\
-& & & & (2.0 arcsec) within an aperture of radius r = 3.00 arcsec.\\
+& & & & (2.0\arcsec) within an aperture of radius r = 3.00\arcsec.\\
 gc8flxR5Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 8 sky pixels \\
-& & & & (2.0 arcsec) within an aperture of radius r = 3.00 arcsec.\\
+& & & & (2.0\arcsec) within an aperture of radius r = 3.00\arcsec.\\
 gc8flxR5Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 8 sky \\
-& & & & pixels (2.0 arcsec) within an aperture of radius r = 3.00 arcsec.\\
+& & & & pixels (2.0\arcsec) within an aperture of radius r = 3.00\arcsec.\\
 gc8flxR5Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 8 sky \\
-& & & & pixels (2.0 arcsec) within an aperture of radius r = 3.00 arcsec.\\
+& & & & pixels (2.0\arcsec) within an aperture of radius r = 3.00\arcsec.\\
 gc8flxR6 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 8 sky pixels\\
-& & & & (2.0 arcsec) within an aperture of radius r = 4.63 arcsec.\\
+& & & & (2.0\arcsec) within an aperture of radius r = 4.63\arcsec.\\
 gc8flxR6Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 8 sky pixels\\
-& & & & (2.0 arcsec) within an aperture of radius r = 4.63 arcsec.\\
+& & & & (2.0\arcsec) within an aperture of radius r = 4.63\arcsec.\\
 gc8flxR6Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of \\
-& & & & 8 sky pixels (2.0 arcsec) within an aperture of radius r = 4.63 arcsec.\\
+& & & & 8 sky pixels (2.0\arcsec) within an aperture of radius r = 4.63\arcsec.\\
 gc8flxR6Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 8 sky pixels \\
-& & & & (2.0 arcsec) within an aperture of radius r = 4.63 arcsec.\\
-gc8flxR7 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 8 sky pixels (2.0 arcsec) \\
-& & & & within an aperture of radius r = 7.43 arcsec.\\
+& & & & (2.0\arcsec) within an aperture of radius r = 4.63\arcsec.\\
+gc8flxR7 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 8 sky pixels (2.0\arcsec) \\
+& & & & within an aperture of radius r = 7.43\arcsec.\\
 gc8flxR7Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target 8 sky pixels \\
-& & & & (2.0 arcsec) within an aperture of radius r = 7.43 arcsec.\\
+& & & & (2.0\arcsec) within an aperture of radius r = 7.43\arcsec.\\
 gc8flxR7Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of \\
-& & & & 8 sky pixels (2.0 arcsec) within an aperture of radius r = 7.43 arcsec.\\
+& & & & 8 sky pixels (2.0\arcsec) within an aperture of radius r = 7.43\arcsec.\\
 gc8flxR7Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 8 sky pixels \\
-& & & & (2.0 arcsec) within an aperture of radius r = 7.43 arcsec.\\
+& & & & (2.0\arcsec) within an aperture of radius r = 7.43\arcsec.\\
 rstackDetectID \\
 ... & & & & same entries repeated for r, i, z, and y filters \\
@@ -3453 +3618 @@
 
 %HAF commented out because stackmodelfitextra is junk: not in DR1 or DR2?
-%\begin{table}[b]
+%\begin{table}[htb]
 %\caption{StackModelFitExtra: Contains the galaxy shape and concentration parameters measured from the \ippstage{stack} detections.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections \citep[see]{Blakeslee2006,Cheng2011,Schade1995,Simard2011,Simard2002}}
 %\begin{center}
@@ -3489 +3654 @@
 %\end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{StackModelFitExp: Contains the exponential fit parameters to extended sources.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections. }
 \begin{center}
@@ -3600 +3765 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{StackModelFitDeV: Contains the \citet{deVaucouleurs1948} fit parameters to extended sources.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.}
 \begin{center}
@@ -3709 +3874 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{StackModelFitSer: Contains the \citet{Sersic1963} fit parameters to extended sources.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections \citep{Sersic1963}.}
 \begin{center}
@@ -3823 +3988 @@
 \end{table}%
 
-\begin{table}[b]
-\caption{StackApFlxExGalUnc: Contains the unconvolved fluxes within the SDSS R3 (r = 1.03 arcsec), R4 (r = 1.76 arcsec), R5 (r = 3.00 arcsec), R6 (r = 4.63 arcsec), R7 (r = 7.43 arcsec), R8 (r = 11.42 arcsec), R9 (r = 18.20 arcsec), R10 (r = 28.20 arcsec), and R11 (r = 44.21 arcsec) apertures \citep{Stoughton2002} for extended sources.  These measurements are only provided for objects in the extragalactic sky, i.e., they are not provided for objects in the Galactic plane because they are not useful in crowded areas.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.  }
+\begin{table}[htb]
+\caption{StackApFlxExGalUnc: Contains the unconvolved fluxes within the SDSS R3 (r = 1.03\arcsec), R4 (r = 1.76\arcsec), R5 (r = 3.00\arcsec), R6 (r = 4.63\arcsec), R7 (r = 7.43\arcsec), R8 (r = 11.42\arcsec), R9 (r = 18.20\arcsec), R10 (r = 28.20\arcsec), and R11 (r = 44.21\arcsec) apertures \citep{Stoughton2002} for extended sources.  These measurements are only provided for objects in the extragalactic sky, i.e., they are not provided for objects in the Galactic plane because they are not useful in crowded areas.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.  }
 \begin{center}
 %\resizebox{\textwidth}{!}{%
@@ -3841 +4006 @@
 gstackDetectID & - & BIGINT & NA  &Unique \ippstage{stack} detection identifier.\\
 gstackImageID & - & BIGINT & NA  &Unique \ippstage{stack} identifier for g filter detection.\\
-gflxR3 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 1.03 arcsec.\\
-gflxR3Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 1.03 arcsec.\\
+gflxR3 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 1.03\arcsec.\\
+gflxR3Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 1.03\arcsec.\\
 gflxR3Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection within an aperture of radius \\
-& & & & r = 1.03 arcsec.\\
-gflxR3Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 1.03 arcsec.\\
-gflxR4 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 1.76 arcsec.\\
-gflxR4Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 1.76 arcsec.\\
+& & & & r = 1.03\arcsec.\\
+gflxR3Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 1.03\arcsec.\\
+gflxR4 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 1.76\arcsec.\\
+gflxR4Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 1.76\arcsec.\\
 gflxR4Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection within an aperture of radius \\
-& & & & r = 1.76 arcsec.\\
-gflxR4Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 1.76 arcsec.\\
-gflxR5 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 3.00 arcsec.\\
-gflxR5Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 3.00 arcsec.\\
+& & & & r = 1.76\arcsec.\\
+gflxR4Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 1.76\arcsec.\\
+gflxR5 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 3.00\arcsec.\\
+gflxR5Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 3.00\arcsec.\\
 gflxR5Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection within an aperture of radius \\
-& & & & r = 3.00 arcsec.\\
-gflxR5Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 3.00 arcsec.\\
-gflxR6 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 4.63 arcsec.\\
-gflxR6Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 4.63 arcsec.\\
+& & & & r = 3.00\arcsec.\\
+gflxR5Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 3.00\arcsec.\\
+gflxR6 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 4.63\arcsec.\\
+gflxR6Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 4.63\arcsec.\\
 gflxR6Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection within an aperture of radius \\
-& & & & r = 4.63 arcsec.\\
-gflxR6Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 4.63 arcsec.\\
-gflxR7 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 7.43 arcsec.\\
-gflxR7Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 7.43 arcsec.\\
+& & & & r = 4.63\arcsec.\\
+gflxR6Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 4.63\arcsec.\\
+gflxR7 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 7.43\arcsec.\\
+gflxR7Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 7.43\arcsec.\\
 gflxR7Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection within an aperture of radius \\
-& & & & r = 7.43 arcsec.\\
-gflxR7Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 7.43 arcsec.\\
-gflxR8 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 11.42 arcsec.\\
-gflxR8Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 11.42 arcsec.\\
+& & & & r = 7.43\arcsec.\\
+gflxR7Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 7.43\arcsec.\\
+gflxR8 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 11.42\arcsec.\\
+gflxR8Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 11.42\arcsec.\\
 gflxR8Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection within an aperture of radius \\
-& & & & r = 11.42 arcsec.\\
-gflxR8Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 11.42 arcsec.\\
-gflxR9 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 18.20 arcsec.\\
-gflxR9Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 18.20 arcsec.\\
+& & & & r = 11.42\arcsec.\\
+gflxR8Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 11.42\arcsec.\\
+gflxR9 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 18.20\arcsec.\\
+gflxR9Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 18.20\arcsec.\\
 gflxR9Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection within an aperture of radius \\
-& & & & r = 18.20 arcsec.\\
-gflxR9Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 18.20 arcsec.\\
-gflxR10 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 28.20 arcsec.\\
-gflxR10Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 28.20 arcsec.\\
+& & & & r = 18.20\arcsec.\\
+gflxR9Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 18.20\arcsec.\\
+gflxR10 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 28.20\arcsec.\\
+gflxR10Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 28.20\arcsec.\\
 gflxR10Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection within an aperture of radius \\
-& & & & r = 28.20 arcsec.\\
-gflxR10Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 28.20 arcsec.\\
-gflxR11 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 44.21 arcsec.\\
-gflxR11Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 44.21 arcsec.\\
+& & & & r = 28.20\arcsec.\\
+gflxR10Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 28.20\arcsec.\\
+gflxR11 & Jy & REAL & -999  &Flux from g filter detection within an aperture of radius r = 44.21\arcsec.\\
+gflxR11Err & Jy & REAL & -999  &Error in flux from g filter detection within an aperture of radius r = 44.21\arcsec.\\
 gflxR11Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection within an aperture of radius \\
-& & & & r = 44.21 arcsec.\\
-gflxR11Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 44.21 arcsec.\\
+& & & & r = 44.21\arcsec.\\
+gflxR11Fill & - & REAL & -999  &Aperture fill factor for g filter detection within an aperture of radius r = 44.21\arcsec.\\
 rippDetectID\\
 ... & & & & same entries repeated for r, i, z, and y filters \\
@@ -3895 +4060 @@
 \end{table}%
 
-\begin{table}[b]
-\caption{StackApFlxExGalCon6: Contains the fluxes within the SDSS R3 (r = 1.03 arcsec), R4 (r = 1.76 arcsec), R5 (r = 3.00 arcsec), R6 (r = 4.63 arcsec), R7 (r = 7.43 arcsec), R8 (r = 11.42 arcsec), R9 (r = 18.20 arcsec), R10 (r = 28.20 arcsec), and R11 (r = 44.21 arcsec) apertures (\citep{Stoughton2002} for extended sources after the images have been convolved to a target of 6 sky pixels (1.5 arcsec).  These measurements are only provided for objects in the extragalactic sky, i.e., they are not provided for objects in the Galactic plane because they are not useful in crowded areas.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.}
+\begin{table}[htb]
+\caption{StackApFlxExGalCon6: Contains the fluxes within the SDSS R3 (r = 1.03\arcsec), R4 (r = 1.76\arcsec), R5 (r = 3.00\arcsec), R6 (r = 4.63\arcsec), R7 (r = 7.43\arcsec), R8 (r = 11.42\arcsec), R9 (r = 18.20\arcsec), R10 (r = 28.20\arcsec), and R11 (r = 44.21\arcsec) apertures (\citep{Stoughton2002} for extended sources after the images have been convolved to a target of 6 sky pixels (1.5\arcsec).  These measurements are only provided for objects in the extragalactic sky, i.e., they are not provided for objects in the Galactic plane because they are not useful in crowded areas.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.}
 \begin{center}
 %\resizebox{\textwidth}{!}{%
@@ -3913 +4078 @@
 gstackDetectID & - & BIGINT & NA  &Unique \ippstage{stack} detection identifier.\\
 gstackImageID & - & BIGINT & NA  &Unique \ippstage{stack} identifier for g filter detection.\\
-gc6flxR3 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 arcsec) \\
-& & & & within an aperture of radius r = 1.03 arcsec.\\
+gc6flxR3 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\
+& & & & within an aperture of radius r = 1.03\arcsec.\\
 gc6flxR3Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 6 sky pixels \\
-& & & & (1.5 arcsec) within an aperture of radius r = 1.03 arcsec.\\
+& & & & (1.5\arcsec) within an aperture of radius r = 1.03\arcsec.\\
 gc6flxR3Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 6 \\
-& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 1.03 arcsec.\\
+& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 1.03\arcsec.\\
 gc6flxR3Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\
-& & & & (1.5 arcsec) within an aperture of radius r = 1.03 arcsec.\\
-%gc6flxR4 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 arcsec) \\
-%& & & & within an aperture of radius r = 1.76 arcsec.\\
+& & & & (1.5\arcsec) within an aperture of radius r = 1.03\arcsec.\\
+%gc6flxR4 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\
+%& & & & within an aperture of radius r = 1.76\arcsec.\\
 %gc6flxR4Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 1.76 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 1.76\arcsec.\\
 %gc6flxR4Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 6 \\
-%& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 1.76 arcsec.\\
+%& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 1.76\arcsec.\\
 %gc6flxR4Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 1.76 arcsec.\\
-%gc6flxR5 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 arcsec) \\
-%& & & & within an aperture of radius r = 3.00 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 1.76\arcsec.\\
+%gc6flxR5 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\
+%& & & & within an aperture of radius r = 3.00\arcsec.\\
 %gc6flxR5Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 3.00 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\
 %gc6flxR5Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 6 \\
-%& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 3.00 arcsec.\\
+%& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\
 %gc6flxR5Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 3.00 arcsec.\\
-%gc6flxR6 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 arcsec) \\
-%& & & & within an aperture of radius r = 4.63 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\
+%gc6flxR6 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\
+%& & & & within an aperture of radius r = 4.63\arcsec.\\
 %gc6flxR6Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 4.63 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\
 %gc6flxR6Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 6 \\
-%& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 4.63 arcsec.\\
+%& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\
 %gc6flxR6Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 4.63 arcsec.\\
-%gc6flxR7 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 arcsec) \\
-%& & & & within an aperture of radius r = 7.43 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\
+%gc6flxR7 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\
+%& & & & within an aperture of radius r = 7.43\arcsec.\\
 %gc6flxR7Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 7.43 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\
 %gc6flxR7Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 6 \\
-%& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 7.43 arcsec.\\
+%& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\
 %gc6flxR7Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 7.43 arcsec.\\
-%gc6flxR8 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 arcsec) \\
-%& & & & within an aperture of radius r = 11.42 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\
+%gc6flxR8 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\
+%& & & & within an aperture of radius r = 11.42\arcsec.\\
 %gc6flxR8Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 11.42 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 11.42\arcsec.\\
 %gc6flxR8Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 6 \\
-%& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 11.42 arcsec.\\
+%& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 11.42\arcsec.\\
 %gc6flxR8Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 11.42 arcsec.\\
-%gc6flxR9 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 arcsec) \\
-%& & & & within an aperture of radius r = 18.20 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 11.42\arcsec.\\
+%gc6flxR9 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\
+%& & & & within an aperture of radius r = 18.20\arcsec.\\
 %gc6flxR9Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 18.20 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 18.20\arcsec.\\
 %gc6flxR9Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 6 \\
-%& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 18.20 arcsec.\\
+%& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 18.20\arcsec.\\
 %gc6flxR9Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 18.20 arcsec.\\
-%gc6flxR10 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 arcsec) \\
-%& & & & within an aperture of radius r = 28.20 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 18.20\arcsec.\\
+%gc6flxR10 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\
+%& & & & within an aperture of radius r = 28.20\arcsec.\\
 %gc6flxR10Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 28.20 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 28.20\arcsec.\\
 %gc6flxR10Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 6 \\
-%& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 28.20 arcsec.\\
+%& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 28.20\arcsec.\\
 %gc6flxR10Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\
-%& & & & (1.5 arcsec) within an aperture of radius r = 28.20 arcsec.\\
-... &  & & & gc6flxR3 ... gc6flxR3Fill columns repeated for R4 (r = 1.76 arcsec).\\
-... &  & & & repeated for R5 (r = 3.00 arcsec).\\
-... &  & & & repeated for R6 (r = 4.63 arcsec).\\
-... &  & & & repeated for R7 (r = 7.43 arcsec).\\
-... &  & & & repeated for R8 (r = 11.42 arcsec).\\
-... &  & & & repeated for R9 (r = 18.20 arcsec).\\
-... &  & & & repeated for R10 (r = 28.20 arcsec).\\
-gc6flxR11 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 arcsec) \\
-& & & & within an aperture of radius r = 44.21 arcsec.\\
+%& & & & (1.5\arcsec) within an aperture of radius r = 28.20\arcsec.\\
+... &  & & & gc6flxR3 ... gc6flxR3Fill columns repeated for R4 (r = 1.76\arcsec).\\
+... &  & & & repeated for R5 (r = 3.00\arcsec).\\
+... &  & & & repeated for R6 (r = 4.63\arcsec).\\
+... &  & & & repeated for R7 (r = 7.43\arcsec).\\
+... &  & & & repeated for R8 (r = 11.42\arcsec).\\
+... &  & & & repeated for R9 (r = 18.20\arcsec).\\
+... &  & & & repeated for R10 (r = 28.20\arcsec).\\
+gc6flxR11 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\
+& & & & within an aperture of radius r = 44.21\arcsec.\\
 gc6flxR11Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 6 sky pixels \\
-& & & & (1.5 arcsec) within an aperture of radius r = 44.21 arcsec.\\
+& & & & (1.5\arcsec) within an aperture of radius r = 44.21\arcsec.\\
 gc6flxR11Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 6 \\
-& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 44.21 arcsec.\\
+& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 44.21\arcsec.\\
 gc6flxR11Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\
-& & & & (1.5 arcsec) within an aperture of radius r = 44.21 arcsec.\\
+& & & & (1.5\arcsec) within an aperture of radius r = 44.21\arcsec.\\
 rippDetectID\\
 ... & & & & same entries repeated for r, i, z, and y filters \\
@@ -4001 +4166 @@
 \end{table}%
 
-\begin{table}[b]
-\caption{StackApFlxExGalCon8: Contains the fluxes within the SDSS R3 (r = 1.03 arcsec), R4 (r = 1.76 arcsec), R5 (r = 3.00 arcsec), R6 (r = 4.63 arcsec), R7 (r = 7.43 arcsec), R8 (r = 11.42 arcsec), R9 (r = 18.20 arcsec), R10 (r = 28.20 arcsec), and R11 (r = 44.21 arcsec) apertures \citep{Stoughton2002} for extended sources after the images have been convolved to a target of 8 sky pixels (2.0 arcsec).  These measurements are only provided for objects in the extragalactic sky, i.e., they are not provided for objects in the Galactic plane because they are not useful in crowded areas.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.}
+\begin{table}[htb]
+\caption{StackApFlxExGalCon8: Contains the fluxes within the SDSS R3 (r = 1.03\arcsec), R4 (r = 1.76\arcsec), R5 (r = 3.00\arcsec), R6 (r = 4.63\arcsec), R7 (r = 7.43\arcsec), R8 (r = 11.42\arcsec), R9 (r = 18.20\arcsec), R10 (r = 28.20\arcsec), and R11 (r = 44.21\arcsec) apertures \citep{Stoughton2002} for extended sources after the images have been convolved to a target of 8 sky pixels (2.0\arcsec).  These measurements are only provided for objects in the extragalactic sky, i.e., they are not provided for objects in the Galactic plane because they are not useful in crowded areas.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.}
 \begin{center}
 %\resizebox{\textwidth}{!}{%
@@ -4019 +4184 @@
 gstackDetectID & - & BIGINT & NA  &Unique \ippstage{stack} detection identifier.\\
 gstackImageID & - & BIGINT & NA  &Unique \ippstage{stack} identifier for g filter detection.\\
-gc8flxR3 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 8 sky pixels (2.0 arcsec) \\
-& & & & within an aperture of radius r = 1.03 arcsec.\\
+gc8flxR3 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 8 sky pixels (2.0\arcsec) \\
+& & & & within an aperture of radius r = 1.03\arcsec.\\
 gc8flxR3Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 8 sky pixels \\
-& & & & (2.0 arcsec) within an aperture of radius r = 1.03 arcsec.\\
+& & & & (2.0\arcsec) within an aperture of radius r = 1.03\arcsec.\\
 gc8flxR3Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 8 \\
-& & & & sky pixels (2.0 arcsec) within an aperture of radius r = 1.03 arcsec.\\
+& & & & sky pixels (2.0\arcsec) within an aperture of radius r = 1.03\arcsec.\\
 gc8flxR3Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 8 sky pixels \\
-& & & & (2.0 arcsec) within an aperture of radius r = 1.03 arcsec.\\
-... &  & & & gc8flxR3 ... gc8flxR3Fill columns repeated for R4 (r = 1.76 arcsec).\\
-... &  & & & repeated for R5 (r = 3.00 arcsec).\\
-... &  & & & repeated for R6 (r = 4.63 arcsec).\\
-... &  & & & repeated for R7 (r = 7.43 arcsec).\\
-... &  & & & repeated for R8 (r = 11.42 arcsec).\\
-... &  & & & repeated for R9 (r = 18.20 arcsec).\\
-... &  & & & repeated for R10 (r = 28.20 arcsec).\\
-gc8flxR11 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 8 sky pixels (2.0 arcsec) \\
-& & & & within an aperture of radius r = 44.21 arcsec.\\
+& & & & (2.0\arcsec) within an aperture of radius r = 1.03\arcsec.\\
+... &  & & & gc8flxR3 ... gc8flxR3Fill columns repeated for R4 (r = 1.76\arcsec).\\
+... &  & & & repeated for R5 (r = 3.00\arcsec).\\
+... &  & & & repeated for R6 (r = 4.63\arcsec).\\
+... &  & & & repeated for R7 (r = 7.43\arcsec).\\
+... &  & & & repeated for R8 (r = 11.42\arcsec).\\
+... &  & & & repeated for R9 (r = 18.20\arcsec).\\
+... &  & & & repeated for R10 (r = 28.20\arcsec).\\
+gc8flxR11 & Jy & REAL & -999  &Flux from g filter detection convolved to a target of 8 sky pixels (2.0\arcsec) \\
+& & & & within an aperture of radius r = 44.21\arcsec.\\
 gc8flxR11Err & Jy & REAL & -999  &Error in flux from g filter detection convolved to a target of 8 sky pixels \\
-& & & & (2.0 arcsec) within an aperture of radius r = 44.21 arcsec.\\
+& & & & (2.0\arcsec) within an aperture of radius r = 44.21\arcsec.\\
 gc8flxR11Std & Jy & REAL & -999  &Standard deviation of flux from g filter detection convolved to a target of 8 \\
-& & & & sky pixels (2.0 arcsec) within an aperture of radius r = 44.21 arcsec.\\
+& & & & sky pixels (2.0\arcsec) within an aperture of radius r = 44.21\arcsec.\\
 gc8flxR11Fill & - & REAL & -999  &Aperture fill factor for g filter detection convolved to a target of 8 sky pixels \\
-& & & & (2.0 arcsec) within an aperture of radius r = 44.21 arcsec.\\
+& & & & (2.0\arcsec) within an aperture of radius r = 44.21\arcsec.\\
 rippDetectID \\
 ... & & & & same entries repeated for r, i, z, and y filters \\
@@ -4051 +4216 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{StackPetrosian: Contains the \citet{Petrosian1976} magnitudes and radii for extended sources.  See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.}
 \begin{center}
@@ -4135 +4300 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{StackToImage: Contains the mapping of which input images were used to construct a particular stack.}
 \begin{center}
@@ -4145 +4310 @@
 \hline
 stackImageID & - & BIGINT & NA  &Unique \ippstage{stack} identifier.\\
-imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 * frameID + ccdID).\\
+imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 $\times$ frameID + ccdID).\\
 \hline
 \end{tabular}
@@ -4154 +4319 @@
 %\end{document} happy
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{StackToFrame: Contains the mapping of input frames used to construct a particular \ippstage{stack} along with processing statistics.}
 \begin{center}
@@ -4182 +4347 @@
 
 %this table is broken FIXXXXX AFFTER LUNCH
-\begin{table}[b]
+\begin{table}[htb]
 \caption{StackDetEffMeta: Contains the detection efficiency information for a given stacked image.  Provides the number of recovered sources out of 500 injected sources for each magnitude bin and statistics about the magnitudes of the recovered sources for a range of magnitude offsets.}
 \begin{center}
@@ -4224 +4389 @@
 \subsection{Forced Warp Tables}
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ForcedMeanObject: Contains the mean of single-epoch photometric information for sources detected in the stacked data, calculated as described in \citet{Magnier2013}.  The mean is calculated for detections associated into objects within a one arcsecond correlation radius.  PSF, \citet{Kron1980}, and SDSS aperture R5 (r = 3.00\arcsec), R6 (r = 4.63\arcsec), and R7 (r = 7.43\arcsec) apertures \citep{Stoughton2002} magnitudes and statistics are listed for all filters. See also \citet{Kaiser1995}.}
 \begin{center}
@@ -4244 +4409 @@
 gnIncKronFlux & - & SMALLINT & -999  &Number of forced single epoch detections in Kron (1980) flux mean in g filter.\\
 gnIncApFlux & - & SMALLINT & -999  &Number of forced single epoch detections in aperture flux mean in g filter.\\
-gnIncR5 & - & SMALLINT & -999  &Number of forced single epoch detections in R5 (r = 3.00 arcsec) aperture flux mean in g filter.\\
-gnIncR6 & - & SMALLINT & -999  &Number of forced single epoch detections in R6 (r = 4.63 arcsec) aperture flux mean in g filter.\\
-gnIncR7 & - & SMALLINT & -999  &Number of forced single epoch detections in R7 (r = 7.43 arcsec) aperture flux mean in g filter.\\
+gnIncR5 & - & SMALLINT & -999  &Number of forced single epoch detections in R5 (r = 3.00\arcsec) aperture flux mean in g filter.\\
+gnIncR6 & - & SMALLINT & -999  &Number of forced single epoch detections in R6 (r = 4.63\arcsec) aperture flux mean in g filter.\\
+gnIncR7 & - & SMALLINT & -999  &Number of forced single epoch detections in R7 (r = 7.43\arcsec) aperture flux mean in g filter.\\
 gFPSFFlux & Jy & REAL & -999  &Mean PSF flux from forced single epoch g filter detections.\\
 gFPSFFluxErr & Jy & REAL & -999  &Error in mean PSF flux from forced single epoch g filter detections.\\
@@ -4263 +4428 @@
 gFApMagErr & AB & REAL & -999  &Error in magnitude from mean aperture flux from forced single epoch g filter detections.\\
 gFmeanflxR5 & Jy & REAL & -999  &Mean flux from forced single epoch g filter \\
-& & & & detections within an aperture of radius r = 3.00 arcsec.\\
+& & & & detections within an aperture of radius r = 3.00\arcsec.\\
 gFmeanflxR5Err & Jy & REAL & -999  &Error in mean flux from forced single epoch g filter \\
-& & & & detections within an aperture of radius r = 3.00 arcsec.\\
+& & & & detections within an aperture of radius r = 3.00\arcsec.\\
 gFmeanflxR5Std & Jy & REAL & -999  &Standard deviation of forced single epoch g filter \\
-& & & & detection fluxes within an aperture of radius r = 3.00 arcsec.\\
+& & & & detection fluxes within an aperture of radius r = 3.00\arcsec.\\
 gFmeanflxR5Fill & - & REAL & -999  &Aperture fill factor for forced single epoch g filter \\
-& & & & detections within an aperture of radius r = 3.00 arcsec.\\
+& & & & detections within an aperture of radius r = 3.00\arcsec.\\
 gFmeanMagR5 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch g filter \\
-& & & & detections within an aperture of radius r = 3.00 arcsec.\\
+& & & & detections within an aperture of radius r = 3.00\arcsec.\\
 gFmeanMagR5Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch \\
-& & & & g filter detections within an aperture of radius r = 3.00 arcsec.\\
+& & & & g filter detections within an aperture of radius r = 3.00\arcsec.\\
 gFmeanflxR6 & Jy & REAL & -999  &Mean flux from forced single epoch g filter \\
-& & & & detections within an aperture of radius r = 4.63 arcsec.\\
+& & & & detections within an aperture of radius r = 4.63\arcsec.\\
 gFmeanflxR6Err & Jy & REAL & -999  &Error in mean flux from forced single epoch g filter \\
-& & & & detections within an aperture of radius r = 4.63 arcsec.\\
+& & & & detections within an aperture of radius r = 4.63\arcsec.\\
 gFmeanflxR6Std & Jy & REAL & -999  &Standard deviation of forced single epoch g filter \\
-& & & & detection fluxes within an aperture of radius r = 4.63 arcsec.\\
+& & & & detection fluxes within an aperture of radius r = 4.63\arcsec.\\
 gFmeanflxR6Fill & - & REAL & -999  &Aperture fill factor for forced single epoch g filter \\
-& & & & detections within an aperture of radius r = 4.63 arcsec.\\
+& & & & detections within an aperture of radius r = 4.63\arcsec.\\
 gFmeanMagR6 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch g filter \\
-& & & & detections within an aperture of radius r = 4.63 arcsec.\\
+& & & & detections within an aperture of radius r = 4.63\arcsec.\\
 gFmeanMagR6Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch \\
-& & & & g filter detections within an aperture of radius r = 4.63 arcsec.\\
+& & & & g filter detections within an aperture of radius r = 4.63\arcsec.\\
 gFmeanflxR7 & Jy & REAL & -999  &Mean flux from forced single epoch g filter \\
-& & & & detections within an aperture of radius r = 7.43 arcsec.\\
+& & & & detections within an aperture of radius r = 7.43\arcsec.\\
 gFmeanflxR7Err & Jy & REAL & -999  &Error in mean flux from forced single epoch g filter\\
-& & & & detections within an aperture of radius r = 7.43 arcsec.\\
+& & & & detections within an aperture of radius r = 7.43\arcsec.\\
 gFmeanflxR7Std & Jy & REAL & -999  &Standard deviation of forced single epoch g filter \\
-& & & & detection fluxes within an aperture of radius r = 7.43 arcsec.\\
+& & & & detection fluxes within an aperture of radius r = 7.43\arcsec.\\
 gFmeanflxR7Fill & - & REAL & -999  &Aperture fill factor for forced single epoch g filter \\
-& & & & detections within an aperture of radius r = 7.43 arcsec.\\
+& & & & detections within an aperture of radius r = 7.43\arcsec.\\
 gFmeanMagR7 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch g filter\\
-& & & & detections within an aperture of radius r = 7.43 arcsec.\\
+& & & & detections within an aperture of radius r = 7.43\arcsec.\\
 gFmeanMagR7Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch\\
-& & & & g filter detections within an aperture of radius r = 7.43 arcsec.\\
+& & & & g filter detections within an aperture of radius r = 7.43\arcsec.\\
 gFlags & - & INT & 0  &Information flag bitmask indicating details of the photometry from forced \\
 & & & & single epoch g filter detections.  Values listed in ObjectInfoFlags.\\
@@ -4310 +4475 @@
 %rnIncKronFlux & - & SMALLINT & -999  &Number of forced single epoch detections in Kron (1980) flux mean in r filter.\\
 %rnIncApFlux & - & SMALLINT & -999  &Number of forced single epoch detections in aperture flux mean in r filter.\\
-%rnIncR5 & - & SMALLINT & -999  &Number of forced single epoch detections in R5 (r = 3.00 arcsec) aperture flux mean in r filter.\\
-%rnIncR6 & - & SMALLINT & -999  &Number of forced single epoch detections in R6 (r = 4.63 arcsec) aperture flux mean in r filter.\\
-%rnIncR7 & - & SMALLINT & -999  &Number of forced single epoch detections in R7 (r = 7.43 arcsec) aperture flux mean in r filter.\\
+%rnIncR5 & - & SMALLINT & -999  &Number of forced single epoch detections in R5 (r = 3.00\arcsec) aperture flux mean in r filter.\\
+%rnIncR6 & - & SMALLINT & -999  &Number of forced single epoch detections in R6 (r = 4.63\arcsec) aperture flux mean in r filter.\\
+%rnIncR7 & - & SMALLINT & -999  &Number of forced single epoch detections in R7 (r = 7.43\arcsec) aperture flux mean in r filter.\\
 %rFPSFFlux & Jy & REAL & -999  &Mean PSF flux from forced single epoch r filter detections.\\
 %rFPSFFluxErr & Jy & REAL & -999  &Error in mean PSF flux from forced single epoch r filter detections.\\
@@ -4328 +4493 @@
 %rFApMag & AB & REAL & -999  &Magnitude from mean aperture flux from forced single epoch r filter detections.\\
 %rFApMagErr & AB & REAL & -999  &Error in magnitude from mean aperture flux from forced single epoch r filter detections.\\
-%rFmeanflxR5 & Jy & REAL & -999  &Mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00 arcsec.\\
-%rFmeanflxR5Err & Jy & REAL & -999  &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00 arcsec.\\
-%rFmeanflxR5Std & Jy & REAL & -999  &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 3.00 arcsec.\\
-%rFmeanflxR5Fill & - & REAL & -999  &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 3.00 arcsec.\\
-%rFmeanMagR5 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00 arcsec.\\
-%rFmeanMagR5Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00 arcsec.\\
-%rFmeanflxR6 & Jy & REAL & -999  &Mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63 arcsec.\\
-%rFmeanflxR6Err & Jy & REAL & -999  &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63 arcsec.\\
-%rFmeanflxR6Std & Jy & REAL & -999  &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 4.63 arcsec.\\
-%rFmeanflxR6Fill & - & REAL & -999  &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 4.63 arcsec.\\
-%rFmeanMagR6 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63 arcsec.\\
-%rFmeanMagR6Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63 arcsec.\\
-%rFmeanflxR7 & Jy & REAL & -999  &Mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43 arcsec.\\
-%rFmeanflxR7Err & Jy & REAL & -999  &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43 arcsec.\\
-%rFmeanflxR7Std & Jy & REAL & -999  &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 7.43 arcsec.\\
-%rFmeanflxR7Fill & - & REAL & -999  &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 7.43 arcsec.\\
-%rFmeanMagR7 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43 arcsec.\\
-%rFmeanMagR7Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43 arcsec.\\
+%rFmeanflxR5 & Jy & REAL & -999  &Mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00\arcsec.\\
+%rFmeanflxR5Err & Jy & REAL & -999  &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00\arcsec.\\
+%rFmeanflxR5Std & Jy & REAL & -999  &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 3.00\arcsec.\\
+%rFmeanflxR5Fill & - & REAL & -999  &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 3.00\arcsec.\\
+%rFmeanMagR5 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00\arcsec.\\
+%rFmeanMagR5Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00\arcsec.\\
+%rFmeanflxR6 & Jy & REAL & -999  &Mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63\arcsec.\\
+%rFmeanflxR6Err & Jy & REAL & -999  &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63\arcsec.\\
+%rFmeanflxR6Std & Jy & REAL & -999  &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 4.63\arcsec.\\
+%rFmeanflxR6Fill & - & REAL & -999  &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 4.63\arcsec.\\
+%rFmeanMagR6 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63\arcsec.\\
+%rFmeanMagR6Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63\arcsec.\\
+%rFmeanflxR7 & Jy & REAL & -999  &Mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43\arcsec.\\
+%rFmeanflxR7Err & Jy & REAL & -999  &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43\arcsec.\\
+%rFmeanflxR7Std & Jy & REAL & -999  &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 7.43\arcsec.\\
+%rFmeanflxR7Fill & - & REAL & -999  &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 7.43\arcsec.\\
+%rFmeanMagR7 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43\arcsec.\\
+%rFmeanMagR7Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43\arcsec.\\
 %rFlags & - & INT & 0  &Information flag bitmask indicating details of the photometry from forced single epoch r filter detections.  Values listed in ObjectInfoFlags.\\
 %rE1 & - & REAL & -999  &\citet{Kaiser1995} polarization parameter e1 = (Mxx - Myy) / (Mxx + Myy) from forced single epoch r filter detections.\\
@@ -4353 +4518 @@
 %inIncKronFlux & - & SMALLINT & -999  &Number of forced single epoch detections in Kron (1980) flux mean in i filter.\\
 %inIncApFlux & - & SMALLINT & -999  &Number of forced single epoch detections in aperture flux mean in i filter.\\
-%inIncR5 & - & SMALLINT & -999  &Number of forced single epoch detections in R5 (r = 3.00 arcsec) aperture flux mean in i filter.\\
-%inIncR6 & - & SMALLINT & -999  &Number of forced single epoch detections in R6 (r = 4.63 arcsec) aperture flux mean in i filter.\\
-%inIncR7 & - & SMALLINT & -999  &Number of forced single epoch detections in R7 (r = 7.43 arcsec) aperture flux mean in i filter.\\
+%inIncR5 & - & SMALLINT & -999  &Number of forced single epoch detections in R5 (r = 3.00\arcsec) aperture flux mean in i filter.\\
+%inIncR6 & - & SMALLINT & -999  &Number of forced single epoch detections in R6 (r = 4.63\arcsec) aperture flux mean in i filter.\\
+%inIncR7 & - & SMALLINT & -999  &Number of forced single epoch detections in R7 (r = 7.43\arcsec) aperture flux mean in i filter.\\
 %iFPSFFlux & Jy & REAL & -999  &Mean PSF flux from forced single epoch i filter detections.\\
 %iFPSFFluxErr & Jy & REAL & -999  &Error in mean PSF flux from forced single epoch i filter detections.\\
@@ -4371 +4536 @@
 %iFApMag & AB & REAL & -999  &Magnitude from mean aperture flux from forced single epoch i filter detections.\\
 %iFApMagErr & AB & REAL & -999  &Error in magnitude from mean aperture flux from forced single epoch i filter detections.\\
-%iFmeanflxR5 & Jy & REAL & -999  &Mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00 arcsec.\\
-%iFmeanflxR5Err & Jy & REAL & -999  &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00 arcsec.\\
-%iFmeanflxR5Std & Jy & REAL & -999  &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 3.00 arcsec.\\
-%iFmeanflxR5Fill & - & REAL & -999  &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 3.00 arcsec.\\
-%iFmeanMagR5 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00 arcsec.\\
-%iFmeanMagR5Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00 arcsec.\\
-%iFmeanflxR6 & Jy & REAL & -999  &Mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63 arcsec.\\
-%iFmeanflxR6Err & Jy & REAL & -999  &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63 arcsec.\\
-%iFmeanflxR6Std & Jy & REAL & -999  &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 4.63 arcsec.\\
-%iFmeanflxR6Fill & - & REAL & -999  &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 4.63 arcsec.\\
-%iFmeanMagR6 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63 arcsec.\\
-%iFmeanMagR6Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63 arcsec.\\
-%iFmeanflxR7 & Jy & REAL & -999  &Mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43 arcsec.\\
-%iFmeanflxR7Err & Jy & REAL & -999  &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43 arcsec.\\
-%iFmeanflxR7Std & Jy & REAL & -999  &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 7.43 arcsec.\\
-%iFmeanflxR7Fill & - & REAL & -999  &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 7.43 arcsec.\\
-%iFmeanMagR7 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43 arcsec.\\
-%iFmeanMagR7Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43 arcsec.\\
+%iFmeanflxR5 & Jy & REAL & -999  &Mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00\arcsec.\\
+%iFmeanflxR5Err & Jy & REAL & -999  &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00\arcsec.\\
+%iFmeanflxR5Std & Jy & REAL & -999  &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 3.00\arcsec.\\
+%iFmeanflxR5Fill & - & REAL & -999  &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 3.00\arcsec.\\
+%iFmeanMagR5 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00\arcsec.\\
+%iFmeanMagR5Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00\arcsec.\\
+%iFmeanflxR6 & Jy & REAL & -999  &Mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63\arcsec.\\
+%iFmeanflxR6Err & Jy & REAL & -999  &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63\arcsec.\\
+%iFmeanflxR6Std & Jy & REAL & -999  &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 4.63\arcsec.\\
+%iFmeanflxR6Fill & - & REAL & -999  &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 4.63\arcsec.\\
+%iFmeanMagR6 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63\arcsec.\\
+%iFmeanMagR6Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63\arcsec.\\
+%iFmeanflxR7 & Jy & REAL & -999  &Mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43\arcsec.\\
+%iFmeanflxR7Err & Jy & REAL & -999  &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43\arcsec.\\
+%iFmeanflxR7Std & Jy & REAL & -999  &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 7.43\arcsec.\\
+%iFmeanflxR7Fill & - & REAL & -999  &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 7.43\arcsec.\\
+%iFmeanMagR7 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43\arcsec.\\
+%iFmeanMagR7Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43\arcsec.\\
 %iFlags & - & INT & 0  &Information flag bitmask indicating details of the photometry from forced single epoch i filter detections.  Values listed in ObjectInfoFlags.\\
 %iE1 & - & REAL & -999  &\citet{Kaiser1995} polarization parameter e1 = (Mxx - Myy) / (Mxx + Myy) from forced single epoch i filter detections.\\
@@ -4396 +4561 @@
 %znIncKronFlux & - & SMALLINT & -999  &Number of forced single epoch detections in Kron (1980) flux mean in z filter.\\
 %znIncApFlux & - & SMALLINT & -999  &Number of forced single epoch detections in aperture flux mean in z filter.\\
-%znIncR5 & - & SMALLINT & -999  &Number of forced single epoch detections in R5 (r = 3.00 arcsec) aperture flux mean in z filter.\\
-%znIncR6 & - & SMALLINT & -999  &Number of forced single epoch detections in R6 (r = 4.63 arcsec) aperture flux mean in z filter.\\
-%znIncR7 & - & SMALLINT & -999  &Number of forced single epoch detections in R7 (r = 7.43 arcsec) aperture flux mean in z filter.\\
+%znIncR5 & - & SMALLINT & -999  &Number of forced single epoch detections in R5 (r = 3.00\arcsec) aperture flux mean in z filter.\\
+%znIncR6 & - & SMALLINT & -999  &Number of forced single epoch detections in R6 (r = 4.63\arcsec) aperture flux mean in z filter.\\
+%znIncR7 & - & SMALLINT & -999  &Number of forced single epoch detections in R7 (r = 7.43\arcsec) aperture flux mean in z filter.\\
 %zFPSFFlux & Jy & REAL & -999  &Mean PSF flux from forced single epoch z filter detections.\\
 %zFPSFFluxErr & Jy & REAL & -999  &Error in mean PSF flux from forced single epoch z filter detections.\\
@@ -4414 +4579 @@
 %zFApMag & AB & REAL & -999  &Magnitude from mean aperture flux from forced single epoch z filter detections.\\
 %zFApMagErr & AB & REAL & -999  &Error in magnitude from mean aperture flux from forced single epoch z filter detections.\\
-%zFmeanflxR5 & Jy & REAL & -999  &Mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00 arcsec.\\
-%zFmeanflxR5Err & Jy & REAL & -999  &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00 arcsec.\\
-%zFmeanflxR5Std & Jy & REAL & -999  &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 3.00 arcsec.\\
-%zFmeanflxR5Fill & - & REAL & -999  &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 3.00 arcsec.\\
-%zFmeanMagR5 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00 arcsec.\\
-%zFmeanMagR5Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00 arcsec.\\
-%zFmeanflxR6 & Jy & REAL & -999  &Mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63 arcsec.\\
-%zFmeanflxR6Err & Jy & REAL & -999  &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63 arcsec.\\
-%zFmeanflxR6Std & Jy & REAL & -999  &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 4.63 arcsec.\\
-%zFmeanflxR6Fill & - & REAL & -999  &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 4.63 arcsec.\\
-%zFmeanMagR6 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63 arcsec.\\
-%zFmeanMagR6Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63 arcsec.\\
-%zFmeanflxR7 & Jy & REAL & -999  &Mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43 arcsec.\\
-%zFmeanflxR7Err & Jy & REAL & -999  &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43 arcsec.\\
-%zFmeanflxR7Std & Jy & REAL & -999  &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 7.43 arcsec.\\
-%zFmeanflxR7Fill & - & REAL & -999  &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 7.43 arcsec.\\
-%zFmeanMagR7 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43 arcsec.\\
-%zFmeanMagR7Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43 arcsec.\\
+%zFmeanflxR5 & Jy & REAL & -999  &Mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00\arcsec.\\
+%zFmeanflxR5Err & Jy & REAL & -999  &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00\arcsec.\\
+%zFmeanflxR5Std & Jy & REAL & -999  &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 3.00\arcsec.\\
+%zFmeanflxR5Fill & - & REAL & -999  &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 3.00\arcsec.\\
+%zFmeanMagR5 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00\arcsec.\\
+%zFmeanMagR5Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00\arcsec.\\
+%zFmeanflxR6 & Jy & REAL & -999  &Mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63\arcsec.\\
+%zFmeanflxR6Err & Jy & REAL & -999  &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63\arcsec.\\
+%zFmeanflxR6Std & Jy & REAL & -999  &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 4.63\arcsec.\\
+%zFmeanflxR6Fill & - & REAL & -999  &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 4.63\arcsec.\\
+%zFmeanMagR6 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63\arcsec.\\
+%zFmeanMagR6Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63\arcsec.\\
+%zFmeanflxR7 & Jy & REAL & -999  &Mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43\arcsec.\\
+%zFmeanflxR7Err & Jy & REAL & -999  &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43\arcsec.\\
+%zFmeanflxR7Std & Jy & REAL & -999  &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 7.43\arcsec.\\
+%zFmeanflxR7Fill & - & REAL & -999  &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 7.43\arcsec.\\
+%zFmeanMagR7 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43\arcsec.\\
+%zFmeanMagR7Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43\arcsec.\\
 %zFlags & - & INT & 0  &Information flag bitmask indicating details of the photometry from forced single epoch z filter detections.  Values listed in ObjectInfoFlags.\\
 %zE1 & - & REAL & -999  &\citet{Kaiser1995} polarization parameter e1 = (Mxx - Myy) / (Mxx + Myy) from forced single epoch z filter detections.\\
@@ -4439 +4604 @@
 %ynIncKronFlux & - & SMALLINT & -999  &Number of forced single epoch detections in Kron (1980) flux mean in y filter.\\
 %ynIncApFlux & - & SMALLINT & -999  &Number of forced single epoch detections in aperture flux mean in y filter.\\
-%ynIncR5 & - & SMALLINT & -999  &Number of forced single epoch detections in R5 (r = 3.00 arcsec) aperture flux mean in y filter.\\
-%ynIncR6 & - & SMALLINT & -999  &Number of forced single epoch detections in R6 (r = 4.63 arcsec) aperture flux mean in y filter.\\
-%ynIncR7 & - & SMALLINT & -999  &Number of forced single epoch detections in R7 (r = 7.43 arcsec) aperture flux mean in y filter.\\
+%ynIncR5 & - & SMALLINT & -999  &Number of forced single epoch detections in R5 (r = 3.00\arcsec) aperture flux mean in y filter.\\
+%ynIncR6 & - & SMALLINT & -999  &Number of forced single epoch detections in R6 (r = 4.63\arcsec) aperture flux mean in y filter.\\
+%ynIncR7 & - & SMALLINT & -999  &Number of forced single epoch detections in R7 (r = 7.43\arcsec) aperture flux mean in y filter.\\
 %yFPSFFlux & Jy & REAL & -999  &Mean PSF flux from forced single epoch y filter detections.\\
 %yFPSFFluxErr & Jy & REAL & -999  &Error in mean PSF flux from forced single epoch y filter detections.\\
@@ -4457 +4622 @@
 %yFApMag & AB & REAL & -999  &Magnitude from mean aperture flux from forced single epoch y filter detections.\\
 %yFApMagErr & AB & REAL & -999  &Error in magnitude from mean aperture flux from forced single epoch y filter detections.\\
-%yFmeanflxR5 & Jy & REAL & -999  &Mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00 arcsec.\\
-%yFmeanflxR5Err & Jy & REAL & -999  &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00 arcsec.\\
-%yFmeanflxR5Std & Jy & REAL & -999  &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 3.00 arcsec.\\
-%yFmeanflxR5Fill & - & REAL & -999  &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 3.00 arcsec.\\
-%yFmeanMagR5 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00 arcsec.\\
-%yFmeanMagR5Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00 arcsec.\\
-%yFmeanflxR6 & Jy & REAL & -999  &Mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63 arcsec.\\
-%yFmeanflxR6Err & Jy & REAL & -999  &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63 arcsec.\\
-%yFmeanflxR6Std & Jy & REAL & -999  &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 4.63 arcsec.\\
-%yFmeanflxR6Fill & - & REAL & -999  &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 4.63 arcsec.\\
-%yFmeanMagR6 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63 arcsec.\\
-%yFmeanMagR6Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63 arcsec.\\
-%yFmeanflxR7 & Jy & REAL & -999  &Mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43 arcsec.\\
-%yFmeanflxR7Err & Jy & REAL & -999  &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43 arcsec.\\
-%yFmeanflxR7Std & Jy & REAL & -999  &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 7.43 arcsec.\\
-%yFmeanflxR7Fill & - & REAL & -999  &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 7.43 arcsec.\\
-%yFmeanMagR7 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43 arcsec.\\
-%yFmeanMagR7Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43 arcsec.\\
+%yFmeanflxR5 & Jy & REAL & -999  &Mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00\arcsec.\\
+%yFmeanflxR5Err & Jy & REAL & -999  &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00\arcsec.\\
+%yFmeanflxR5Std & Jy & REAL & -999  &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 3.00\arcsec.\\
+%yFmeanflxR5Fill & - & REAL & -999  &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 3.00\arcsec.\\
+%yFmeanMagR5 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00\arcsec.\\
+%yFmeanMagR5Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00\arcsec.\\
+%yFmeanflxR6 & Jy & REAL & -999  &Mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63\arcsec.\\
+%yFmeanflxR6Err & Jy & REAL & -999  &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63\arcsec.\\
+%yFmeanflxR6Std & Jy & REAL & -999  &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 4.63\arcsec.\\
+%yFmeanflxR6Fill & - & REAL & -999  &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 4.63\arcsec.\\
+%yFmeanMagR6 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63\arcsec.\\
+%yFmeanMagR6Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63\arcsec.\\
+%yFmeanflxR7 & Jy & REAL & -999  &Mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43\arcsec.\\
+%yFmeanflxR7Err & Jy & REAL & -999  &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43\arcsec.\\
+%yFmeanflxR7Std & Jy & REAL & -999  &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 7.43\arcsec.\\
+%yFmeanflxR7Fill & - & REAL & -999  &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 7.43\arcsec.\\
+%yFmeanMagR7 & AB & REAL & -999  &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43\arcsec.\\
+%yFmeanMagR7Err & AB & REAL & -999  &Error in magnitude from  mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43\arcsec.\\
 %yFlags & - & INT & 0  &Information flag bitmask indicating details of the photometry from forced single epoch y filter detections.  Values listed in ObjectInfoFlags.\\
 %yE1 & - & REAL & -999  &\citet{Kaiser1995} polarization parameter e1 = (Mxx - Myy) / (Mxx + Myy) from forced single epoch y filter detections.\\
@@ -4487 +4652 @@
 
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ForcedMeanLensing: Contains the mean \citet[K95]{Kaiser1995} lensing parameters measured from the forced photometry of objects detected in stacked images on the individual single epoch data.}
 \begin{center}
@@ -4503 +4668 @@
 batchID & - & BIGINT & NA  &Internal database batch identifier.\\
 processingVersion & - & TINYINT & NA  &Data release version.\\
-gLensObjSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced g filter detections.\\
-gLensObjSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced g filter detections.\\
-gLensObjSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced g filter detections.\\
-gLensObjSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced g filter detections.\\
-gLensObjSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced g filter detections.\\
+gLensObjSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced g filter detections.\\
+gLensObjSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced g filter detections.\\
+gLensObjSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced g filter detections.\\
+gLensObjSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced g filter detections.\\
+gLensObjSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced g filter detections.\\
 gLensObjShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from forced g filter detections.\\
 gLensObjShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from forced g filter detections.\\
@@ -4513 +4678 @@
 gLensObjShearE1 & - & REAL & -999  &K95 eq. (B12) shear polarizability e1 term from forced g filter detections.\\
 gLensObjShearE2 & - & REAL & -999  &K95 eq. (B12) shear polarizability e2 term from forced g filter detections.\\
-gLensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced g filter detections.\\
-gLensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced g filter detections.\\
-gLensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced g filter detections.\\
-gLensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced g filter detections.\\
-gLensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced g filter detections.\\
+gLensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced g filter detections.\\
+gLensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced g filter detections.\\
+gLensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced g filter detections.\\
+gLensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced g filter detections.\\
+gLensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced g filter detections.\\
 gLensPSFShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from PSF model for forced g filter detections.\\
 gLensPSFShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from PSF model for forced g filter detections.\\
@@ -4525 +4690 @@
 rlensObjSmearX11 \\
 ... & & & & same entries repeated for r, i, z, and y filters \\
-%rlensObjSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced r filter detections.\\
-%rlensObjSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced r filter detections.\\
-%rlensObjSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced r filter detections.\\
-%rlensObjSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced r filter detections.\\
-%rlensObjSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced r filter detections.\\
+%rlensObjSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced r filter detections.\\
+%rlensObjSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced r filter detections.\\
+%rlensObjSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced r filter detections.\\
+%rlensObjSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced r filter detections.\\
+%rlensObjSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced r filter detections.\\
 %rlensObjShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from forced r filter detections.\\
 %rlensObjShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from forced r filter detections.\\
@@ -4535 +4700 @@
 %rlensObjShearE1 & - & REAL & -999  &K95 eq. (B12) shear polarizability e1 term from forced r filter detections.\\
 %rlensObjShearE2 & - & REAL & -999  &K95 eq. (B12) shear polarizability e2 term from forced r filter detections.\\
-%rlensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced r filter detections.\\
-%rlensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced r filter detections.\\
-%rlensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced r filter detections.\\
-%rlensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced r filter detections.\\
-%rlensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced r filter detections.\\
+%rlensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced r filter detections.\\
+%rlensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced r filter detections.\\
+%rlensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced r filter detections.\\
+%rlensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced r filter detections.\\
+%rlensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced r filter detections.\\
 %rlensPSFShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from PSF model for forced r filter detections.\\
 %rlensPSFShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from PSF model for forced r filter detections.\\
@@ -4545 +4710 @@
 %rlensPSFShearE1 & - & REAL & -999  &K95 eq. (B12) shear polarizability e1 term from PSF model for forced r filter detections.\\
 %rlensPSFShearE2 & - & REAL & -999  &K95 eq. (B12) shear polarizability e2 term from PSF model forced r filter detections.\\
-%ilensObjSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced i filter detections.\\
-%ilensObjSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced i filter detections.\\
-%ilensObjSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced i filter detections.\\
-%ilensObjSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced i filter detections.\\
-%ilensObjSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced i filter detections.\\
+%ilensObjSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced i filter detections.\\
+%ilensObjSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced i filter detections.\\
+%ilensObjSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced i filter detections.\\
+%ilensObjSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced i filter detections.\\
+%ilensObjSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced i filter detections.\\
 %ilensObjShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from forced i filter detections.\\
 %ilensObjShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from forced i filter detections.\\
@@ -4555 +4720 @@
 %ilensObjShearE1 & - & REAL & -999  &K95 eq. (B12) shear polarizability e1 term from forced i filter detections.\\
 %ilensObjShearE2 & - & REAL & -999  &K95 eq. (B12) shear polarizability e2 term from forced i filter detections.\\
-%ilensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced i filter detections.\\
-%ilensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced i filter detections.\\
-%ilensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced i filter detections.\\
-%ilensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced i filter detections.\\
-%ilensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced i filter detections.\\
+%ilensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced i filter detections.\\
+%ilensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced i filter detections.\\
+%ilensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced i filter detections.\\
+%ilensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced i filter detections.\\
+%ilensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced i filter detections.\\
 %ilensPSFShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from PSF model for forced i filter detections.\\
 %ilensPSFShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from PSF model for forced i filter detections.\\
@@ -4565 +4730 @@
 %ilensPSFShearE1 & - & REAL & -999  &K95 eq. (B12) shear polarizability e1 term from PSF model for forced i filter detections.\\
 %ilensPSFShearE2 & - & REAL & -999  &K95 eq. (B12) shear polarizability e2 term from PSF model forced i filter detections.\\
-%zlensObjSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced z filter detections.\\
-%zlensObjSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced z filter detections.\\
-%zlensObjSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced z filter detections.\\
-%zlensObjSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced z filter detections.\\
-%zlensObjSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced z filter detections.\\
+%zlensObjSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced z filter detections.\\
+%zlensObjSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced z filter detections.\\
+%zlensObjSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced z filter detections.\\
+%zlensObjSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced z filter detections.\\
+%zlensObjSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced z filter detections.\\
 %zlensObjShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from forced z filter detections.\\
 %zlensObjShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from forced z filter detections.\\
@@ -4575 +4740 @@
 %zlensObjShearE1 & - & REAL & -999  &K95 eq. (B12) shear polarizability e1 term from forced z filter detections.\\
 %zlensObjShearE2 & - & REAL & -999  &K95 eq. (B12) shear polarizability e2 term from forced z filter detections.\\
-%zlensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced z filter detections.\\
-%zlensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced z filter detections.\\
-%zlensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced z filter detections.\\
-%zlensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced z filter detections.\\
-%zlensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced z filter detections.\\
+%zlensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced z filter detections.\\
+%zlensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced z filter detections.\\
+%zlensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced z filter detections.\\
+%zlensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced z filter detections.\\
+%zlensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced z filter detections.\\
 %zlensPSFShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from PSF model for forced z filter detections.\\
 %zlensPSFShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from PSF model for forced z filter detections.\\
@@ -4585 +4750 @@
 %zlensPSFShearE1 & - & REAL & -999  &K95 eq. (B12) shear polarizability e1 term from PSF model for forced z filter detections.\\
 %zlensPSFShearE2 & - & REAL & -999  &K95 eq. (B12) shear polarizability e2 term from PSF model forced z filter detections.\\
-%ylensObjSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced y filter detections.\\
-%ylensObjSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced y filter detections.\\
-%ylensObjSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced y filter detections.\\
-%ylensObjSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced y filter detections.\\
-%ylensObjSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced y filter detections.\\
+%ylensObjSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced y filter detections.\\
+%ylensObjSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced y filter detections.\\
+%ylensObjSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced y filter detections.\\
+%ylensObjSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced y filter detections.\\
+%ylensObjSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced y filter detections.\\
 %ylensObjShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from forced y filter detections.\\
 %ylensObjShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from forced y filter detections.\\
@@ -4595 +4760 @@
 %ylensObjShearE1 & - & REAL & -999  &K95 eq. (B12) shear polarizability e1 term from forced y filter detections.\\
 %ylensObjShearE2 & - & REAL & -999  &K95 eq. (B12) shear polarizability e2 term from forced y filter detections.\\
-%ylensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced y filter detections.\\
-%ylensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced y filter detections.\\
-%ylensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced y filter detections.\\
-%ylensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced y filter detections.\\
-%ylensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced y filter detections.\\
+%ylensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced y filter detections.\\
+%ylensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced y filter detections.\\
+%ylensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced y filter detections.\\
+%ylensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced y filter detections.\\
+%ylensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced y filter detections.\\
 %ylensPSFShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from PSF model for forced y filter detections.\\
 %ylensPSFShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from PSF model for forced y filter detections.\\
@@ -4614 +4779 @@
 % \subsection{Forced \ippstage{warp} Exposure Tables}
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ForcedWarpMeta: Contains the metadata related to a sky-aligned distortion corrected \ippstage{warp} image, upon which forced photometry is performed.  The astrometric and photometric calibration of the \ippstage{warp} image are listed.}
 \begin{center}
@@ -4650 +4815 @@
 psfTheta & degrees & REAL & -999  &PSF major axis orientation at image center.\\
 photoZero & magnitudes & REAL & -999  &Locally derived photometric zero point for this \ippstage{warp} image.\\
-ctype1 & - & VARCHAR(100) &   &Name of astrometric projection in RA.\\
+ctype1 & - & VARCHAR(100) &   &Name of astrometric projection in R.A..\\
 ctype2 & - & VARCHAR(100) &   &Name of astrometric projection in Dec.\\
 crval1 & degrees & FLOAT & -999  &Right ascension corresponding to reference pixel.\\
 crval2 & degrees & FLOAT & -999  &Declination corresponding to reference pixel.\\
-crpix1 & sky pixels & FLOAT & -999  &Reference pixel for RA.\\
+crpix1 & sky pixels & FLOAT & -999  &Reference pixel for R.A..\\
 crpix2 & sky pixels & FLOAT & -999  &Reference pixel for Dec.\\
-cdelt1 & degrees/pixel & FLOAT & -999  &Pixel scale in RA.\\
+cdelt1 & degrees/pixel & FLOAT & -999  &Pixel scale in R.A..\\
 cdelt2 & degrees/pixel & FLOAT & -999  &Pixel scale in Dec.\\
-pc001001 & - & FLOAT & -999  &Linear transformation matrix element between image pixel x and RA.\\
-pc001002 & - & FLOAT & -999  &Linear transformation matrix element between image pixel y and RA.\\
+pc001001 & - & FLOAT & -999  &Linear transformation matrix element between image pixel x and R.A..\\
+pc001002 & - & FLOAT & -999  &Linear transformation matrix element between image pixel y and R.A..\\
 pc002001 & - & FLOAT & -999  &Linear transformation matrix element between image pixel x and Dec.\\
 pc002002 & - & FLOAT & -999  &Linear transformation matrix element between image pixel y and Dec.\\
@@ -4672 +4837 @@
 
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ForcedWarpMeasurement: Contains single epoch forced photometry of individual measurements of objects detected in the stacked images.  The identifiers connecting the measurement back to the original image and to the object association are provided.  PSF, aperture, and \citet{Kron1980} photometry are included, along with sky and detector coordinate positions.}
 \begin{center}
@@ -4716 +4881 @@
 FpsfQfPerfect & - & REAL & -999  &PSF weighted fraction of pixels totally unmasked.\\
 FpsfChiSq & - & REAL & -999  &Reduced chi squared value of the PSF model fit.\\
-FmomentXX & $arcsec^2$ & REAL & -999  &Second moment $M_{xx}$.\\
-FmomentXY & $arcsec^2$ & REAL & -999  &Second moment $M_{xy}$.\\
-FmomentYY & $arcsec^2$ & REAL & -999  &Second moment $M_{yy}$.\\
+FmomentXX & arcsec$^2$ & REAL & -999  &Second moment $M_{xx}$.\\
+FmomentXY & arcsec$^2$ & REAL & -999  &Second moment $M_{xy}$.\\
+FmomentYY & arcsec$^2$ & REAL & -999  &Second moment $M_{yy}$.\\
 FmomentR1 & arcsec & REAL & -999  &First radial moment.\\
-FmomentRH & $arcsec^{0.5}$ & REAL & -999  &Half radial moment ($r^{0.5}$ weighting).\\
-FmomentM3C & $arcsec^2$ & REAL & -999  &Cosine of trefoil second moment term: $r^2 cos(3 theta) = M_{xxx} - 3 * M_{xyy}$.\\
-FmomentM3S & $arcsec^2$ & REAL & -999  &Sine of trefoil second moment: $r^2 sin (3 theta) = 3 * M_{xxy} - M_{yyy}$.\\
-FmomentM4C & $arcsec^2$ & REAL & -999  &Cosine of quadrupole second moment: $r^2 cos (4 theta) = M_{xxxx} - 6 * M_{xxyy} + M_{yyyy}$.\\
-FmomentM4S & $arcsec^2$ & REAL & -999  &Sine of quadrupole second moment: $r^2 sin (4 theta) = 4 * M_{xxxy} - 4 * M_{xyyy}$.\\
+FmomentRH & arcsec$^{0.5}$ & REAL & -999  &Half radial moment ($r^{0.5}$ weighting).\\
+FmomentM3C & arcsec$^2$ & REAL & -999  &Cosine of trefoil second moment term: $r^2 \cos(3 \theta) = M_{xxx} - 3 M_{xyy}$.\\
+FmomentM3S & arcsec$^2$ & REAL & -999  &Sine of trefoil second moment: $r^2 \sin (3 \theta) = 3 M_{xxy} - M_{yyy}$.\\
+FmomentM4C & arcsec$^2$ & REAL & -999  &Cosine of quadrupole second moment: $r^2 \cos (4 \theta) = M_{xxxx} - 6 M_{xxyy} + M_{yyyy}$.\\
+FmomentM4S & arcsec$^2$ & REAL & -999  &Sine of quadrupole second moment: $r^2 \sin (4 \theta) = 4 M_{xxxy} - 4 M_{xyyy}$.\\
 FapFlux & Jy & REAL & -999  &Aperture flux.\\
 FapFluxErr & Jy & REAL & -999  &Error in aperture flux.\\
@@ -4732 +4897 @@
 FkronFluxErr & Jy & REAL & -999  &Error in Kron (1980) flux.\\
 FkronRad & arcsec & REAL & -999  &Kron (1980) radius.\\
-Fsky & $Jy/arcsec^2$ & REAL & -999  &Background sky level.\\
-FskyErr & $Jy/arcsec^2$ & REAL & -999  &Error in background sky level.\\
+Fsky & Jy arcsec$^{-2}$ & REAL & -999  &Background sky level.\\
+FskyErr & Jy arcsec$^{-2}$ & REAL & -999  &Error in background sky level.\\
 FinfoFlag & - & BIGINT & 0  &Information flag bitmask indicating details of the photometry.  \\
 & & & & Values listed in DetectionFlags.\\
@@ -4749 +4914 @@
 
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ForcedWarpMasked: Contains an entry for objects detected in the stacked images which were in the footprint of a single epoch exposure, but for which there are no unmasked pixels at that epoch.}
 \begin{center}
@@ -4778 +4943 @@
 \end{table}%
 
-\begin{table}[b]
-\caption{ForcedWarpExtended: Contains the single epoch forced photometry fluxes within the SDSS R5 (r = 3.00 arcsec), R6 (r = 4.63 arcsec), and R7 (r = 7.43 arcsec) apertures \citep{Stoughton2002} for objects detected in the stacked images.}
+\begin{table}[htb]
+\caption{ForcedWarpExtended: Contains the single epoch forced photometry fluxes within the SDSS R5 (r = 3.00\arcsec), R6 (r = 4.63\arcsec), and R7 (r = 7.43\arcsec) apertures \citep{Stoughton2002} for objects detected in the stacked images.}
 \begin{center}
 %\resizebox{\textwidth}{!}{%
@@ -4802 +4967 @@
 obsTime & days & FLOAT & -999  &Modified Julian Date at the midpoint of the observation.\\
 flxR5 & Jy & REAL & -999  &Flux from forced photometry measurement within an aperture of radius \\
-& & & & r = 3.00 arcsec.\\
+& & & & r = 3.00\arcsec.\\
 flxR5Err & Jy & REAL & -999  &Error in flux from forced photometry measurement within an aperture of\\
-& & & & radius r = 3.00 arcsec.\\
+& & & & radius r = 3.00\arcsec.\\
 flxR5Std & Jy & REAL & -999  &Standard deviation of flux from forced photometry measurement within \\
-& & & & an aperture of radius r = 3.00 arcsec.\\
+& & & & an aperture of radius r = 3.00\arcsec.\\
 flxR5Fill & - & REAL & -999  &Aperture fill factor for forced photometry measurement within an \\
-& & & & aperture of radius r = 3.00 arcsec.\\
+& & & & aperture of radius r = 3.00\arcsec.\\
 flxR6 & Jy & REAL & -999  &Flux from forced photometry measurement within an aperture of radius \\
-& & & & r = 4.63 arcsec.\\
+& & & & r = 4.63\arcsec.\\
 flxR6Err & Jy & REAL & -999  &Error in flux from forced photometry measurement within an aperture of\\
-& & & & radius r = 4.63 arcsec.\\
+& & & & radius r = 4.63\arcsec.\\
 flxR6Std & Jy & REAL & -999  &Standard deviation of flux from forced photometry measurement within \\
-& & & & an aperture of radius r = 4.63 arcsec.\\
+& & & & an aperture of radius r = 4.63\arcsec.\\
 flxR6Fill & - & REAL & -999  &Aperture fill factor for forced photometry measurement within an \\
-& & & & aperture of radius r = 4.63 arcsec.\\
+& & & & aperture of radius r = 4.63\arcsec.\\
 flxR7 & Jy & REAL & -999  &Flux from forced photometry measurement within an aperture of radius \\
-& & & & r = 7.43 arcsec.\\
+& & & & r = 7.43\arcsec.\\
 flxR7Err & Jy & REAL & -999  &Error in flux from forced photometry measurement within an aperture of\\
-& & & & radius r = 7.43 arcsec.\\
+& & & & radius r = 7.43\arcsec.\\
 flxR7Std & Jy & REAL & -999  &Standard deviation of flux from forced photometry measurement within \\
-& & & & an aperture of radius r = 7.43 arcsec.\\
+& & & & an aperture of radius r = 7.43\arcsec.\\
 flxR7Fill & - & REAL & -999  &Aperture fill factor for forced photometry measurement within an \\
-& & & & aperture of radius r = 7.43 arcsec.\\
+& & & & aperture of radius r = 7.43\arcsec.\\
 \hline
 \end{tabular}
@@ -4833 +4998 @@
 
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ForcedWarpLensing: Contains the \citet[K95]{Kaiser1995} lensing parameters measured from the forced photometry of objects detected in stacked images on the individual single epoch data.}
 \begin{center}
@@ -4856 +5021 @@
 dvoRegionID & - & INT & -1  &Internal DVO region identifier.\\
 obsTime & days & FLOAT & -999  &Modified Julian Date at the midpoint of the observation.\\
-lensObjSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced photometry.\\
-lensObjSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced photometry.\\
-lensObjSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced photometry.\\
-lensObjSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced photometry.\\
-lensObjSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced photometry.\\
+lensObjSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from forced photometry.\\
+lensObjSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from forced photometry.\\
+lensObjSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from forced photometry.\\
+lensObjSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from forced photometry.\\
+lensObjSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from forced photometry.\\
 lensObjShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from forced photometry.\\
 lensObjShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from forced photometry.\\
@@ -4866 +5031 @@
 lensObjShearE1 & - & REAL & -999  &K95 eq. (B12) shear polarizability e1 term from forced photometry.\\
 lensObjShearE2 & - & REAL & -999  &K95 eq. (B12) shear polarizability e2 term from forced photometry.\\
-lensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced photometry.\\
-lensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced photometry.\\
-lensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced photometry.\\
-lensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced photometry.\\
-lensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced photometry.\\
+lensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X11 term from PSF model for forced photometry.\\
+lensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X12 term from PSF model for forced photometry.\\
+lensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A11) smear polarizability X22 term from PSF model for forced photometry.\\
+lensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e1 term from PSF model for forced photometry.\\
+lensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999  &K95 eq. (A12) smear polarizability e2 term from PSF model for forced photometry.\\
 lensPSFShearX11 & - & REAL & -999  &K95 eq. (B11) shear polarizability X11 term from PSF model for forced photometry.\\
 lensPSFShearX12 & - & REAL & -999  &K95 eq. (B11) shear polarizability X12 term from PSF model for forced photometry.\\
@@ -4888 +5053 @@
 
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ForcedWarpToImage: Contains the mapping of which input image comprises a particular \ippstage{warp} image used for forced photometry.}
 \begin{center}
@@ -4898 +5063 @@
 \hline
 forcedWarpID & - & BIGINT & NA  &Unique forced \ippstage{warp} identifier.\\
-imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 * frameID + ccdID).\\
+imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 $\times$ frameID + ccdID).\\
 \hline
 \end{tabular}
@@ -4907 +5072 @@
 % \subsection{Forced Galaxy Tables}
 
-\begin{table}[b]
-\caption{ForcedGalaxyShape: Contains the extended source galaxy shape parameters.  All filters are matched into a single row.  The positions, magnitudes, fluxes, and Sersic indices are inherited from their parent measurement in the StackModelFit tables, and are reproduced here for convenience.  The major and minor axes and orientation are recalculated on a warp-by-warp basis from the best fit given these inherited properties (\citep{Sersic1963}).}
+\begin{table}[htb]
+\caption{ForcedGalaxyShape: Contains the extended source galaxy shape parameters.  All filters are matched into a single row.  The positions, magnitudes, fluxes, and \Sersic\ indices are inherited from their parent measurement in the StackModelFit tables, and are reproduced here for convenience.  The major and minor axes and orientation are recalculated on a warp-by-warp basis from the best fit given these inherited properties (\citep{Sersic1963}).}
 \begin{center}
 %\resizebox{\textwidth}{!}{%
@@ -4932 +5097 @@
 gGalMagErr & AB & REAL & -999  &Error in galaxy fit magnitude for g filter measurement.\\
 gGalPhi & degrees & REAL & -999  &Major axis position angle of the model fit for the g filter measurement.\\
-gGalIndex & - & REAL & -999  &Sersic index of the model fit for the g filter measurement.\\
+gGalIndex & - & REAL & -999  &\Sersic\ index of the model fit for the g filter measurement.\\
 gGalFlags & - & SMALLINT & -999  &Analysis flags for the galaxy model chi-square fit (g filter measurement, values \\
 & & & & defined in ForcedGalaxyShapeFlags).\\
@@ -4997 +5162 @@
 \subsection{Tables Related to Difference Image Analysis}
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{DiffDetObject: Contains the positional information for difference detection objects in a number of coordinate systems.  The objects associate difference detections within a one arcsecond radius.  The number of detections in each filter from is listed, along with maximum coverage fractions \citep[see][]{Szalay2007}.}
 \begin{center}
@@ -5060 +5225 @@
 % \subsection{Diff Detection Tables}
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{DiffMeta: Contains metadata related to a difference image constructed by subtracting a stacked image from a single epoch image, or in the case of the MD Survey from a nightly \ippstage{stack} (stack made from all exposures in a single filter in a single night).  The astrometric calibration of the reference \ippstage{stack} is listed.}
 \begin{center}
@@ -5124 +5289 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{DiffDetection: Contains the photometry of individual detections from a difference image.  The identifiers connecting the detection back to the difference image and to the object association are provided.  PSF, aperture, and \citet{Kron1980} photometry are included, along with sky and detector coordinate positions.}
 \begin{center}
@@ -5176 +5341 @@
 DpsfChiSq & - & REAL & -999  &Reduced chi squared value of the PSF model fit.\\
 DpsfLikelihood & - & REAL & -999  &Likelihood that this detection is best fit by a PSF.\\
-DmomentXX & $arcsec^2$ & REAL & -999  &Second moment $M_{xx}$.\\
-DmomentXY & $arcsec^2$ & REAL & -999  &Second moment $M_{xy}$.\\
-DmomentYY & $arcsec^2$ & REAL & -999  &Second moment $M_{yy}$.\\
+DmomentXX & arcsec$^2$ & REAL & -999  &Second moment $M_{xx}$.\\
+DmomentXY & arcsec$^2$ & REAL & -999  &Second moment $M_{xy}$.\\
+DmomentYY & arcsec$^2$ & REAL & -999  &Second moment $M_{yy}$.\\
 DmomentR1 & arcsec & REAL & -999  &First radial moment.\\
-DmomentRH & $arcsec^{0.5}$ & REAL & -999  &Half radial moment ($r^{0.5}$ weighting).\\
+DmomentRH & arcsec$^{0.5}$ & REAL & -999  &Half radial moment ($r^{0.5}$ weighting).\\
 DapFlux & Jy & REAL & -999  &Aperture flux.\\
 DapFluxErr & Jy & REAL & -999  &Error in aperture flux.\\
@@ -5200 +5365 @@
 diffPosSN & - & REAL & -999  &Signal to noise of matching source in positive image.\\
 diffNegSN & - & REAL & -999  &Signal to noise of matching source in negative image.\\
-Dsky & $Jy/arcsec^2$ & REAL & -999  &Background sky level.\\
-DskyErr & $Jy/arcsec^2$ & REAL & -999  &Error in background sky level.\\
+Dsky & Jy arcsec$^{-2}$ & REAL & -999  &Background sky level.\\
+DskyErr & Jy arcsec$^{-2}$ & REAL & -999  &Error in background sky level.\\
 DinfoFlag & - & BIGINT & 0  &Information flag bitmask indicating details of the photometry. see DetectionFlags.\\
 DinfoFlag2 & - & INT & 0  &Information flag bitmask indicating details of the photometry.  see DetectionFlags2.\\
@@ -5213 +5378 @@
 
  
-\begin{table}[b]
+\begin{table}[htb]
 \caption{DiffToImage: Contains the mapping of which input images were used to construct a particular difference image.}
 \begin{center}
@@ -5223 +5388 @@
 \hline
 diffImageID & - & BIGINT & NA  &Unique difference identifier.\\
-imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 * frameID + ccdID).\\
+imageID & - & BIGINT & NA  &Unique image identifier.  Constructed as (100 $\times$ frameID + ccdID).\\
 \hline
 \end{tabular}
@@ -5230 +5395 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{DiffDetEffMeta: Contains the detection efficiency information for a given individual difference image.  Provides the number of recovered sources out of 500 injected sources and statistics about the magnitudes of the recovered sources for a range of magnitude offsets.}
 \begin{center}
@@ -5282 +5447 @@
 system for objects).  
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{ObjectThin: This describes the sources for each of the columns within ippdbtable{ObjectThin} as well the formula to generate the data within the column, if it is not just copying directly. For this table, DVO cpt NAME shows that this comes from the cpt files in the DVO database, and has a column of NAME.  The sources for this table include: the DVO cpt files, \ippstage{IppToPsps}, PSPS, as well as a few columns that are not currently being used.}
 \begin{center}
@@ -5347 +5512 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{MeanObject: This describes the sources for each of the columns within MeanObject as well the formula to generate the data within the column, if it is not just copying directly. For this table, DVO cps NAME shows that this comes from the cps files in the DVO database, and has a column of NAME.  The sources for this table include: the DVO cps files and \ippstage{IppToPsps}.}
 \begin{center}
@@ -5383 +5548 @@
 \end{table}%
 
-\begin{table}[b]
+\begin{table}[htb]
 \caption{StackObjectThin: This describes the sources for each of the columns within StackObjectThin as well the formula to generate the data within the column, if it is not just copying directly. For this table, DVO cps NAME shows that this comes from the cps files in the DVO database, and has a column of NAME.  The sources for this table include: the DVO cps files and \ippstage{IppToPsps}.}
 \begin{center}

trunk/doc/release.2015/ps1.dataproducts/fundamentalipp.tex

@@ -28 +28 @@
              & ForcedGalaxyShape     & dvo & DR2\\
              & ForcedWarpMasked      & dvo and forced warp cmf & DR2\\
-Difference   & DiffDetection         & dvo and diff skycal cmf & DR2\\
-             & DiffDetObject         & dvo  & DR2\\
+Difference   & DiffDetection         & dvo and diff skycal cmf & DR3\\
+             & DiffDetObject         & dvo  & DR3\\
 \hline            
 \end{tabular}

trunk/doc/release.2015/ps1.dataproducts/objid.tex

@@ -1 +1 @@
 \begin{figure}
 %\centerline{\includegraphics[width=1.1\columnwidth,angle=0]{objid.pdf}}
-
 \centerline{\includegraphics[width=\columnwidth,angle=0]{objid.pdf}}
-
-\note{FIX THE EXAMPLE NUMBERS (see email from Rick)}
-
+% \note{FIX THE EXAMPLE NUMBERS (see email from Rick)}
 \vskip -0.5cm
 \caption{Graphical description of how \texttt{ObjID} is calculated from RA and Dec. It is not recommended to derive the RA and Dec from the \texttt{objID} as this will result in an innaccurate RA and Dec, the \texttt{ObjID} is assigned when the stack/skycal cmfs are ingested into the database, and are not yet calibrated against 2MASS and Gaia. ObjID is primarily used for indexing the database. }

trunk/doc/release.2015/ps1.dataproducts/pspstables.tex

@@ -15 +15 @@
 StackType & System Metadata & DR1 \\
 DiffType& System Metadata & DR1 \\
-Tessellation Type& System Metadata & DR1 \\
+TessellationType & System Metadata & DR1 \\
 ImageFlags& System Metadata & DR1 \\
 DetectionFlags& System Metadata & DR1 \\

trunk/doc/release.2015/ps1.dataproducts/report.v0.txt

@@ -22 +22 @@
 it is also still a *relational* SQL database, so that should be mentioned as well.
 
->> TBD
+>> the use of the word 'hierarchical' in that sentence was irrelevant.
+   We've removed that word, but added a following paragraph to
+   introduce these database concepts to the reader.
 
 * Page 2, Section 3: The release dates for DR1 and DR2 are mentioned here.
@@ -42 +44 @@
 http with https wherever that changeover has been made.
 
->> TBD
+>> Fixed this one and checked all URLs
 
 * Page 6, Section 5.1.6, last paragraph: Has the reconstruction of
@@ -48 +50 @@
 reference or give an example in the sample queries appendix.
 
->> TBD
+>> reconstruction of difference images within the IPP is regularly
+   used, but an implementation of this process at MAST has not been
+   developed.  The text has been modified to explain the concept and
+   current status within the IPP.
 
 * Page 10, Section 6.5: Isn't it Simple Object Access? Please provide a
 reference and/or URL for SOAP.
 
->> TBD
+>> correct -- URL to W3C specification added
 
 * Page 19, Section 7.7: I understand the reason for using a number such as
@@ -63 +68 @@
 developers can probably assist with that.
 
->> TBD
+>> The linked microsoft technical report has not been published in a
+refereed journal, but it has been placed on the arxiv, so we have adjusted the
+reference to cite that article.
 
 * Page 21, Section 8.1.1: What total area of the sky is affected by the polar
@@ -69 +76 @@
 described in Paper IV, but it's worth including a single sentence here.
 
+>> Added words to describe the affected area.
+
 * Appendix, Table Schema: The authors should detail how they ensure that all
 the table and column descriptions are accurate. For example, what automation,
 if any, is used to convert SQL table definitions into these LaTeX tables?
+
+>> added a mention of the XML-to-LaTeX translation code.
 
 SQL Examples
@@ -82 +93 @@
 * It is not clear from this section which specific context to use. I used DR2.
 
+>> yes, these queries are meant for DR2.  Text updated to reflect this.
+
 A particular database context should be explicitly mentioned and some names
 should be checked for consistency with that context. You could also state
@@ -91 +104 @@
 an arithmetic overflow exception.
 
+>>> yes, we added a word of warning.
+
 * Example 2: This query returned 3868 rows in DR2, not 3867.
 
@@ -97 +112 @@
 * Example 5: This query returned 1806 objects in DR2, not 1805.
 
+>>> our retry confirms these numbers: numbers in text updated (for all three).
+
 * Example 9: Most of the objects selected have -999 for gMeanPSFMag.
 Is this expected?
+
+>> It is expected, added text to note and explain.
 
 * Example 10: The name of the MyDB table implies DR2. Again, choose a specific
 context or rename to be data-release agnostic.
 
+>> context for all examples is DR2
+
 * Example 12: Is there a reason the MyDB table name is enclosed in brackets in
 one example and not the other? Also the '_PS1' name doesn't seem to be
 consistent with the apparent DR2 context.
+
+>> the square brackets are always allowed, but are needed to protect
+   table names with spaces or special words.  changed the examples to
+   all used square brackets.  The _PS1 addition is meant to identify
+   the table containing results for PS1 (vs Gaia) and would be
+   appropriate for either DR1 or DR2 (both from PS1).
 
 Spelling, Typos, etc.
@@ -115 +142 @@
 * In general: Hawaii or Hawai'i?
 
+>> should be all Hawai`i, except in the adjective Hawaiian
+
 * In general: Check terms like 'Section', 'Table', 'Figure' (vs. 'Fig') for
 consistency.
 
+>> fixed
+
 * In general: Spell Sérsic consistently throughout the paper.
+
+>> fixed
 
 * In general: Choose a single notation for RA (RA vs. R.A.).
 
+>> fixed (to R.A.)
+
 * Page 1, 1st paragraph: "perform as set of astronomical" -> "as a set".
+
+>> "perform a set of..."
 
 * Page 2, Table 1: There seem to be several different quotation conventions in
 the paper, e.g. `Release'. Elsewhere double quotes are used.
 
+>> fixed (all double quotes)
+
 * Page 2, Table 1: "Tessellation Type" -> "TessellationType"
+
+>> fixed
 
 * Page 5, Section 5.1.4: in the description of SDSS apertures, double prime
@@ -134 +175 @@
 both notations are used in the paper.
 
+>> converted instances of XX arcsec to XX" where XX is numerical.
+   Entries as units in tables and the rare case of a word (one
+   arcsecond) are written out.
+
 * Page 10: "csv, FITS or xml"; CSV and XML are acronyms just like FITS, so the
 same typography should be used.
 
+>> fixed
+
 * Page 21, Section 8.1.1: "This issues" -> "This issue".
 
+>> fixed
+
 * Page 22, Section 9: Use official IAU designation for Oumuamua.
+
+>> fixed