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trunk/doc/release.2015/ps1.dataproducts/dataproducts.tex
r41399 r41401 50 50 \newcommand\showfigure[1]{\input{#1}} 51 51 %\newcommand\showfigure[1]{} 52 53 \newcommand\Sersic{S{\'e}rsic} 52 54 53 55 \def\Ha{H{$\alpha$}} … … 110 112 \shortauthors{H. A. Flewelling} 111 113 114 \def\IfA{1} 115 \def\CFHT{2} 116 \def\BackYard{3} 117 \def\STSCI{4} 118 \def\Google{5} 119 \def\MPE{6} 120 \def\SpireGlobal{7} 121 \def\DUR{8} 122 \def\DurComp{9} 123 \def\DurCEA{10} 124 \def\JHU{11} 125 \def\Princeton{12} 112 126 113 127 \begin{document} 114 128 \title{The Pan-STARRS1 Database and Data Products} 115 129 \author{ 116 H.~A.~Flewelling\altaffilmark{ 1},117 E.~A.~Magnier\altaffilmark{ 1},118 K.~C.~Chambers\altaffilmark{ 1},119 J.~N.~Heasley\altaffilmark{ 8},120 C.~Holmberg\altaffilmark{ 1},121 M.~E.~Huber\altaffilmark{ 1},122 W.~Sweeney\altaffilmark{ 1},123 C.~Z.~Waters\altaffilmark{ 1},124 A.~Calamida\altaffilmark{ 4},125 S.~Casertano\altaffilmark{ 4},126 X.~Chen\altaffilmark{ 10},127 D.~Farrow\altaffilmark{ 5}128 G.~Hasinger\altaffilmark{ 1},129 R.~Henderson\altaffilmark{ 11},130 K.~S.~Long\altaffilmark{ 4},131 N.~Metcalfe\altaffilmark{ 2},132 G.~Narayan\altaffilmark{ 4},133 M.~A.~Nieto-Santisteban\altaffilmark{ 4},134 P.~Norberg\altaffilmark{ 6,7},135 A.~Rest\altaffilmark{ 4},136 R.~P.~Saglia\altaffilmark{ 5},137 A.~Szalay\altaffilmark{ 3},138 A.~R.~Thakar\altaffilmark{ 3},139 J.~L.~Tonry\altaffilmark{ 1},140 J.~Valenti\altaffilmark{ 4},141 S.~Werner\altaffilmark{ 3},142 R.~White\altaffilmark{ 4},130 H.~A.~Flewelling\altaffilmark{\IfA,\CFHT}, 131 E.~A.~Magnier\altaffilmark{\IfA}, 132 K.~C.~Chambers\altaffilmark{\IfA}, 133 J.~N.~Heasley\altaffilmark{\BackYard}, 134 C.~Holmberg\altaffilmark{\IfA}, 135 M.~E.~Huber\altaffilmark{\IfA}, 136 W.~Sweeney\altaffilmark{\IfA}, 137 C.~Z.~Waters\altaffilmark{\IfA}, 138 A.~Calamida\altaffilmark{\STSCI}, 139 S.~Casertano\altaffilmark{\STSCI}, 140 X.~Chen\altaffilmark{\Google}, 141 D.~Farrow\altaffilmark{\MPE} 142 G.~Hasinger\altaffilmark{\IfA}, 143 R.~Henderson\altaffilmark{\SpireGlobal}, 144 K.~S.~Long\altaffilmark{\STSCI}, 145 N.~Metcalfe\altaffilmark{\DUR}, 146 G.~Narayan\altaffilmark{\STSCI}, 147 M.~A.~Nieto-Santisteban\altaffilmark{\STSCI}, 148 P.~Norberg\altaffilmark{\DurComp,\DurCEA}, 149 A.~Rest\altaffilmark{\STSCI}, 150 R.~P.~Saglia\altaffilmark{\MPE}, 151 A.~Szalay\altaffilmark{\JHU}, 152 A.~R.~Thakar\altaffilmark{\JHU}, 153 J.~L.~Tonry\altaffilmark{\IfA}, 154 J.~Valenti\altaffilmark{\STSCI}, 155 S.~Werner\altaffilmark{\JHU}, 156 R.~White\altaffilmark{\STSCI}, 143 157 % 144 L.~Denneau\altaffilmark{ 1},145 P.~W.~Draper\altaffilmark{ 2},146 K.~W.~Hodapp\altaffilmark{ 1},147 R.~Jedicke\altaffilmark{ 1},148 N.~Kaiser\altaffilmark{ 1},149 R.~P.~Kudritzki\altaffilmark{ 1},150 P.~A.~Price\altaffilmark{ 9},151 R.~J.~Wainscoat\altaffilmark{ 1},152 % P.~S.~Builders\altaffilmark{PS1},153 S.~Chastel\altaffilmark{ 1},154 B.~McLean\altaffilmark{ 4},155 M.~Postman\altaffilmark{ 4},156 B.~Shiao\altaffilmark{ 4}.158 L.~Denneau\altaffilmark{\IfA}, 159 P.~W.~Draper\altaffilmark{\DUR}, 160 K.~W.~Hodapp\altaffilmark{\IfA}, 161 R.~Jedicke\altaffilmark{\IfA}, 162 N.~Kaiser\altaffilmark{\IfA}, 163 R.~P.~Kudritzki\altaffilmark{\IfA}, 164 P.~A.~Price\altaffilmark{\Princeton}, 165 R.~J.~Wainscoat\altaffilmark{\IfA}, 166 % 167 S.~Chastel\altaffilmark{\IfA}, 168 B.~McLean\altaffilmark{\STSCI}, 169 M.~Postman\altaffilmark{\STSCI}, 170 B.~Shiao\altaffilmark{\STSCI}. 157 171 } 158 172 159 160 161 \altaffiltext{1}{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, Hawaii 96822, USA} 162 \altaffiltext{2}{Department of Physics, Durham University, South Road, Durham DH1 3LE, UK} 163 \altaffiltext{6}{Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK} 164 \altaffiltext{7}{Centre for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK} 165 \altaffiltext{3}{Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA} 166 \altaffiltext{4}{Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA} 167 \altaffiltext{5}{ Max-Planck Institut f\"ur extraterrestrische Physik, Giessenbachstra\ss e 1, D-85748 Garching, Germany} 168 \altaffiltext{8}{Back Yard Observatory, P.O. BOX 68856, Tucson, AZ 85737} 169 \altaffiltext{9}{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA} 170 \altaffiltext{10}{Google Inc., 1600 Amphitheatre Pkwy, Mountain View, CA 94043} 171 \altaffiltext{11}{Spire Global, Sky Park 5,45 Finnieston Street, Glasgow, G3 8JU, UK } 173 \altaffiltext{\IfA}{Institute for Astronomy, University of Hawai`i, 2680 Woodlawn Drive, Honolulu, Hawai`i 96822, USA} 174 \altaffiltext{\CFHT}{Canada-France-Hawai`i Telescope, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743, USA} 175 \altaffiltext{\BackYard}{Back Yard Observatory, P.O. BOX 68856, Tucson, AZ 85737} 176 \altaffiltext{\STSCI}{Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA} 177 \altaffiltext{\Google}{Google Inc., 1600 Amphitheatre Pkwy, Mountain View, CA 94043} 178 \altaffiltext{\MPE}{Max-Planck Institut f\"ur extraterrestrische Physik, Giessenbachstra\ss e 1, D-85748 Garching, Germany} 179 \altaffiltext{\SpireGlobal}{Spire Global, Sky Park 5,45 Finnieston Street, Glasgow, G3 8JU, UK } 180 \altaffiltext{\DUR}{Department of Physics, Durham University, South Road, Durham DH1 3LE, UK} 181 \altaffiltext{\DurComp}{Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK} 182 \altaffiltext{\DurCEA}{Centre for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK} 183 \altaffiltext{\JHU}{Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA} 184 \altaffiltext{\Princeton}{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA} 172 185 % \altaffiltext{PS1}{Pan-STARRS1 Builders} 173 186 %\begin{document} … … 226 239 \section{Introduction}\label{sec:introduction} 227 240 228 For nearly four years, from 2010 May through 2014 March, the 1.8m \PS\ telescope (PS1) was used to perform a s 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.241 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. 229 242 230 243 % Operating under the aegis of the Pan-STARRS Science Consortium, … … 247 260 The Pan-STARRS Project teamed with Alex Szalay's database development 248 261 group at The Johns Hopkins University (JHU) to undertake the task of 249 providing a publicly accessible hierarchicaldatabase for262 providing a publicly accessible database for 250 263 \PS\ \citep{Heasley2008}. The JHU team was the major developer of the 251 264 Sloan Digital Sky Survey (SDSS) public database \citep{Thakar2003}, … … 262 275 The system developed for \PS\ is called the {\em Published Science 263 276 Products Subsystem}, or PSPS \citep{Heasley2006}. 264 \note{define hierarchical, note relational} 265 266 267 %(SDSS) public database \citep{Thakar2003}, and it is useful to reuse as much of the software developed for the SDSS as possible. However, due 268 %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 269 %includes measurements on the stacks, single exposures, and mean properties of each, major changes were required. The system developed is 270 %called the {\em Published Science Products Subsystem}, or PSPS \citep{Heasley2006}. 271 272 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. 277 278 \textadd{As a widely-used database engine, the Microsoft SQL Server provides a 279 robust tool to define, build, and query the full database. The engine 280 implements the SQL relational database language: data within different 281 tables of the database are related to data in other tables by common 282 fields, or indexes. In the PSPS implementation, the relationships are 283 largely hierarchical: many measurements are linked to the images from 284 which they came; associated measurements from the same astrophysical 285 object are linked together to those objects. The tables use unique 286 indexes to form these relationships, as detailed throughput this article.} 287 288 %(SDSS) public database \citep{Thakar2003}, and it is useful to reuse 289 %as much of the software developed for the SDSS as possible. However, 290 %due to the Pan-STARRS's data having a larger intrinsic size and more 291 %complicated dataset, which covers a larger area of sky than SDSS and 292 %which includes measurements on the stacks, single exposures, and mean 293 %properties of each, major changes were required. The system developed 294 %is called the {\em Published Science Products Subsystem}, or PSPS 295 %\citep{Heasley2006}. 296 297 The most significant challenge for the PSPS relative to the SDSS 298 database implementation was the need to address the very large volume 299 of \PS\ data. The single monolithic database design of SDSS could not 300 scale to the level needed for PS1 data. While SQL Server does not 301 have (at present) a cluster implementation, a bespoke version can be 302 crafted using a combination of distributed partition views and data 303 slices~\citep{Heasley2008}. Partitioning data into smaller databases 304 spread over multiple server machines allows the information to be 305 presented to the users as a single, unified table. 273 306 274 307 %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} 317 350 351 % https://panstarrs.stsci.edu is OK (2020.08.13) 352 % https://mastweb.stsci.edu/mcasjobs is OK (2020.08.13) 353 318 354 Public access to the Pan-STARRS data is through the web server located 319 at \url{http://panstarrs.stsci.edu} and is hosted by the {\em 320 Barbara A. Mikulski Archive for Space Telescopes} (MAST) at 355 at \url{https://panstarrs.stsci.edu} 356 % http is OK here 357 and is hosted by the {\em 358 Barbara A. Mikulski Archive for Space Telescopes} (MAST) at 321 359 STScI. MAST provides the access point for downloading different pixel 322 360 data products and their associated metadata and source catalogs. This … … 328 366 Pan-STARRS tables is available through the Catalog Archive Server Jobs 329 367 System (CasJobs) interface (see description at 330 \url{http ://mastweb.stsci.edu/mcasjobs}). CasJobs emulates local368 \url{https://mastweb.stsci.edu/mcasjobs}). CasJobs emulates local 331 369 free-form SQL access in a web environment, and provides both 332 370 synchronous and asynchronous query execution. The interface can … … 353 391 preferred to making a new measurement directly from the available 354 392 released pixel data, and care should be taken when using the 355 recalibrated astrometry with the original images (see Table 356 \ref{table:fundamentalipp}). 393 recalibrated astrometry with the original images (see Table~\ref{table:fundamentalipp}). 357 394 358 395 \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 384 421 the user. For more information on views, including the currently 385 defines ones, see Table 422 defines ones, see Table~\ref{table:views}. 386 423 387 424 This paper covers the data products and schema for the 3$\pi$ data … … 422 459 \label{sec:chipandcamera} 423 460 424 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 DR2.461 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. 425 462 426 463 … … 428 465 \label{sec:fakeandwarp} 429 466 430 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.467 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. 431 468 432 469 The warp image products are available to users via MAST for the $3\pi$ survey as part of DR2. … … 435 472 \label{sec:stackstages} 436 473 437 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}.474 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}. 438 475 439 476 \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. 442 479 443 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 Table7 in ][]{Stoughton2002}. For more details on the photometric analysis of the stack images, see Paper IV.444 445 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.480 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. 481 482 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. 446 483 447 484 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. 455 492 456 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) Sersicradius 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.493 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. 457 494 458 495 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. 476 513 477 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. 478 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. 514 For the difference image analysis, the input images (\ippstage{stack} 515 or \ippstage{warp}) are convolved to have similar PSFs 516 \citep{Waters2017} and one subtracted from the other. Sources are 517 detected on the difference image, basic photometry is performed on the 518 sources, and \ippstage{diff} catalog files are created. The 519 \ippstage{diff} catalog files are then ingested into the 520 \ippstage{diff} DVO, and later ingested into the PSPS. The results 521 from this stage of processing include diff catalog files, which will 522 be available in a future release (nominally DR3). \textmod{At this 523 time, it is undecided if, as part of DR3, the complete collection of 524 PV3 difference images will be 525 stored at MAST or if they will be generated on demand. Within the 526 IPP, difference images are generally stored on disk only for a short 527 period of time (days to weeks) in order to save on storage space. 528 When needed, historical difference images are regularly regenerated based on stored 529 results (difference kernels and PSF models). MAST may rely on this 530 process for DR3.} 479 531 480 532 \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. 493 545 494 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 Aand 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).495 496 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 Aand 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).497 498 \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 Aand Dec are listed in these files.546 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). 547 548 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). 549 550 \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. 499 551 500 552 \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). 569 621 570 \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 Aand 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.622 \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. 571 623 572 624 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} 588 640 589 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}641 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} 590 642 591 643 % \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. 600 652 601 \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.653 \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. 602 654 603 655 \input{pspsslicetable.tex} … … 609 661 \showfigure{psps_loadprocess.tex} 610 662 611 \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. 663 % https://mastweb.stsci.edu/ps1casjobs is OK (2020.08.13) 664 % https://catalogs.mast.stsci.edu/panstarrs is OK (2020.08.13) 665 666 \subsection{The Data Retrieval Layer (DRL)} 667 The DRL is the layer between the user and the PSPS database. The DRL 668 is responsible for management of queries that the user submits via the 669 DRL API. The DRL is based on CasJobs \citep{Szalay2007}, and has many 670 similar features. It primarily keeps track of all user queries and 671 provides progress updates of those queries in a secure way. It also 672 kills queries that use too many resources or take too long. The DRL 673 API is accessed via \textmod{Simple Object Access Protocol (SOAP, \url{w3.org/TR/soap})}, 674 allowing users multiple ways to access the database. Before the 675 public releases, Pan-STARRS science consortium members used the 676 Published Science Interface (PSI, a web-based user interface) 677 initially based at the IfA and later at STScI. For the general 678 public, the MAST server provides access via the CasJobs interface 679 (\url{https://mastweb.stsci.edu/ps1casjobs/}), as well as a simple 680 object search form which implements a basic cone search 681 (\url{https://catalogs.mast.stsci.edu/panstarrs}). It is also 682 possible for the consortium users to query the database via SOAP calls 683 from command line scripts. 612 684 613 685 %A flowchart of the DRL can be seen in Figure~\ref{fig:psps_drl}. … … 617 689 % Bernie says 'no' 618 690 619 \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 xmlfiles 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.691 \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. 620 692 % SC: consider removing most of the PSI content. The last sentence mostly replicates previous content. 621 693 … … 652 724 \ippdbtable{Detection} table, using \ippdbcolumn{objID}, in order to get the 653 725 individual photometric attributes for all the detections of that 654 object within the single exposures (at a given R Aand Dec).726 object within the single exposures (at a given R.A. and Dec). 655 727 656 728 % \subsection{\ippdbcolumn{objID} and its relation to R.A. and Dec.} … … 659 731 The index \ippdbcolumn{objID} (and \ippdbcolumn{diffObjID} for difference 660 732 tables) is derived from right ascension and declination. While it is 661 possible to calculate the R Aand Dec from the \ippdbcolumn{objID}, this is733 possible to calculate the R.A. and Dec from the \ippdbcolumn{objID}, this is 662 734 not recommended. The \ippdbcolumn{objID} value is determined when an object 663 735 is initially instantiated in the DVO database, and is based on the … … 903 975 detection. These bits include information specific to difference 904 976 imaging, as well as quality issues such as if source is near 905 diffraction spikes, star core, affected by the ` burntool' analysis of977 diffraction spikes, star core, affected by the ``burntool'' analysis of 906 978 persistence features (see Paper III), along with other analysis 907 979 issues. See also Paper IV. … … 972 1044 DR2 version of the database, the astrometry was recalibrated against 973 1045 Gaia DR1; the coordinates reported in the \ippdbtable{ObjectThin} table should be 974 used as the best R Aand Dec. Use \ippdbcolumn{objID} to join to most1046 used as the best R.A. and Dec. Use \ippdbcolumn{objID} to join to most 975 1047 tables. 976 1048 … … 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. 985 1057 986 \subsubsection{Tables based on the ` camera' stage of IPP}1058 \subsubsection{Tables based on the ``camera'' stage of IPP} 987 1059 \label{sec:schemap2} 988 1060 989 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 Aand 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.990 991 \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.1061 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. 1062 1063 \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. 992 1064 993 1065 \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. 998 1070 999 \subsubsection{Tables based on the ` stack' stage of IPP}1071 \subsubsection{Tables based on the ``stack'' stage of IPP} 1000 1072 \label{sec:schemast} 1001 1073 … … 1021 1093 independent. Only one set of such measurements should be used for 1022 1094 valid population statistics. To aid in such analysis, we define a 1023 ` primary' detection for all stack measurements (from a single filter)1024 of the same astronomical object. The ` primary' detection is that1095 ``primary'' detection for all stack measurements (from a single filter) 1096 of the same astronomical object. The ``primary'' detection is that 1025 1097 detection for which the stack pixels are closest to the center of the 1026 1098 skycell. Since the definition is purely geometric, in theory no … … 1029 1101 split a source into multiple detections within the image. For the 1030 1102 primary skycells, these detections will each be identified as 1031 ` primary', though they come from the same astrophysical object.1103 ``primary'', though they come from the same astrophysical object. 1032 1104 However, this is due to the analysis process, not the overlap of the 1033 1105 stack boundaries. … … 1039 1111 object. Users who prefer a high-quality measurement of a particular 1040 1112 object may choose to use these secondary measurements rather than the 1041 primary. We attempt to identify the ` best' stack measurement for each1113 primary. We attempt to identify the ``best'' stack measurement for each 1042 1114 filter by examining the signal-to-noise of the measurements and the 1043 1115 {\tt PSF\_QF\_PERFECT} values, a measurement of the masked-fraction … … 1058 1130 STACK\_PRIMARY} bit set in the \ipptable{StackObjectThin.XinfoFlag3} 1059 1131 field for the appropriate filter while stack measurements which are 1060 identified as the ` best' measurement for an object within a given1132 identified as the ``best'' measurement for an object within a given 1061 1133 filter have the {\tt STACK\_PHOT\_SRC} bit set in the same field (see 1062 1134 Tables~\ref{table:detectionflags3} and \ref{table:StackObjectThin}). … … 1067 1139 %% (this field is identical for all filters). 1068 1140 1069 If all of the ` best' measurements for a stack object (across all 51141 If all of the ``best'' measurements for a stack object (across all 5 1070 1142 filters) are also primary measurements, then the {\tt BEST\_STACK} bit 1071 1143 is set in the \ipptable{ObjectThin.objInfoFlag} entry for the … … 1074 1146 1075 1147 Several bits in the \ipptable{StackObjectThin.XinfoFlag4} field for 1076 each filter may be set based on the ` primary' and `best' detections1148 each filter may be set based on the ``primary'' and ``best'' detections 1077 1149 (see Tables~\ref{table:detectionflags3} and 1078 \ref{table:StackObjectThin}). If a ` primary' measurement exists for a1150 \ref{table:StackObjectThin}). If a ``primary'' measurement exists for a 1079 1151 given filter, then the {\tt SECF\_STACK\_PRIMARY} bit is set for that 1080 1152 filter. If multiple primary stack measurements exist for a given 1081 1153 filter, then the {\tt SECF\_STACK\_PRIMARY\_MULTIPLE} bit is also set for 1082 that filter (not set in DR1). If the ` best' measurement for a filter1154 that filter (not set in DR1). If the ``best'' measurement for a filter 1083 1155 is a significant detection (not forced from another band), then the 1084 {\tt SECF\_STACK\_BESTDET} bit is set. If any of the ` primary' measurements1156 {\tt SECF\_STACK\_BESTDET} bit is set. If any of the ``primary'' measurements 1085 1157 for a filter is a significant detection (not forced from another 1086 1158 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 1107 1179 object represents the primary detection. In addition, a detection is 1108 flagged as ` best' if it is a primary detection with a \ippdbcolumn{psfQf}1180 flagged as ``best'' if it is a primary detection with a \ippdbcolumn{psfQf} 1109 1181 value greater than 0.98; if that condition is not met, then the 1110 1182 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. 1164 1236 1165 \subsubsection{Tables from the ` forced photometry' stage of IPP}1237 \subsubsection{Tables from the ``forced photometry'' stage of IPP} 1166 1238 \label{sec:schemafw} 1167 1239 … … 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. 1186 1258 1187 \parheading{ForcedGalaxyShape} Contains the extended source galaxy shape parameters. The positions, magnitudes, fluxes, and Sersicindices 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.1259 \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. 1188 1260 1189 1261 \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} 1204 1276 1205 \subsubsection{Tables based on the ` diff' stage of IPP}1277 \subsubsection{Tables based on the ``diff'' stage of IPP} 1206 1278 \label{sec:schemadiff} 1207 1279 … … 1228 1300 PSPS Table & \multicolumn{2}{c}{column names} & comments \\ 1229 1301 \hline 1230 FrameMeta & raBore & decBore & R A/Dec of telescope boresite \\1302 FrameMeta & raBore & decBore & R.A./Dec of telescope boresite \\ 1231 1303 %- where the telescope was pointed when image was taken \\ 1232 ObjectThin & raMean & decMean & mean R Aand Dec from single exposure, calibrated against 2MASS \\1233 ObjectThin & raStack & decStack & mean R Aand Dec calculated from \ippstage{stack} skycells \\1234 Detection & R A & Dec & RAand Dec for single exposure detections \\1235 StackObjectThin & (grizy)ra & (grizy)dec & R Aand Dec calculated from individual \ippstage{stack} skycells \\1236 DiffDetection & R A & Dec & RAand Dec for single \ippstage{diff} exposure detections \\1237 DiffDetObject & R A& Dec & similar to raMean/decMean, calculated for \ippstage{diff} objects \\1238 GaiaFrameCoordinate & R A & Dec & \textbf{Best RAand Dec, recalibrated to Gaia (DR1 only).}\\%\tablenotemark{a} \\1304 ObjectThin & raMean & decMean & mean R.A. and Dec from single exposure, calibrated against 2MASS \\ 1305 ObjectThin & raStack & decStack & mean R.A. and Dec calculated from \ippstage{stack} skycells \\ 1306 Detection & R.A. & Dec & R.A. and Dec for single exposure detections \\ 1307 StackObjectThin & (grizy)ra & (grizy)dec & R.A. and Dec calculated from individual \ippstage{stack} skycells \\ 1308 DiffDetection & R.A. & Dec & R.A. and Dec for single \ippstage{diff} exposure detections \\ 1309 DiffDetObject & R.A. & Dec & similar to raMean/decMean, calculated for \ippstage{diff} objects \\ 1310 GaiaFrameCoordinate & R.A. & Dec & \textbf{Best R.A. and Dec, recalibrated to Gaia (DR1 only).}\\%\tablenotemark{a} \\ 1239 1311 \hline 1240 1312 \end{tabular} 1241 1313 \end{center} 1242 %\tablenotetext{a}{This is the best and most accurate R Aand Dec to use if interested in the static sky.}1314 %\tablenotetext{a}{This is the best and most accurate R.A. and Dec to use if interested in the static sky.} 1243 1315 \label{table:radec} 1244 1316 \end{table*} 1245 1317 1246 1318 1247 \subsection{Which R Aand Dec to use?}1319 \subsection{Which R.A. and Dec to use?} 1248 1320 \label{sec:schemaradec} 1249 1321 … … 1255 1327 proper motion or moving objects, it is best to use coordinates from 1256 1328 \ippdbtable{GaiaFrameCoordinate} if using DR1, as this is the weighted mean 1257 R Aand Dec (similar to \ippdbtable{ObjectThin}), but tied to the Gaia system.1329 R.A. and Dec (similar to \ippdbtable{ObjectThin}), but tied to the Gaia system. 1258 1330 This information is in a separate table and not part of \ippdbtable{ObjectThin} because the mean properties were calculated and ingested 1259 1331 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 1277 1349 designed to be used to join tables together. Generally, if a column 1278 name ends in ``\ippdbcolumn{ID} ", it is designed to be joined to other1350 name ends in ``\ippdbcolumn{ID}'', it is designed to be joined to other 1279 1351 tables, either to system metadata tables (examples include 1280 1352 \ippdbcolumn{filterID}, \ippdbcolumn{surveyID}, \ippdbcolumn{ccdID}), or to … … 1301 1373 different sources or objects have an index, called \ippdbcolumn{objID}. 1302 1374 \ippdbcolumn{objID} is only unique for the object type of tables, and is 1303 loosely based on R Aand Dec, see Section~\ref{sec:schemaobjid} for1375 loosely based on R.A. and Dec, see Section~\ref{sec:schemaobjid} for 1304 1376 more information. It is possible to use the \ippdbcolumn{objID} to get a 1305 rough estimate of the R Aand Dec, but this should not be used for the1306 definitive R A and Dec. Use \ippdbtable{ObjectThin} to get the RAand Dec1377 rough estimate of the R.A. and Dec, but this should not be used for the 1378 definitive R.A. and Dec. Use \ippdbtable{ObjectThin} to get the R.A. and Dec 1307 1379 calibrated to 2MASS, and use \ippdbtable{GaiaFrameCoordinate}(for DR1) or 1308 \ippdbtable{ObjectThin}(for DR2)to get the R Aand Dec calibrated to Gaia1380 \ippdbtable{ObjectThin}(for DR2)to get the R.A. and Dec calibrated to Gaia 1309 1381 astrometry. When available and possible, if joining 2 tables and they 1310 1382 both have the same column name like \ippdbcolumn{uniquePspsXXId}, join … … 1364 1436 \label{sec:schemanulls} 1365 1437 1366 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. 1367 1438 % https://skyserver.sdss.org/edr/en/sdss/skyserver is OK (2020.08.13) 1439 1440 The PSPS uses \texttt{-999} to denote \texttt{NULL} values, as PSPS is 1441 based off of CasJobs which also does not use NULL. The justification 1442 for this is explained by \cite{Szalay2002}: 1443 % at the following url: \url{https://skyserver.sdss.org/edr/en/sdss/skyserver/}. 1444 % Specifically, they state 1445 ``We also insist that all fields are non-null. These 1446 integrity constraints are invaluable tools in detecting errors during 1447 loading and they aid tools that automatically navigate the database'' 1448 \citep[see also][]{Gray2002}. 1449 Since our own database design has in its roots many of the same 1450 parts as the SDSS database, we also adopt this convention of non-null 1451 fields. 1452 1453 % the Szalay et al (2001) reference above is a technical report only on the SDSS. There is a possibly-related publication in : 1454 % https://www.springer.com/gp/book/9783540424680 1455 1456 % Szalay, A. S., Gray, J., Kunszt, P., Thakar, A., & Slutz, D. 2001, in Mining 1457 % the Sky, ed. A. J. Banday, S. Zaroubi, & M. Bartelmann (Berlin: 1458 % Springer), 99 1459 1460 % the paper itself is on arxiv: 1461 % https://arxiv.org/abs/cs/0202013 1368 1462 1369 1463 %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. 1417 1511 1418 \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.1512 \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. 1419 1513 1420 1514 \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} 1432 1526 1433 % {\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 DR1.1527 % {\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. 1434 1528 1435 1529 % {\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 1463 1557 revealed some problems for data in the vicinity of the celestial north 1464 pole. This issue sis described in some detail in Paper IV. In short,1558 pole. This issue is described in some detail in Paper IV. In short, 1465 1559 the on-the-fly astrometric calibration performed during the PV3 1466 1560 analysis (Section~\ref{sec:chipandcamera}) relied on an astrometric … … 1483 1577 the affected images are set to {\tt NULL} as these values cannot 1484 1578 be trusted. A list of the affected skycells is provided at MAST and 1485 users are advised to be cautious of measurements from these regions. 1579 users are advised to be cautious of measurements from these regions. 1580 % 1581 \textadd{The problem skycells are almost entirely north of Dec = 1582 80\degrees, comprising roughly 21 of the 313 square degrees 1583 in this region.} 1584 % 1486 1585 A reprocessing of the polar regions north of Dec = 70\degrees\ is 1487 underway (Nov 2019)and will be released to users in the future.1586 underway and will be released to users in the future. 1488 1587 1489 1588 %{\color{red} The diff DVO database } … … 1599 1698 \section{Conclusion} 1600 1699 \label{sec:conclusion} 1601 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 âOumuamua, 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. 1700 The Pan-STARRS database contains 10,723,304,629 objects. It is the 1701 largest data release from the largest digital sky survey to date, 1702 distilling the information from 1.6 petabytes of images and tables 1703 into a form that is accessible to the astronomical community through 1704 MAST. Nevertheless, sifting through such a large database can prove 1705 daunting, and this work is intended to describe the primary tables and 1706 quantities within the database, together with example queries. Data 1707 from Pan-STARRS has been used for myriad purposes including detecting 1708 moving objects within the solar system (and in the case of 1I/2017 U1 (âOumuamua), 1709 from outside it!), the analysis of tens of thousands of high-energy 1710 transient events, mapping the 3D structure of dust within our Galaxy, 1711 and studies of the large scale structure of our Universe. Yet these 1712 only scratch the surface, and it is likely that mining the database 1713 will lead to discoveries that were missed and correlations that were 1714 overlooked. As we enter the era of multi-messenger astrophysics, the 1715 Pan-STARRS data products will be essential to identifying the host 1716 galaxies and electromagnetic counterparts of events detected by 1717 gravitational wave, high-energy particle, neutrino and radio 1718 observatories. While we have provided various tools to work with this 1719 data release, we anticipate that it will spur the development of new 1720 interfaces and ways of working with high-dimensional datasets. This 1721 work will be critical to science with future surveys such as 1722 LSST. Combining this Pan-STARRS data release with other large catalogs 1723 such as \emph{GALEX}, 2MASS and \emph{Gaia} will provide a rich, 1724 high-dimensional dataset that will enable new scientific studies, and 1725 may yield astronomical treasures that we have not even begun to 1726 imagine. 1602 1727 1603 1728 {\color{red} } … … 1610 1735 The Pan-STARRS1 Surveys (PS1) have been made possible through 1611 1736 contributions of the Institute for Astronomy, the University of 1612 Hawai i, the Pan-STARRS Project Office, the Max-Planck Society and its1737 Hawai`i, the Pan-STARRS Project Office, the Max-Planck Society and its 1613 1738 participating institutes, the Max Planck Institute for Astronomy, 1614 1739 Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, … … 1625 1750 and Betty Moore foundation. 1626 1751 1752 % http://www.cosmos.esa.int/gaia : OK 1753 % http://www.cosmos.esa.int/web/gaia/dpac/consortium : OK 1754 1627 1755 This work has made use of data from the European Space Agency (ESA) 1628 1756 mission {\em Gaia} (\url{http://www.cosmos.esa.int/gaia}), processed by … … 1636 1764 \bibliographystyle{apj} 1637 1765 \bibliography{dataproducts}{} 1638 % \input{dataproducts.bbl}1766 % \input{dataproducts.bbl} 1639 1767 1640 1768 \appendix … … 1647 1775 \label{sec:query} 1648 1776 1649 This section shows example queries for the \PS\ database. The1777 This section shows example queries for the \PS\ DR2 database. The 1650 1778 progression will be from simple queries to more complicated queries. 1651 1779 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 1654 1782 database schema. The queries given below may all be run from the 1655 CasJobs tab on the MAST web site. Note the some of the later queries 1656 rely on myDB tables generated in the earlier queries. 1783 CasJobs tab on the MAST web site \textadd{using the context 1784 ``PanSTARRS\_DR2''.} Note the some of the later queries rely on 1785 myDB tables generated in the earlier queries. \textadd{The names for 1786 these output tables are surrounded by square brackets in the 1787 examples. These brackets are always allowed, but are {\em required} if 1788 the table name includes spaces or reserved 1789 words\footnote{\url{https://docs.microsoft.com/en-us/sql/relational-databases/databases/database-identifiers}} 1790 Also beware that cut-and-paste in some browsers can convert the 1791 underscore characters to space.} 1657 1792 1658 1793 %\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} 1662 1797 1663 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. 1798 This is an example of a simple query, it needs to be run in the slow 1799 queue. The difference between \texttt{COUNT\_BIG()} and 1800 \texttt{COUNT()} is that \texttt{COUNT\_BIG()} returns a 1801 \texttt{BIGINT}, while \texttt{COUNT()} returns an \texttt{INT}. The 1802 PSPS tables are so large that \texttt{COUNT()}, which goes up to 2.14 1803 billion, is too small of a number. Users should choose the method of 1804 counting rows that is appropriate for their data ranges. Unless it 1805 involves large tables and large areas of sky, \texttt{COUNT()} is 1806 recommended. \textadd{However, if the result is too large, using 1807 \texttt{COUNT()} will result in an aritmetic overflow exception.} 1664 1808 1665 1809 %% careful with these: underscores from PDFs convert to spaces when copy-paste-ing … … 1686 1830 AND decMean < 0.1 \\ 1687 1831 } 1688 % EAM : 2019.11.08 : OK, I get 386 7objects against DR21689 1690 This returns 386 7objects. The majority of these objects have only been detected once.1832 % EAM : 2019.11.08 : OK, I get 3868 objects against DR2 1833 1834 This returns 3868 objects. The majority of these objects have only been detected once. 1691 1835 1692 1836 \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 1695 1839 to make queries on your MyDB. Do the query from above, but save it to 1696 your MyDB as 'MyDBtest'. Run the following query on your MyDB to make1697 a histogram of \ippdbcolumn{nDetections}.1840 your MyDB as 'MyDBtest'. Run the following query on your MyDB (MyDB 1841 context) to make a histogram of \ippdbcolumn{nDetections}. 1698 1842 1699 1843 %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 1736 1880 } 1737 % EAM : 2019.11.08 : OK, I get 74 7objects from DR21738 1739 This returns 74 7objects, a significant reduction from the 3867 returned in query \# 2.1881 % EAM : 2019.11.08 : OK, I get 748 objects from DR2 1882 1883 This returns 748 objects, a significant reduction from the 3867 returned in query \# 2. 1740 1884 1741 1885 \item \textbf{Select \ippstage{stack} PSF magnitudes for all filters for a rectangular patch of sky} … … 1754 1898 AND decMean < 0.1 \\ 1755 1899 } 1756 % EAM : 2019.11.08 : OK, I get 180 5objects from DR21757 1758 This returns 180 5objects.1900 % EAM : 2019.11.08 : OK, I get 1806 objects from DR2 1901 1902 This returns 1806 objects. 1759 1903 1760 1904 \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} 1778 1922 1779 Similar to query \# 5, except uses \texttt{BETWEEN} to limit RA and Dec ranges as well as iPSFMag ranges. 1923 Similar to query \# 5, except uses \texttt{BETWEEN} to limit R.A. and 1924 Dec ranges as well as iPSFMag ranges. 1780 1925 1781 1926 % QUERY 07 … … 1794 1939 \item \textbf{Using built-in functions to do a box search} 1795 1940 1796 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. 1941 ObjectThin contains Hierarchical triangular mesh information, making 1942 it possible to use the built in function dbo.fGetObjFromRectEq(minra, 1943 mindec, maxra, maxdec) to do a rectangular search. Tables which have 1944 htm, cx,cy, cz can use this built in function. 1797 1945 1798 1946 % QUERY 08 … … 1808 1956 \item \textbf{Using built in functions to do a cone search} 1809 1957 1810 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. 1958 ObjectThin contains Hierarchical triangular mesh information, making 1959 it possible to use the built in function dbo.fGetNearbyObjEq(ra, dec, 1960 conesize(arcmin)) to do a radial search for objects near a given ra and 1961 dec (cone search). Tables which have htm, cx,cy, cz can use this built 1962 in function. \textadd{The query below returns the objects within 0.2 arcmin of 1963 the coordinate 56.85, 24.12. Note that only one of these objects was 1964 detected in a \gps-band image and thus has a valid value for the \gps-magnitude.} 1811 1965 1812 1966 % QUERY 09 … … 1818 1972 ON o.objID = n.objID 1819 1973 } 1820 % EAM : 2019.11.10 : OK, I get 4 0objects from DR21974 % EAM : 2019.11.10 : OK, I get 41 objects from DR2 1821 1975 1822 1976 \item \textbf{Cone search of high fidelity stellar-like objects} 1823 1977 1824 We want to get all objects with R degrees of a given position that are high fidelity stellar-like objects. 1825 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. 1978 We want to get all objects with R degrees of a given position that are 1979 high fidelity stellar-like objects. We get all objects within 0.2 1980 degrees of R.A.=334.0 and Dec=0.0 which have mean magnitudes in griz 1981 (i.e. at least 1 detection in each band that can be used for the mean 1982 mag). In addition, we require QfPerfect $> 0.85$ in all bands. We 1983 select stars with small ($<0.05$) difference between Kron and PSF 1984 magnitudes. 1826 1985 1827 1986 % QUERY 10 … … 1894 2053 1895 2054 Star CSS J030521.9+013231 (Catalina Sky Survey), 584630948352256 1896 (GAIA) is an RR Lyrae with period = 0.55547 days and coordinates R A=2055 (GAIA) is an RR Lyrae with period = 0.55547 days and coordinates R.A. = 1897 2056 46.341468915923 and DEC = 1.54199810825252 (ref. GAIA DR2, 1898 2057 2018yCat.1345....0G). In the following, we obtain the PSF and aperture … … 1907 2066 ra AS RA\_GAIA, dec AS DEC\_GAIA, 1908 2067 phot\_g\_mean\_mag AS Gmag 1909 INTO mydb. RRL\_5846309483522562068 INTO mydb.[RRL\_584630948352256] 1910 2069 FROM gaia\_source 1911 2070 WHERE source\_id = 584630948352256 … … 2048 2207 %} 2049 2208 2050 %\item extracting a light curve for an object by R Aand Dec using the Detection table (DR2)2051 2052 %If the \ippdbcolumn{objID} of the object is not know, it is necessary to do a join on \ippdbtable{ObjectThin} to search by R Aand Dec. This method is much slower than to search by the \ippdbcolumn{objID}.2209 %\item extracting a light curve for an object by R.A. and Dec using the Detection table (DR2) 2210 2211 %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}. 2053 2212 2054 2213 %\item extracting a light curve for an object with a known \ippdbcolumn{objID} using the \ippdbtable{ForcedWarpMeasurement} table(DR2) 2055 2214 2056 %\item extracting a light curve for an object by R Aand Dec using the \ippdbtable{ForcedWarpMeasurement} table (DR2)2215 %\item extracting a light curve for an object by R.A. and Dec using the \ippdbtable{ForcedWarpMeasurement} table (DR2) 2057 2216 2058 2217 %\item extracting a light curve for an object with a known \ippdbcolumn{objID} using the \ippdbtable{DiffDetection} table(DR2) 2059 2218 2060 %\item extracting a light curve for an object by R Aand Dec using the \ippdbtable{DiffDetection} table (DR2)2219 %\item extracting a light curve for an object by R.A. and Dec using the \ippdbtable{DiffDetection} table (DR2) 2061 2220 2062 2221 \end{enumerate} … … 2175 2334 %% \note{table order is a bit funny; compare with text} 2176 2335 2177 \begin{table}[ b]2336 \begin{table}[htb] 2178 2337 \caption{ObjectInfoFlags} 2179 2338 \begin{center} … … 2227 2386 2228 2387 % \FloatBarrier 2229 \begin{table}[ b]2388 \begin{table}[htb] 2230 2389 \caption{ObjectQualityFlags} 2231 2390 \begin{center} … … 2252 2411 \end{table}% 2253 2412 2254 \begin{table}[ b]2413 \begin{table}[htb] 2255 2414 \caption{ObjectFilterFlags} 2256 2415 \begin{center} … … 2290 2449 \end{table}% 2291 2450 2292 \begin{table}[ b]2451 \begin{table}[htb] 2293 2452 \caption{ImageFlags} 2294 2453 \begin{center} … … 2317 2476 \end{table}% 2318 2477 2319 \begin{table}[ b]2478 \begin{table}[htb] 2320 2479 \caption{ForcedGalaxyShapeFlags} 2321 2480 \begin{center} … … 2337 2496 \end{table}% 2338 2497 2339 \begin{table}[ b]2498 \begin{table}[htb] 2340 2499 \caption{DetectionFlags} 2341 2500 \begin{center} … … 2385 2544 \end{table}% 2386 2545 2387 \begin{table}[ b]2546 \begin{table}[htb] 2388 2547 \caption{DetectionFlags2} 2389 2548 \begin{center} … … 2425 2584 \end{table}% 2426 2585 2427 \begin{table}[ b]2586 \begin{table}[htb] 2428 2587 \caption{DetectionFlags3} 2429 2588 \begin{center} … … 2721 2880 %{\color{red} needs to be added} 2722 2881 2882 In this section, we present the contents of all DR2 tables, along with 2883 the expected \ippstage{diff} tables for DR3. These listings were 2884 automatically generated from the XML code used to define the PSPS 2885 tables, with light editing to clean up the formatting for some of the 2886 units and equations. 2887 2723 2888 \subsection{Object / Mean Object Tables} 2724 2889 2725 \begin{table}[ b]2890 \begin{table}[htb] 2726 2891 2727 2892 \caption{ObjectThin: Contains the positional information for objects … … 2804 2969 \end{table}% 2805 2970 2806 \begin{table}[ b]2971 \begin{table}[htb] 2807 2972 \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.} 2808 2973 \begin{center} … … 2853 3018 %\end{document} 2854 3019 2855 \begin{table}[ b]3020 \begin{table}[htb] 2856 3021 \caption{GaiaFrameCoordinate: PSPS objects calibrated against Gaia astrometry} 2857 3022 \begin{center} … … 2883 3048 \subsection{Single Exposure Detection Tables} 2884 3049 2885 \begin{table}[ b]2886 \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.}3050 \begin{table}[htb] 3051 \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.} 2887 3052 \begin{center} 2888 3053 \resizebox{\textwidth}{!}{% … … 2914 3079 raBore & degrees & FLOAT & -999 &Right ascension of telescope boresight.\\ 2915 3080 decBore & degrees & FLOAT & -999 &Declination of telescope boresight.\\ 2916 ctype1 & - & VARCHAR(100) & &Name of astrometric projection in R A.\\3081 ctype1 & - & VARCHAR(100) & &Name of astrometric projection in R.A..\\ 2917 3082 ctype2 & - & VARCHAR(100) & &Name of astrometric projection in Dec.\\ 2918 3083 crval1 & degrees & FLOAT & -999 &Right ascension corresponding to reference pixel.\\ 2919 3084 crval2 & degrees & FLOAT & -999 &Declination corresponding to reference pixel.\\ 2920 crpix1 & pixels & FLOAT & -999 &Reference pixel for R A.\\3085 crpix1 & pixels & FLOAT & -999 &Reference pixel for R.A..\\ 2921 3086 crpix2 & pixels & FLOAT & -999 &Reference pixel for Dec.\\ 2922 cdelt1 & degrees/pixel & FLOAT & -999 &Pixel scale in R A.\\3087 cdelt1 & degrees/pixel & FLOAT & -999 &Pixel scale in R.A..\\ 2923 3088 cdelt2 & degrees/pixel & FLOAT & -999 &Pixel scale in Dec.\\ 2924 pc001001 & - & FLOAT & -999 &Linear transformation matrix element between focal plane pixel L and R A.\\2925 pc001002 & - & FLOAT & -999 &Linear transformation matrix element between focal plane pixel M and R A.\\3089 pc001001 & - & FLOAT & -999 &Linear transformation matrix element between focal plane pixel L and R.A..\\ 3090 pc001002 & - & FLOAT & -999 &Linear transformation matrix element between focal plane pixel M and R.A..\\ 2926 3091 pc002001 & - & FLOAT & -999 &Linear transformation matrix element between focal plane pixel L and Dec.\\ 2927 3092 pc002002 & - & FLOAT & -999 &Linear transformation matrix element between focal plane pixel M and Dec.\\ 2928 3093 polyOrder & - & TINYINT & 255 &Polynomial order of astrometric fit between detector focal plane and sky.\\ 2929 pca1x3y0 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^3$ $y^0$) for R A.\\2930 pca1x2y1 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^2$ $y^1$) for R A.\\2931 pca1x1y2 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^1$ $y^2$) for R A.\\2932 pca1x0y3 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^0$ $y^3$) for R A.\\2933 pca1x2y0 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^2$ $y^0$) for R A.\\2934 pca1x1y1 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^1$ $y^1$) for R A.\\2935 pca1x0y2 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^0$ $y^2$) for R A.\\3094 pca1x3y0 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^3$ $y^0$) for R.A..\\ 3095 pca1x2y1 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^2$ $y^1$) for R.A..\\ 3096 pca1x1y2 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^1$ $y^2$) for R.A..\\ 3097 pca1x0y3 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^0$ $y^3$) for R.A..\\ 3098 pca1x2y0 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^2$ $y^0$) for R.A..\\ 3099 pca1x1y1 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^1$ $y^1$) for R.A..\\ 3100 pca1x0y2 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^0$ $y^2$) for R.A..\\ 2936 3101 pca2x3y0 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^3$ $y^0$) for Dec.\\ 2937 3102 pca2x2y1 & - & FLOAT & -999 &Polynomial coefficient for the astrometric fit component ($x^2$ $y^1$) for Dec.\\ … … 2949 3114 \end{table}% 2950 3115 2951 \begin{table}[ b]3116 \begin{table}[htb] 2952 3117 \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.} 2953 3118 \begin{center} %cheaing here, if I do resizebox it compiles … … 2958 3123 column name & units & data type & default & description\\ 2959 3124 \hline 2960 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 *frameID + ccdID).\\3125 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 $\times$ frameID + ccdID).\\ 2961 3126 frameID & - & INT & NA &Unique frame/exposure identifier.\\ 2962 3127 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.\\ 2966 3131 biasScat & adu & REAL & -999 &Scatter in bias level.\\ 2967 sky & $Jy/arcsec^2$ & REAL & -999 &Mean sky brightness.\\2968 skyScat & $Jy/arcsec^2$ & REAL & -999 &Scatter in mean sky brightness.\\3132 sky & Jy arcsec$^{-2}$ & REAL & -999 &Mean sky brightness.\\ 3133 skyScat & Jy arcsec$^{-2}$ & REAL & -999 &Scatter in mean sky brightness.\\ 2969 3134 nDetect & - & INT & -999 &Number of detections in this image.\\ 2970 3135 detectionThreshold & magnitudes & REAL & -999 &Reference magnitude for detection efficiency calculation.\\ … … 2988 3153 momentMajor & arcsec & REAL & -999 &PSF major axis second moment.\\ 2989 3154 momentMinor & arcsec & REAL & -999 &PSF minor axis second moment.\\ 2990 momentM2C & $arcsec^2$ & REAL & -999 &Moment $M2C = M_{xx} - M_{yy}$.\\2991 momentM2S & $arcsec^2$ & REAL & -999 &Moment $M2S = 2 *M_{xy}$.\\2992 momentM3 & $arcsec^2$ & REAL & -999 &trefoil second moment = $sqrt( (M_{xxx} - 3 * M_{xyy})^2 + (3 * M_{xxy} - M_{yyy})^2 )$.\\2993 momentM4 & $arcsec^2$ & REAL & -999 &quadrupole second moment = $sqrt( (M_{xxxx} - 6 * M_{xxyy} + M_{yyyy})^2 + (4 * M_{xxxy} - 4 * M_{xyyy})^2 )$.\\3155 momentM2C & arcsec$^2$ & REAL & -999 &Moment $M2C = M_{xx} - M_{yy}$.\\ 3156 momentM2S & arcsec$^2$ & REAL & -999 &Moment $M2S = 2 M_{xy}$.\\ 3157 momentM3 & arcsec$^2$ & REAL & -999 &trefoil second moment = $\sqrt{(M_{xxx} - 3 M_{xyy})^2 + (3 M_{xxy} - M_{yyy})^2}$.\\ 3158 momentM4 & arcsec$^2$ & REAL & -999 &quadrupole second moment = $\sqrt{(M_{xxxx} - 6 M_{xxyy} + M_{yyyy})^2 + (4 M_{xxxy} - 4 M_{xyyy})^2}$.\\ 2994 3159 apResid & magnitudes & REAL & -999 &Residual of aperture corrections.\\ 2995 3160 dapResid & magnitudes & REAL & -999 &Scatter of aperture corrections.\\ … … 3043 3208 3044 3209 3045 \begin{table}[ b]3210 \begin{table}[htb] 3046 3211 \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.} 3047 3212 \begin{center} … … 3059 3224 filterID & - & TINYINT & NA &Filter identifier. Details in the Filter table.\\ 3060 3225 surveyID & - & TINYINT & NA &Survey identifier. Details in the Survey table.\\ 3061 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 *frameID + ccdID).\\3226 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 $\times$ frameID + ccdID).\\ 3062 3227 randomDetID & - & FLOAT & NA &Random value drawn from the interval between zero and one. \\ 3063 3228 dvoRegionID & - & INT & -1 &Internal DVO region identifier.\\ … … 3093 3258 psfChiSq & - & REAL & -999 &Reduced chi squared value of the PSF model fit.\\ 3094 3259 psfLikelihood & - & REAL & -999 &Likelihood that this detection is best fit by a PSF.\\ 3095 momentXX & $arcsec^2$ & REAL & -999 &Second moment $M_{xx}$.\\3096 momentXY & $arcsec^2$ & REAL & -999 &Second moment $M_{xy}$.\\3097 momentYY & $arcsec^2$ & REAL & -999 &Second moment $M_{yy}$.\\3260 momentXX & arcsec$^2$ & REAL & -999 &Second moment $M_{xx}$.\\ 3261 momentXY & arcsec$^2$ & REAL & -999 &Second moment $M_{xy}$.\\ 3262 momentYY & arcsec$^2$ & REAL & -999 &Second moment $M_{yy}$.\\ 3098 3263 momentR1 & arcsec & REAL & -999 &First radial moment.\\ 3099 momentRH & $arcsec^{0.5}$ & REAL & -999 &Half radial moment ($r^{0.5}$ weighting).\\3100 momentM3C & $arcsec^2$ & REAL & -999 &Cosine of trefoil second moment term: $r^2 cos(3 theta) = M_{xxx} - 3 *M_{xyy}$.\\3101 momentM3S & $arcsec^2$ & REAL & -999 &Sine of trefoil second moment: $r^2 sin (3 theta) = 3 *M_{xxy} - M_{yyy}$.\\3102 momentM4C & $arcsec^2$ & REAL & -999 &Cosine of quadrupole second moment: $r^2 cos (4 theta) = M_{xxxx} - 6 *M_{xxyy} + M_{yyyy}.$\\3103 momentM4S & $arcsec^2$ & REAL & -999 &Sine of quadrupole second moment: $r^2 sin (4 theta) = 4 * M_{xxxy} - 4 *M_{xyyy}$.\\3264 momentRH & arcsec$^{0.5}$ & REAL & -999 &Half radial moment ($r^{0.5}$ weighting).\\ 3265 momentM3C & arcsec$^2$ & REAL & -999 &Cosine of trefoil second moment term: $r^2 \cos(3 \theta) = M_{xxx} - 3 M_{xyy}$.\\ 3266 momentM3S & arcsec$^2$ & REAL & -999 &Sine of trefoil second moment: $r^2 \sin (3 \theta) = 3 M_{xxy} - M_{yyy}$.\\ 3267 momentM4C & arcsec$^2$ & REAL & -999 &Cosine of quadrupole second moment: $r^2 \cos (4 \theta) = M_{xxxx} - 6 M_{xxyy} + M_{yyyy}.$\\ 3268 momentM4S & arcsec$^2$ & REAL & -999 &Sine of quadrupole second moment: $r^2 \sin (4 \theta) = 4 M_{xxxy} - 4 M_{xyyy}$.\\ 3104 3269 apFlux & Jy & REAL & -999 &Flux in seeing-dependent aperture.\\ 3105 3270 apFluxErr & Jy & REAL & -999 &Error on flux in seeing-dependent aperture.\\ … … 3109 3274 kronFluxErr & Jy & REAL & -999 &Error on Kron (1980) flux.\\ 3110 3275 kronRad & arcsec & REAL & -999 &Kron (1980) radius.\\ 3111 sky & $Jy/arcsec^2$ & REAL & -999 &Background sky level.\\3112 skyErr & $Jy/arcsec^2$ & REAL & -999 &Error in background sky level.\\3276 sky & Jy arcsec$^{-2}$ & REAL & -999 &Background sky level.\\ 3277 skyErr & Jy arcsec$^{-2}$ & REAL & -999 &Error in background sky level.\\ 3113 3278 infoFlag & - & BIGINT & 0 &Information flag bitmask indicating details of the photometry. \\ 3114 3279 & & & & Values listed in DetectionFlags.\\ … … 3125 3290 3126 3291 3127 \begin{table}[ b]3292 \begin{table}[htb] 3128 3293 \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.} 3129 3294 \begin{center} … … 3134 3299 column name & units & data type & default & description\\ 3135 3300 \hline 3136 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 *frameID + ccdID).\\3301 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 $\times$ frameID + ccdID).\\ 3137 3302 frameID & - & INT & NA &Unique frame/exposure identifier.\\ 3138 3303 magref & magnitudes & REAL & NA &Detection efficiency reference magnitude.\\ … … 3169 3334 \subsection{Stack Tables} 3170 3335 3171 \begin{table}[ b]3336 \begin{table}[htb] 3172 3337 \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.} 3173 3338 \begin{center} … … 3239 3404 \end{table}% 3240 3405 3241 \begin{table}[ b]3406 \begin{table}[htb] 3242 3407 \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.} 3243 3408 \begin{center} … … 3296 3461 \end{table}% 3297 3462 3298 \begin{table}[ b]3463 \begin{table}[htb] 3299 3464 \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. 3300 3465 } … … 3329 3494 gpsfQfPerfect & - & REAL & -999 &PSF-weighted fraction of pixels totally unmasked for g filter \ippstage{stack} detection.\\ 3330 3495 gpsfChiSq & - & REAL & -999 &Reduced chi squared value of the PSF model fit for g filter \ippstage{stack} detection.\\ 3331 gmomentXX & $arcsec^2$ & REAL & -999 &Second moment $M_{xx}$ for g filter \ippstage{stack} detection.\\3332 gmomentXY & $arcsec^2$ & REAL & -999 &Second moment $M_{xy}$ for g filter \ippstage{stack} detection.\\3333 gmomentYY & $arcsec^2$ & REAL & -999 &Second moment $M_{yy}$ for g filter \ippstage{stack} detection.\\3496 gmomentXX & arcsec$^2$ & REAL & -999 &Second moment $M_{xx}$ for g filter \ippstage{stack} detection.\\ 3497 gmomentXY & arcsec$^2$ & REAL & -999 &Second moment $M_{xy}$ for g filter \ippstage{stack} detection.\\ 3498 gmomentYY & arcsec$^2$ & REAL & -999 &Second moment $M_{yy}$ for g filter \ippstage{stack} detection.\\ 3334 3499 gmomentR1 & arcsec & REAL & -999 &First radial moment for g filter \ippstage{stack} detection.\\ 3335 gmomentRH & $arcsec^{0.5}$ & REAL & -999 &Half radial moment ($r^{0.5}$ weighting) for g filter \ippstage{stack} detection.\\3500 gmomentRH & arcsec$^{0.5}$ & REAL & -999 &Half radial moment ($r^{0.5}$ weighting) for g filter \ippstage{stack} detection.\\ 3336 3501 gPSFFlux & Jy & REAL & -999 &PSF flux from g filter \ippstage{stack} detection.\\ 3337 3502 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 \\ 3349 3514 & & & & by the PSF magnitude uncertainty.\\ 3350 gsky & $Jy/arcsec^2$ & REAL & -999 &Residual background sky level at the g filter \ippstage{stack} detection.\\3351 gskyErr & $Jy/arcsec^2$ & REAL & -999 &Error in residual background sky level at the g filter \ippstage{stack} detection.\\3515 gsky & Jy arcsec$^{-2}$ & REAL & -999 &Residual background sky level at the g filter \ippstage{stack} detection.\\ 3516 gskyErr & Jy arcsec$^{-2}$ & REAL & -999 &Error in residual background sky level at the g filter \ippstage{stack} detection.\\ 3352 3517 gzp & magnitudes & REAL & 0 &Photometric zeropoint for the g filter stack. Necessary for converting\\ 3353 3518 & & & & listed fluxes and magnitudes back to measured ADU counts.\\ … … 3364 3529 \end{table}% 3365 3530 3366 \begin{table}[ b]3367 \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 (2.0arcsec). All filters are matched into a single row. See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.}3531 \begin{table}[htb] 3532 \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.} 3368 3533 \begin{center} 3369 3534 %\resizebox{\textwidth}{!}{% … … 3382 3547 gstackImageID & - & BIGINT & NA &Unique \ippstage{stack} identifier for g filter detection.\\ 3383 3548 gippDetectID & - & BIGINT & NA &IPP internal detection identifier.\\ 3384 gflxR5 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 3.00 3385 gflxR5Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 3.00 3386 gflxR5Std & Jy & REAL & -999 &Standard deviation of g filter flux within an aperture of radius r = 3.00 3387 gflxR5Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 3.00 3388 gflxR6 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 4.63 3389 gflxR6Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 4.63 3390 gflxR6Std & Jy & REAL & -999 &Standard deviation of g filter flux within an aperture of radius r = 4.63 3391 gflxR6Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 4.63 3392 gflxR7 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 7.43 3393 gflxR7Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 7.43 3394 gflxR7Std & Jy & REAL & -999 &Standard deviation of g filter flux within an aperture of radius r = 7.43 3395 gflxR7Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 7.43 3549 gflxR5 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 3.00\arcsec.\\ 3550 gflxR5Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 3.00\arcsec.\\ 3551 gflxR5Std & Jy & REAL & -999 &Standard deviation of g filter flux within an aperture of radius r = 3.00\arcsec.\\ 3552 gflxR5Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 3.00\arcsec.\\ 3553 gflxR6 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 4.63\arcsec.\\ 3554 gflxR6Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 4.63\arcsec.\\ 3555 gflxR6Std & Jy & REAL & -999 &Standard deviation of g filter flux within an aperture of radius r = 4.63\arcsec.\\ 3556 gflxR6Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 4.63\arcsec.\\ 3557 gflxR7 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 7.43\arcsec.\\ 3558 gflxR7Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 7.43\arcsec.\\ 3559 gflxR7Std & Jy & REAL & -999 &Standard deviation of g filter flux within an aperture of radius r = 7.43\arcsec.\\ 3560 gflxR7Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 7.43\arcsec.\\ 3396 3561 gc6flxR5 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels\\ 3397 & & & & (1.5 arcsec) within an aperture of radius r = 3.00arcsec.\\3562 & & & & (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\ 3398 3563 gc6flxR5Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of \\ 3399 & & & & 6 sky pixels (1.5 arcsec) within an aperture of radius r = 3.00arcsec.\\3564 & & & & 6 sky pixels (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\ 3400 3565 gc6flxR5Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to \\ 3401 & & & & a target of 6 sky pixels (1.5 arcsec) within an aperture of radius r = 3.00arcsec.\\3566 & & & & a target of 6 sky pixels (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\ 3402 3567 gc6flxR5Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a \\ 3403 & & & & target of 6 sky pixels (1.5 arcsec) within an aperture of radius r = 3.00arcsec.\\3568 & & & & target of 6 sky pixels (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\ 3404 3569 gc6flxR6 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels\\ 3405 & & & & (1.5 arcsec) within an aperture of radius r = 4.63arcsec.\\3570 & & & & (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\ 3406 3571 gc6flxR6Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of \\ 3407 & & & & 6 sky pixels (1.5 arcsec) within an aperture of radius r = 4.63arcsec.\\3572 & & & & 6 sky pixels (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\ 3408 3573 gc6flxR6Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to \\ 3409 & & & & a target of 6 sky pixels (1.5 arcsec) within an aperture of radius r = 4.63arcsec.\\3574 & & & & a target of 6 sky pixels (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\ 3410 3575 gc6flxR6Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of \\ 3411 & & & & 6 sky pixels (1.5 arcsec) within an aperture of radius r = 4.63arcsec.\\3576 & & & & 6 sky pixels (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\ 3412 3577 gc6flxR7 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels\\ 3413 & & & & (1.5 arcsec) within an aperture of radius r = 7.43arcsec.\\3578 & & & & (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\ 3414 3579 gc6flxR7Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of \\ 3415 & & & & 6 sky pixels (1.5 arcsec) within an aperture of radius r = 7.43arcsec.\\3580 & & & & 6 sky pixels (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\ 3416 3581 gc6flxR7Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of \\ 3417 & & & & 6 sky pixels (1.5 arcsec) within an aperture of radius r = 7.43arcsec.\\3582 & & & & 6 sky pixels (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\ 3418 3583 gc6flxR7Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 6 sky \\ 3419 & & & & pixels (1.5 arcsec) within an aperture of radius r = 7.43arcsec.\\3584 & & & & pixels (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\ 3420 3585 gc8flxR5 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 8 sky pixels\\ 3421 & & & & (2.0 arcsec) within an aperture of radius r = 3.00arcsec.\\3586 & & & & (2.0\arcsec) within an aperture of radius r = 3.00\arcsec.\\ 3422 3587 gc8flxR5Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 8 sky pixels \\ 3423 & & & & (2.0 arcsec) within an aperture of radius r = 3.00arcsec.\\3588 & & & & (2.0\arcsec) within an aperture of radius r = 3.00\arcsec.\\ 3424 3589 gc8flxR5Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 8 sky \\ 3425 & & & & pixels (2.0 arcsec) within an aperture of radius r = 3.00arcsec.\\3590 & & & & pixels (2.0\arcsec) within an aperture of radius r = 3.00\arcsec.\\ 3426 3591 gc8flxR5Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 8 sky \\ 3427 & & & & pixels (2.0 arcsec) within an aperture of radius r = 3.00arcsec.\\3592 & & & & pixels (2.0\arcsec) within an aperture of radius r = 3.00\arcsec.\\ 3428 3593 gc8flxR6 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 8 sky pixels\\ 3429 & & & & (2.0 arcsec) within an aperture of radius r = 4.63arcsec.\\3594 & & & & (2.0\arcsec) within an aperture of radius r = 4.63\arcsec.\\ 3430 3595 gc8flxR6Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 8 sky pixels\\ 3431 & & & & (2.0 arcsec) within an aperture of radius r = 4.63arcsec.\\3596 & & & & (2.0\arcsec) within an aperture of radius r = 4.63\arcsec.\\ 3432 3597 gc8flxR6Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of \\ 3433 & & & & 8 sky pixels (2.0 arcsec) within an aperture of radius r = 4.63arcsec.\\3598 & & & & 8 sky pixels (2.0\arcsec) within an aperture of radius r = 4.63\arcsec.\\ 3434 3599 gc8flxR6Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 8 sky pixels \\ 3435 & & & & (2.0 arcsec) within an aperture of radius r = 4.63arcsec.\\3436 gc8flxR7 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 8 sky pixels (2.0 3437 & & & & within an aperture of radius r = 7.43 3600 & & & & (2.0\arcsec) within an aperture of radius r = 4.63\arcsec.\\ 3601 gc8flxR7 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 8 sky pixels (2.0\arcsec) \\ 3602 & & & & within an aperture of radius r = 7.43\arcsec.\\ 3438 3603 gc8flxR7Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target 8 sky pixels \\ 3439 & & & & (2.0 arcsec) within an aperture of radius r = 7.43arcsec.\\3604 & & & & (2.0\arcsec) within an aperture of radius r = 7.43\arcsec.\\ 3440 3605 gc8flxR7Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of \\ 3441 & & & & 8 sky pixels (2.0 arcsec) within an aperture of radius r = 7.43arcsec.\\3606 & & & & 8 sky pixels (2.0\arcsec) within an aperture of radius r = 7.43\arcsec.\\ 3442 3607 gc8flxR7Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 8 sky pixels \\ 3443 & & & & (2.0 arcsec) within an aperture of radius r = 7.43arcsec.\\3608 & & & & (2.0\arcsec) within an aperture of radius r = 7.43\arcsec.\\ 3444 3609 rstackDetectID \\ 3445 3610 ... & & & & same entries repeated for r, i, z, and y filters \\ … … 3453 3618 3454 3619 %HAF commented out because stackmodelfitextra is junk: not in DR1 or DR2? 3455 %\begin{table}[ b]3620 %\begin{table}[htb] 3456 3621 %\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}} 3457 3622 %\begin{center} … … 3489 3654 %\end{table}% 3490 3655 3491 \begin{table}[ b]3656 \begin{table}[htb] 3492 3657 \caption{StackModelFitExp: Contains the exponential fit parameters to extended sources. See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections. } 3493 3658 \begin{center} … … 3600 3765 \end{table}% 3601 3766 3602 \begin{table}[ b]3767 \begin{table}[htb] 3603 3768 \caption{StackModelFitDeV: Contains the \citet{deVaucouleurs1948} fit parameters to extended sources. See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.} 3604 3769 \begin{center} … … 3709 3874 \end{table}% 3710 3875 3711 \begin{table}[ b]3876 \begin{table}[htb] 3712 3877 \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}.} 3713 3878 \begin{center} … … 3823 3988 \end{table}% 3824 3989 3825 \begin{table}[ b]3826 \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 = 44.21arcsec) 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. }3990 \begin{table}[htb] 3991 \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. } 3827 3992 \begin{center} 3828 3993 %\resizebox{\textwidth}{!}{% … … 3841 4006 gstackDetectID & - & BIGINT & NA &Unique \ippstage{stack} detection identifier.\\ 3842 4007 gstackImageID & - & BIGINT & NA &Unique \ippstage{stack} identifier for g filter detection.\\ 3843 gflxR3 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 1.03 3844 gflxR3Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 1.03 4008 gflxR3 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 1.03\arcsec.\\ 4009 gflxR3Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 1.03\arcsec.\\ 3845 4010 gflxR3Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection within an aperture of radius \\ 3846 & & & & r = 1.03 3847 gflxR3Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 1.03 3848 gflxR4 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 1.76 3849 gflxR4Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 1.76 4011 & & & & r = 1.03\arcsec.\\ 4012 gflxR3Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 1.03\arcsec.\\ 4013 gflxR4 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 1.76\arcsec.\\ 4014 gflxR4Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 1.76\arcsec.\\ 3850 4015 gflxR4Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection within an aperture of radius \\ 3851 & & & & r = 1.76 3852 gflxR4Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 1.76 3853 gflxR5 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 3.00 3854 gflxR5Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 3.00 4016 & & & & r = 1.76\arcsec.\\ 4017 gflxR4Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 1.76\arcsec.\\ 4018 gflxR5 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 3.00\arcsec.\\ 4019 gflxR5Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 3.00\arcsec.\\ 3855 4020 gflxR5Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection within an aperture of radius \\ 3856 & & & & r = 3.00 3857 gflxR5Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 3.00 3858 gflxR6 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 4.63 3859 gflxR6Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 4.63 4021 & & & & r = 3.00\arcsec.\\ 4022 gflxR5Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 3.00\arcsec.\\ 4023 gflxR6 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 4.63\arcsec.\\ 4024 gflxR6Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 4.63\arcsec.\\ 3860 4025 gflxR6Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection within an aperture of radius \\ 3861 & & & & r = 4.63 3862 gflxR6Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 4.63 3863 gflxR7 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 7.43 3864 gflxR7Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 7.43 4026 & & & & r = 4.63\arcsec.\\ 4027 gflxR6Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 4.63\arcsec.\\ 4028 gflxR7 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 7.43\arcsec.\\ 4029 gflxR7Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 7.43\arcsec.\\ 3865 4030 gflxR7Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection within an aperture of radius \\ 3866 & & & & r = 7.43 3867 gflxR7Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 7.43 3868 gflxR8 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 11.42 3869 gflxR8Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 11.42 4031 & & & & r = 7.43\arcsec.\\ 4032 gflxR7Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 7.43\arcsec.\\ 4033 gflxR8 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 11.42\arcsec.\\ 4034 gflxR8Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 11.42\arcsec.\\ 3870 4035 gflxR8Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection within an aperture of radius \\ 3871 & & & & r = 11.42 3872 gflxR8Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 11.42 3873 gflxR9 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 18.20 3874 gflxR9Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 18.20 4036 & & & & r = 11.42\arcsec.\\ 4037 gflxR8Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 11.42\arcsec.\\ 4038 gflxR9 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 18.20\arcsec.\\ 4039 gflxR9Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 18.20\arcsec.\\ 3875 4040 gflxR9Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection within an aperture of radius \\ 3876 & & & & r = 18.20 3877 gflxR9Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 18.20 3878 gflxR10 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 28.20 3879 gflxR10Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 28.20 4041 & & & & r = 18.20\arcsec.\\ 4042 gflxR9Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 18.20\arcsec.\\ 4043 gflxR10 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 28.20\arcsec.\\ 4044 gflxR10Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 28.20\arcsec.\\ 3880 4045 gflxR10Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection within an aperture of radius \\ 3881 & & & & r = 28.20 3882 gflxR10Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 28.20 3883 gflxR11 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 44.21 3884 gflxR11Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 44.21 4046 & & & & r = 28.20\arcsec.\\ 4047 gflxR10Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 28.20\arcsec.\\ 4048 gflxR11 & Jy & REAL & -999 &Flux from g filter detection within an aperture of radius r = 44.21\arcsec.\\ 4049 gflxR11Err & Jy & REAL & -999 &Error in flux from g filter detection within an aperture of radius r = 44.21\arcsec.\\ 3885 4050 gflxR11Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection within an aperture of radius \\ 3886 & & & & r = 44.21 3887 gflxR11Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 44.21 4051 & & & & r = 44.21\arcsec.\\ 4052 gflxR11Fill & - & REAL & -999 &Aperture fill factor for g filter detection within an aperture of radius r = 44.21\arcsec.\\ 3888 4053 rippDetectID\\ 3889 4054 ... & & & & same entries repeated for r, i, z, and y filters \\ … … 3895 4060 \end{table}% 3896 4061 3897 \begin{table}[ b]3898 \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 (1.5arcsec). 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.}4062 \begin{table}[htb] 4063 \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.} 3899 4064 \begin{center} 3900 4065 %\resizebox{\textwidth}{!}{% … … 3913 4078 gstackDetectID & - & BIGINT & NA &Unique \ippstage{stack} detection identifier.\\ 3914 4079 gstackImageID & - & BIGINT & NA &Unique \ippstage{stack} identifier for g filter detection.\\ 3915 gc6flxR3 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 3916 & & & & within an aperture of radius r = 1.03 4080 gc6flxR3 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\ 4081 & & & & within an aperture of radius r = 1.03\arcsec.\\ 3917 4082 gc6flxR3Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 6 sky pixels \\ 3918 & & & & (1.5 arcsec) within an aperture of radius r = 1.03arcsec.\\4083 & & & & (1.5\arcsec) within an aperture of radius r = 1.03\arcsec.\\ 3919 4084 gc6flxR3Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 6 \\ 3920 & & & & sky pixels (1.5 arcsec) within an aperture of radius r = 1.03arcsec.\\4085 & & & & sky pixels (1.5\arcsec) within an aperture of radius r = 1.03\arcsec.\\ 3921 4086 gc6flxR3Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\ 3922 & & & & (1.5 arcsec) within an aperture of radius r = 1.03arcsec.\\3923 %gc6flxR4 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 3924 %& & & & within an aperture of radius r = 1.76 4087 & & & & (1.5\arcsec) within an aperture of radius r = 1.03\arcsec.\\ 4088 %gc6flxR4 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\ 4089 %& & & & within an aperture of radius r = 1.76\arcsec.\\ 3925 4090 %gc6flxR4Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 6 sky pixels \\ 3926 %& & & & (1.5 arcsec) within an aperture of radius r = 1.76arcsec.\\4091 %& & & & (1.5\arcsec) within an aperture of radius r = 1.76\arcsec.\\ 3927 4092 %gc6flxR4Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 6 \\ 3928 %& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 1.76arcsec.\\4093 %& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 1.76\arcsec.\\ 3929 4094 %gc6flxR4Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\ 3930 %& & & & (1.5 arcsec) within an aperture of radius r = 1.76arcsec.\\3931 %gc6flxR5 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 3932 %& & & & within an aperture of radius r = 3.00 4095 %& & & & (1.5\arcsec) within an aperture of radius r = 1.76\arcsec.\\ 4096 %gc6flxR5 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\ 4097 %& & & & within an aperture of radius r = 3.00\arcsec.\\ 3933 4098 %gc6flxR5Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 6 sky pixels \\ 3934 %& & & & (1.5 arcsec) within an aperture of radius r = 3.00arcsec.\\4099 %& & & & (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\ 3935 4100 %gc6flxR5Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 6 \\ 3936 %& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 3.00arcsec.\\4101 %& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\ 3937 4102 %gc6flxR5Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\ 3938 %& & & & (1.5 arcsec) within an aperture of radius r = 3.00arcsec.\\3939 %gc6flxR6 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 3940 %& & & & within an aperture of radius r = 4.63 4103 %& & & & (1.5\arcsec) within an aperture of radius r = 3.00\arcsec.\\ 4104 %gc6flxR6 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\ 4105 %& & & & within an aperture of radius r = 4.63\arcsec.\\ 3941 4106 %gc6flxR6Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 6 sky pixels \\ 3942 %& & & & (1.5 arcsec) within an aperture of radius r = 4.63arcsec.\\4107 %& & & & (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\ 3943 4108 %gc6flxR6Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 6 \\ 3944 %& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 4.63arcsec.\\4109 %& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\ 3945 4110 %gc6flxR6Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\ 3946 %& & & & (1.5 arcsec) within an aperture of radius r = 4.63arcsec.\\3947 %gc6flxR7 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 3948 %& & & & within an aperture of radius r = 7.43 4111 %& & & & (1.5\arcsec) within an aperture of radius r = 4.63\arcsec.\\ 4112 %gc6flxR7 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\ 4113 %& & & & within an aperture of radius r = 7.43\arcsec.\\ 3949 4114 %gc6flxR7Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 6 sky pixels \\ 3950 %& & & & (1.5 arcsec) within an aperture of radius r = 7.43arcsec.\\4115 %& & & & (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\ 3951 4116 %gc6flxR7Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 6 \\ 3952 %& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 7.43arcsec.\\4117 %& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\ 3953 4118 %gc6flxR7Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\ 3954 %& & & & (1.5 arcsec) within an aperture of radius r = 7.43arcsec.\\3955 %gc6flxR8 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 3956 %& & & & within an aperture of radius r = 11.42 4119 %& & & & (1.5\arcsec) within an aperture of radius r = 7.43\arcsec.\\ 4120 %gc6flxR8 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\ 4121 %& & & & within an aperture of radius r = 11.42\arcsec.\\ 3957 4122 %gc6flxR8Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 6 sky pixels \\ 3958 %& & & & (1.5 arcsec) within an aperture of radius r = 11.42arcsec.\\4123 %& & & & (1.5\arcsec) within an aperture of radius r = 11.42\arcsec.\\ 3959 4124 %gc6flxR8Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 6 \\ 3960 %& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 11.42arcsec.\\4125 %& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 11.42\arcsec.\\ 3961 4126 %gc6flxR8Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\ 3962 %& & & & (1.5 arcsec) within an aperture of radius r = 11.42arcsec.\\3963 %gc6flxR9 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 3964 %& & & & within an aperture of radius r = 18.20 4127 %& & & & (1.5\arcsec) within an aperture of radius r = 11.42\arcsec.\\ 4128 %gc6flxR9 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\ 4129 %& & & & within an aperture of radius r = 18.20\arcsec.\\ 3965 4130 %gc6flxR9Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 6 sky pixels \\ 3966 %& & & & (1.5 arcsec) within an aperture of radius r = 18.20arcsec.\\4131 %& & & & (1.5\arcsec) within an aperture of radius r = 18.20\arcsec.\\ 3967 4132 %gc6flxR9Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 6 \\ 3968 %& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 18.20arcsec.\\4133 %& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 18.20\arcsec.\\ 3969 4134 %gc6flxR9Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\ 3970 %& & & & (1.5 arcsec) within an aperture of radius r = 18.20arcsec.\\3971 %gc6flxR10 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 3972 %& & & & within an aperture of radius r = 28.20 4135 %& & & & (1.5\arcsec) within an aperture of radius r = 18.20\arcsec.\\ 4136 %gc6flxR10 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\ 4137 %& & & & within an aperture of radius r = 28.20\arcsec.\\ 3973 4138 %gc6flxR10Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 6 sky pixels \\ 3974 %& & & & (1.5 arcsec) within an aperture of radius r = 28.20arcsec.\\4139 %& & & & (1.5\arcsec) within an aperture of radius r = 28.20\arcsec.\\ 3975 4140 %gc6flxR10Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 6 \\ 3976 %& & & & sky pixels (1.5 arcsec) within an aperture of radius r = 28.20arcsec.\\4141 %& & & & sky pixels (1.5\arcsec) within an aperture of radius r = 28.20\arcsec.\\ 3977 4142 %gc6flxR10Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\ 3978 %& & & & (1.5 arcsec) within an aperture of radius r = 28.20arcsec.\\3979 ... & & & & gc6flxR3 ... gc6flxR3Fill columns repeated for R4 (r = 1.76 3980 ... & & & & repeated for R5 (r = 3.00 3981 ... & & & & repeated for R6 (r = 4.63 3982 ... & & & & repeated for R7 (r = 7.43 3983 ... & & & & repeated for R8 (r = 11.42 3984 ... & & & & repeated for R9 (r = 18.20 3985 ... & & & & repeated for R10 (r = 28.20 3986 gc6flxR11 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5 3987 & & & & within an aperture of radius r = 44.21 4143 %& & & & (1.5\arcsec) within an aperture of radius r = 28.20\arcsec.\\ 4144 ... & & & & gc6flxR3 ... gc6flxR3Fill columns repeated for R4 (r = 1.76\arcsec).\\ 4145 ... & & & & repeated for R5 (r = 3.00\arcsec).\\ 4146 ... & & & & repeated for R6 (r = 4.63\arcsec).\\ 4147 ... & & & & repeated for R7 (r = 7.43\arcsec).\\ 4148 ... & & & & repeated for R8 (r = 11.42\arcsec).\\ 4149 ... & & & & repeated for R9 (r = 18.20\arcsec).\\ 4150 ... & & & & repeated for R10 (r = 28.20\arcsec).\\ 4151 gc6flxR11 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 6 sky pixels (1.5\arcsec) \\ 4152 & & & & within an aperture of radius r = 44.21\arcsec.\\ 3988 4153 gc6flxR11Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 6 sky pixels \\ 3989 & & & & (1.5 arcsec) within an aperture of radius r = 44.21arcsec.\\4154 & & & & (1.5\arcsec) within an aperture of radius r = 44.21\arcsec.\\ 3990 4155 gc6flxR11Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 6 \\ 3991 & & & & sky pixels (1.5 arcsec) within an aperture of radius r = 44.21arcsec.\\4156 & & & & sky pixels (1.5\arcsec) within an aperture of radius r = 44.21\arcsec.\\ 3992 4157 gc6flxR11Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 6 sky pixels \\ 3993 & & & & (1.5 arcsec) within an aperture of radius r = 44.21arcsec.\\4158 & & & & (1.5\arcsec) within an aperture of radius r = 44.21\arcsec.\\ 3994 4159 rippDetectID\\ 3995 4160 ... & & & & same entries repeated for r, i, z, and y filters \\ … … 4001 4166 \end{table}% 4002 4167 4003 \begin{table}[ b]4004 \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 (2.0arcsec). 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.}4168 \begin{table}[htb] 4169 \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.} 4005 4170 \begin{center} 4006 4171 %\resizebox{\textwidth}{!}{% … … 4019 4184 gstackDetectID & - & BIGINT & NA &Unique \ippstage{stack} detection identifier.\\ 4020 4185 gstackImageID & - & BIGINT & NA &Unique \ippstage{stack} identifier for g filter detection.\\ 4021 gc8flxR3 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 8 sky pixels (2.0 4022 & & & & within an aperture of radius r = 1.03 4186 gc8flxR3 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 8 sky pixels (2.0\arcsec) \\ 4187 & & & & within an aperture of radius r = 1.03\arcsec.\\ 4023 4188 gc8flxR3Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 8 sky pixels \\ 4024 & & & & (2.0 arcsec) within an aperture of radius r = 1.03arcsec.\\4189 & & & & (2.0\arcsec) within an aperture of radius r = 1.03\arcsec.\\ 4025 4190 gc8flxR3Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 8 \\ 4026 & & & & sky pixels (2.0 arcsec) within an aperture of radius r = 1.03arcsec.\\4191 & & & & sky pixels (2.0\arcsec) within an aperture of radius r = 1.03\arcsec.\\ 4027 4192 gc8flxR3Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 8 sky pixels \\ 4028 & & & & (2.0 arcsec) within an aperture of radius r = 1.03arcsec.\\4029 ... & & & & gc8flxR3 ... gc8flxR3Fill columns repeated for R4 (r = 1.76 4030 ... & & & & repeated for R5 (r = 3.00 4031 ... & & & & repeated for R6 (r = 4.63 4032 ... & & & & repeated for R7 (r = 7.43 4033 ... & & & & repeated for R8 (r = 11.42 4034 ... & & & & repeated for R9 (r = 18.20 4035 ... & & & & repeated for R10 (r = 28.20 4036 gc8flxR11 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 8 sky pixels (2.0 4037 & & & & within an aperture of radius r = 44.21 4193 & & & & (2.0\arcsec) within an aperture of radius r = 1.03\arcsec.\\ 4194 ... & & & & gc8flxR3 ... gc8flxR3Fill columns repeated for R4 (r = 1.76\arcsec).\\ 4195 ... & & & & repeated for R5 (r = 3.00\arcsec).\\ 4196 ... & & & & repeated for R6 (r = 4.63\arcsec).\\ 4197 ... & & & & repeated for R7 (r = 7.43\arcsec).\\ 4198 ... & & & & repeated for R8 (r = 11.42\arcsec).\\ 4199 ... & & & & repeated for R9 (r = 18.20\arcsec).\\ 4200 ... & & & & repeated for R10 (r = 28.20\arcsec).\\ 4201 gc8flxR11 & Jy & REAL & -999 &Flux from g filter detection convolved to a target of 8 sky pixels (2.0\arcsec) \\ 4202 & & & & within an aperture of radius r = 44.21\arcsec.\\ 4038 4203 gc8flxR11Err & Jy & REAL & -999 &Error in flux from g filter detection convolved to a target of 8 sky pixels \\ 4039 & & & & (2.0 arcsec) within an aperture of radius r = 44.21arcsec.\\4204 & & & & (2.0\arcsec) within an aperture of radius r = 44.21\arcsec.\\ 4040 4205 gc8flxR11Std & Jy & REAL & -999 &Standard deviation of flux from g filter detection convolved to a target of 8 \\ 4041 & & & & sky pixels (2.0 arcsec) within an aperture of radius r = 44.21arcsec.\\4206 & & & & sky pixels (2.0\arcsec) within an aperture of radius r = 44.21\arcsec.\\ 4042 4207 gc8flxR11Fill & - & REAL & -999 &Aperture fill factor for g filter detection convolved to a target of 8 sky pixels \\ 4043 & & & & (2.0 arcsec) within an aperture of radius r = 44.21arcsec.\\4208 & & & & (2.0\arcsec) within an aperture of radius r = 44.21\arcsec.\\ 4044 4209 rippDetectID \\ 4045 4210 ... & & & & same entries repeated for r, i, z, and y filters \\ … … 4051 4216 \end{table}% 4052 4217 4053 \begin{table}[ b]4218 \begin{table}[htb] 4054 4219 \caption{StackPetrosian: Contains the \citet{Petrosian1976} magnitudes and radii for extended sources. See \ippdbtable{StackObjectThin} table for discussion of primary, secondary, and best detections.} 4055 4220 \begin{center} … … 4135 4300 \end{table}% 4136 4301 4137 \begin{table}[ b]4302 \begin{table}[htb] 4138 4303 \caption{StackToImage: Contains the mapping of which input images were used to construct a particular stack.} 4139 4304 \begin{center} … … 4145 4310 \hline 4146 4311 stackImageID & - & BIGINT & NA &Unique \ippstage{stack} identifier.\\ 4147 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 *frameID + ccdID).\\4312 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 $\times$ frameID + ccdID).\\ 4148 4313 \hline 4149 4314 \end{tabular} … … 4154 4319 %\end{document} happy 4155 4320 4156 \begin{table}[ b]4321 \begin{table}[htb] 4157 4322 \caption{StackToFrame: Contains the mapping of input frames used to construct a particular \ippstage{stack} along with processing statistics.} 4158 4323 \begin{center} … … 4182 4347 4183 4348 %this table is broken FIXXXXX AFFTER LUNCH 4184 \begin{table}[ b]4349 \begin{table}[htb] 4185 4350 \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.} 4186 4351 \begin{center} … … 4224 4389 \subsection{Forced Warp Tables} 4225 4390 4226 \begin{table}[ b]4391 \begin{table}[htb] 4227 4392 \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}.} 4228 4393 \begin{center} … … 4244 4409 gnIncKronFlux & - & SMALLINT & -999 &Number of forced single epoch detections in Kron (1980) flux mean in g filter.\\ 4245 4410 gnIncApFlux & - & SMALLINT & -999 &Number of forced single epoch detections in aperture flux mean in g filter.\\ 4246 gnIncR5 & - & SMALLINT & -999 &Number of forced single epoch detections in R5 (r = 3.00 4247 gnIncR6 & - & SMALLINT & -999 &Number of forced single epoch detections in R6 (r = 4.63 4248 gnIncR7 & - & SMALLINT & -999 &Number of forced single epoch detections in R7 (r = 7.43 4411 gnIncR5 & - & SMALLINT & -999 &Number of forced single epoch detections in R5 (r = 3.00\arcsec) aperture flux mean in g filter.\\ 4412 gnIncR6 & - & SMALLINT & -999 &Number of forced single epoch detections in R6 (r = 4.63\arcsec) aperture flux mean in g filter.\\ 4413 gnIncR7 & - & SMALLINT & -999 &Number of forced single epoch detections in R7 (r = 7.43\arcsec) aperture flux mean in g filter.\\ 4249 4414 gFPSFFlux & Jy & REAL & -999 &Mean PSF flux from forced single epoch g filter detections.\\ 4250 4415 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.\\ 4264 4429 gFmeanflxR5 & Jy & REAL & -999 &Mean flux from forced single epoch g filter \\ 4265 & & & & detections within an aperture of radius r = 3.00 4430 & & & & detections within an aperture of radius r = 3.00\arcsec.\\ 4266 4431 gFmeanflxR5Err & Jy & REAL & -999 &Error in mean flux from forced single epoch g filter \\ 4267 & & & & detections within an aperture of radius r = 3.00 4432 & & & & detections within an aperture of radius r = 3.00\arcsec.\\ 4268 4433 gFmeanflxR5Std & Jy & REAL & -999 &Standard deviation of forced single epoch g filter \\ 4269 & & & & detection fluxes within an aperture of radius r = 3.00 4434 & & & & detection fluxes within an aperture of radius r = 3.00\arcsec.\\ 4270 4435 gFmeanflxR5Fill & - & REAL & -999 &Aperture fill factor for forced single epoch g filter \\ 4271 & & & & detections within an aperture of radius r = 3.00 4436 & & & & detections within an aperture of radius r = 3.00\arcsec.\\ 4272 4437 gFmeanMagR5 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch g filter \\ 4273 & & & & detections within an aperture of radius r = 3.00 4438 & & & & detections within an aperture of radius r = 3.00\arcsec.\\ 4274 4439 gFmeanMagR5Err & AB & REAL & -999 &Error in magnitude from mean flux from forced single epoch \\ 4275 & & & & g filter detections within an aperture of radius r = 3.00 4440 & & & & g filter detections within an aperture of radius r = 3.00\arcsec.\\ 4276 4441 gFmeanflxR6 & Jy & REAL & -999 &Mean flux from forced single epoch g filter \\ 4277 & & & & detections within an aperture of radius r = 4.63 4442 & & & & detections within an aperture of radius r = 4.63\arcsec.\\ 4278 4443 gFmeanflxR6Err & Jy & REAL & -999 &Error in mean flux from forced single epoch g filter \\ 4279 & & & & detections within an aperture of radius r = 4.63 4444 & & & & detections within an aperture of radius r = 4.63\arcsec.\\ 4280 4445 gFmeanflxR6Std & Jy & REAL & -999 &Standard deviation of forced single epoch g filter \\ 4281 & & & & detection fluxes within an aperture of radius r = 4.63 4446 & & & & detection fluxes within an aperture of radius r = 4.63\arcsec.\\ 4282 4447 gFmeanflxR6Fill & - & REAL & -999 &Aperture fill factor for forced single epoch g filter \\ 4283 & & & & detections within an aperture of radius r = 4.63 4448 & & & & detections within an aperture of radius r = 4.63\arcsec.\\ 4284 4449 gFmeanMagR6 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch g filter \\ 4285 & & & & detections within an aperture of radius r = 4.63 4450 & & & & detections within an aperture of radius r = 4.63\arcsec.\\ 4286 4451 gFmeanMagR6Err & AB & REAL & -999 &Error in magnitude from mean flux from forced single epoch \\ 4287 & & & & g filter detections within an aperture of radius r = 4.63 4452 & & & & g filter detections within an aperture of radius r = 4.63\arcsec.\\ 4288 4453 gFmeanflxR7 & Jy & REAL & -999 &Mean flux from forced single epoch g filter \\ 4289 & & & & detections within an aperture of radius r = 7.43 4454 & & & & detections within an aperture of radius r = 7.43\arcsec.\\ 4290 4455 gFmeanflxR7Err & Jy & REAL & -999 &Error in mean flux from forced single epoch g filter\\ 4291 & & & & detections within an aperture of radius r = 7.43 4456 & & & & detections within an aperture of radius r = 7.43\arcsec.\\ 4292 4457 gFmeanflxR7Std & Jy & REAL & -999 &Standard deviation of forced single epoch g filter \\ 4293 & & & & detection fluxes within an aperture of radius r = 7.43 4458 & & & & detection fluxes within an aperture of radius r = 7.43\arcsec.\\ 4294 4459 gFmeanflxR7Fill & - & REAL & -999 &Aperture fill factor for forced single epoch g filter \\ 4295 & & & & detections within an aperture of radius r = 7.43 4460 & & & & detections within an aperture of radius r = 7.43\arcsec.\\ 4296 4461 gFmeanMagR7 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch g filter\\ 4297 & & & & detections within an aperture of radius r = 7.43 4462 & & & & detections within an aperture of radius r = 7.43\arcsec.\\ 4298 4463 gFmeanMagR7Err & AB & REAL & -999 &Error in magnitude from mean flux from forced single epoch\\ 4299 & & & & g filter detections within an aperture of radius r = 7.43 4464 & & & & g filter detections within an aperture of radius r = 7.43\arcsec.\\ 4300 4465 gFlags & - & INT & 0 &Information flag bitmask indicating details of the photometry from forced \\ 4301 4466 & & & & 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.\\ 4311 4476 %rnIncApFlux & - & SMALLINT & -999 &Number of forced single epoch detections in aperture flux mean in r filter.\\ 4312 %rnIncR5 & - & SMALLINT & -999 &Number of forced single epoch detections in R5 (r = 3.00 4313 %rnIncR6 & - & SMALLINT & -999 &Number of forced single epoch detections in R6 (r = 4.63 4314 %rnIncR7 & - & SMALLINT & -999 &Number of forced single epoch detections in R7 (r = 7.43 4477 %rnIncR5 & - & SMALLINT & -999 &Number of forced single epoch detections in R5 (r = 3.00\arcsec) aperture flux mean in r filter.\\ 4478 %rnIncR6 & - & SMALLINT & -999 &Number of forced single epoch detections in R6 (r = 4.63\arcsec) aperture flux mean in r filter.\\ 4479 %rnIncR7 & - & SMALLINT & -999 &Number of forced single epoch detections in R7 (r = 7.43\arcsec) aperture flux mean in r filter.\\ 4315 4480 %rFPSFFlux & Jy & REAL & -999 &Mean PSF flux from forced single epoch r filter detections.\\ 4316 4481 %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.\\ 4329 4494 %rFApMagErr & AB & REAL & -999 &Error in magnitude from mean aperture flux from forced single epoch r filter detections.\\ 4330 %rFmeanflxR5 & Jy & REAL & -999 &Mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00 4331 %rFmeanflxR5Err & Jy & REAL & -999 &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00 4332 %rFmeanflxR5Std & Jy & REAL & -999 &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 3.00 4333 %rFmeanflxR5Fill & - & REAL & -999 &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 3.00 4334 %rFmeanMagR5 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00 4335 %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 4336 %rFmeanflxR6 & Jy & REAL & -999 &Mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63 4337 %rFmeanflxR6Err & Jy & REAL & -999 &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63 4338 %rFmeanflxR6Std & Jy & REAL & -999 &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 4.63 4339 %rFmeanflxR6Fill & - & REAL & -999 &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 4.63 4340 %rFmeanMagR6 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63 4341 %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 4342 %rFmeanflxR7 & Jy & REAL & -999 &Mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43 4343 %rFmeanflxR7Err & Jy & REAL & -999 &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43 4344 %rFmeanflxR7Std & Jy & REAL & -999 &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 7.43 4345 %rFmeanflxR7Fill & - & REAL & -999 &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 7.43 4346 %rFmeanMagR7 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43 4347 %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 4495 %rFmeanflxR5 & Jy & REAL & -999 &Mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00\arcsec.\\ 4496 %rFmeanflxR5Err & Jy & REAL & -999 &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00\arcsec.\\ 4497 %rFmeanflxR5Std & Jy & REAL & -999 &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 3.00\arcsec.\\ 4498 %rFmeanflxR5Fill & - & REAL & -999 &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 3.00\arcsec.\\ 4499 %rFmeanMagR5 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 3.00\arcsec.\\ 4500 %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.\\ 4501 %rFmeanflxR6 & Jy & REAL & -999 &Mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63\arcsec.\\ 4502 %rFmeanflxR6Err & Jy & REAL & -999 &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63\arcsec.\\ 4503 %rFmeanflxR6Std & Jy & REAL & -999 &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 4.63\arcsec.\\ 4504 %rFmeanflxR6Fill & - & REAL & -999 &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 4.63\arcsec.\\ 4505 %rFmeanMagR6 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 4.63\arcsec.\\ 4506 %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.\\ 4507 %rFmeanflxR7 & Jy & REAL & -999 &Mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43\arcsec.\\ 4508 %rFmeanflxR7Err & Jy & REAL & -999 &Error in mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43\arcsec.\\ 4509 %rFmeanflxR7Std & Jy & REAL & -999 &Standard deviation of forced single epoch r filter detection fluxes within an aperture of radius r = 7.43\arcsec.\\ 4510 %rFmeanflxR7Fill & - & REAL & -999 &Aperture fill factor for forced single epoch r filter detections within an aperture of radius r = 7.43\arcsec.\\ 4511 %rFmeanMagR7 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch r filter detections within an aperture of radius r = 7.43\arcsec.\\ 4512 %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.\\ 4348 4513 %rFlags & - & INT & 0 &Information flag bitmask indicating details of the photometry from forced single epoch r filter detections. Values listed in ObjectInfoFlags.\\ 4349 4514 %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.\\ 4354 4519 %inIncApFlux & - & SMALLINT & -999 &Number of forced single epoch detections in aperture flux mean in i filter.\\ 4355 %inIncR5 & - & SMALLINT & -999 &Number of forced single epoch detections in R5 (r = 3.00 4356 %inIncR6 & - & SMALLINT & -999 &Number of forced single epoch detections in R6 (r = 4.63 4357 %inIncR7 & - & SMALLINT & -999 &Number of forced single epoch detections in R7 (r = 7.43 4520 %inIncR5 & - & SMALLINT & -999 &Number of forced single epoch detections in R5 (r = 3.00\arcsec) aperture flux mean in i filter.\\ 4521 %inIncR6 & - & SMALLINT & -999 &Number of forced single epoch detections in R6 (r = 4.63\arcsec) aperture flux mean in i filter.\\ 4522 %inIncR7 & - & SMALLINT & -999 &Number of forced single epoch detections in R7 (r = 7.43\arcsec) aperture flux mean in i filter.\\ 4358 4523 %iFPSFFlux & Jy & REAL & -999 &Mean PSF flux from forced single epoch i filter detections.\\ 4359 4524 %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.\\ 4372 4537 %iFApMagErr & AB & REAL & -999 &Error in magnitude from mean aperture flux from forced single epoch i filter detections.\\ 4373 %iFmeanflxR5 & Jy & REAL & -999 &Mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00 4374 %iFmeanflxR5Err & Jy & REAL & -999 &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00 4375 %iFmeanflxR5Std & Jy & REAL & -999 &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 3.00 4376 %iFmeanflxR5Fill & - & REAL & -999 &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 3.00 4377 %iFmeanMagR5 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00 4378 %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 4379 %iFmeanflxR6 & Jy & REAL & -999 &Mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63 4380 %iFmeanflxR6Err & Jy & REAL & -999 &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63 4381 %iFmeanflxR6Std & Jy & REAL & -999 &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 4.63 4382 %iFmeanflxR6Fill & - & REAL & -999 &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 4.63 4383 %iFmeanMagR6 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63 4384 %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 4385 %iFmeanflxR7 & Jy & REAL & -999 &Mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43 4386 %iFmeanflxR7Err & Jy & REAL & -999 &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43 4387 %iFmeanflxR7Std & Jy & REAL & -999 &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 7.43 4388 %iFmeanflxR7Fill & - & REAL & -999 &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 7.43 4389 %iFmeanMagR7 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43 4390 %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 4538 %iFmeanflxR5 & Jy & REAL & -999 &Mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00\arcsec.\\ 4539 %iFmeanflxR5Err & Jy & REAL & -999 &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00\arcsec.\\ 4540 %iFmeanflxR5Std & Jy & REAL & -999 &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 3.00\arcsec.\\ 4541 %iFmeanflxR5Fill & - & REAL & -999 &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 3.00\arcsec.\\ 4542 %iFmeanMagR5 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 3.00\arcsec.\\ 4543 %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.\\ 4544 %iFmeanflxR6 & Jy & REAL & -999 &Mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63\arcsec.\\ 4545 %iFmeanflxR6Err & Jy & REAL & -999 &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63\arcsec.\\ 4546 %iFmeanflxR6Std & Jy & REAL & -999 &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 4.63\arcsec.\\ 4547 %iFmeanflxR6Fill & - & REAL & -999 &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 4.63\arcsec.\\ 4548 %iFmeanMagR6 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 4.63\arcsec.\\ 4549 %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.\\ 4550 %iFmeanflxR7 & Jy & REAL & -999 &Mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43\arcsec.\\ 4551 %iFmeanflxR7Err & Jy & REAL & -999 &Error in mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43\arcsec.\\ 4552 %iFmeanflxR7Std & Jy & REAL & -999 &Standard deviation of forced single epoch i filter detection fluxes within an aperture of radius r = 7.43\arcsec.\\ 4553 %iFmeanflxR7Fill & - & REAL & -999 &Aperture fill factor for forced single epoch i filter detections within an aperture of radius r = 7.43\arcsec.\\ 4554 %iFmeanMagR7 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch i filter detections within an aperture of radius r = 7.43\arcsec.\\ 4555 %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.\\ 4391 4556 %iFlags & - & INT & 0 &Information flag bitmask indicating details of the photometry from forced single epoch i filter detections. Values listed in ObjectInfoFlags.\\ 4392 4557 %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.\\ 4397 4562 %znIncApFlux & - & SMALLINT & -999 &Number of forced single epoch detections in aperture flux mean in z filter.\\ 4398 %znIncR5 & - & SMALLINT & -999 &Number of forced single epoch detections in R5 (r = 3.00 4399 %znIncR6 & - & SMALLINT & -999 &Number of forced single epoch detections in R6 (r = 4.63 4400 %znIncR7 & - & SMALLINT & -999 &Number of forced single epoch detections in R7 (r = 7.43 4563 %znIncR5 & - & SMALLINT & -999 &Number of forced single epoch detections in R5 (r = 3.00\arcsec) aperture flux mean in z filter.\\ 4564 %znIncR6 & - & SMALLINT & -999 &Number of forced single epoch detections in R6 (r = 4.63\arcsec) aperture flux mean in z filter.\\ 4565 %znIncR7 & - & SMALLINT & -999 &Number of forced single epoch detections in R7 (r = 7.43\arcsec) aperture flux mean in z filter.\\ 4401 4566 %zFPSFFlux & Jy & REAL & -999 &Mean PSF flux from forced single epoch z filter detections.\\ 4402 4567 %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.\\ 4415 4580 %zFApMagErr & AB & REAL & -999 &Error in magnitude from mean aperture flux from forced single epoch z filter detections.\\ 4416 %zFmeanflxR5 & Jy & REAL & -999 &Mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00 4417 %zFmeanflxR5Err & Jy & REAL & -999 &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00 4418 %zFmeanflxR5Std & Jy & REAL & -999 &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 3.00 4419 %zFmeanflxR5Fill & - & REAL & -999 &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 3.00 4420 %zFmeanMagR5 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00 4421 %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 4422 %zFmeanflxR6 & Jy & REAL & -999 &Mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63 4423 %zFmeanflxR6Err & Jy & REAL & -999 &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63 4424 %zFmeanflxR6Std & Jy & REAL & -999 &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 4.63 4425 %zFmeanflxR6Fill & - & REAL & -999 &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 4.63 4426 %zFmeanMagR6 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63 4427 %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 4428 %zFmeanflxR7 & Jy & REAL & -999 &Mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43 4429 %zFmeanflxR7Err & Jy & REAL & -999 &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43 4430 %zFmeanflxR7Std & Jy & REAL & -999 &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 7.43 4431 %zFmeanflxR7Fill & - & REAL & -999 &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 7.43 4432 %zFmeanMagR7 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43 4433 %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 4581 %zFmeanflxR5 & Jy & REAL & -999 &Mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00\arcsec.\\ 4582 %zFmeanflxR5Err & Jy & REAL & -999 &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00\arcsec.\\ 4583 %zFmeanflxR5Std & Jy & REAL & -999 &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 3.00\arcsec.\\ 4584 %zFmeanflxR5Fill & - & REAL & -999 &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 3.00\arcsec.\\ 4585 %zFmeanMagR5 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 3.00\arcsec.\\ 4586 %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.\\ 4587 %zFmeanflxR6 & Jy & REAL & -999 &Mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63\arcsec.\\ 4588 %zFmeanflxR6Err & Jy & REAL & -999 &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63\arcsec.\\ 4589 %zFmeanflxR6Std & Jy & REAL & -999 &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 4.63\arcsec.\\ 4590 %zFmeanflxR6Fill & - & REAL & -999 &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 4.63\arcsec.\\ 4591 %zFmeanMagR6 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 4.63\arcsec.\\ 4592 %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.\\ 4593 %zFmeanflxR7 & Jy & REAL & -999 &Mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43\arcsec.\\ 4594 %zFmeanflxR7Err & Jy & REAL & -999 &Error in mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43\arcsec.\\ 4595 %zFmeanflxR7Std & Jy & REAL & -999 &Standard deviation of forced single epoch z filter detection fluxes within an aperture of radius r = 7.43\arcsec.\\ 4596 %zFmeanflxR7Fill & - & REAL & -999 &Aperture fill factor for forced single epoch z filter detections within an aperture of radius r = 7.43\arcsec.\\ 4597 %zFmeanMagR7 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch z filter detections within an aperture of radius r = 7.43\arcsec.\\ 4598 %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.\\ 4434 4599 %zFlags & - & INT & 0 &Information flag bitmask indicating details of the photometry from forced single epoch z filter detections. Values listed in ObjectInfoFlags.\\ 4435 4600 %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.\\ 4440 4605 %ynIncApFlux & - & SMALLINT & -999 &Number of forced single epoch detections in aperture flux mean in y filter.\\ 4441 %ynIncR5 & - & SMALLINT & -999 &Number of forced single epoch detections in R5 (r = 3.00 4442 %ynIncR6 & - & SMALLINT & -999 &Number of forced single epoch detections in R6 (r = 4.63 4443 %ynIncR7 & - & SMALLINT & -999 &Number of forced single epoch detections in R7 (r = 7.43 4606 %ynIncR5 & - & SMALLINT & -999 &Number of forced single epoch detections in R5 (r = 3.00\arcsec) aperture flux mean in y filter.\\ 4607 %ynIncR6 & - & SMALLINT & -999 &Number of forced single epoch detections in R6 (r = 4.63\arcsec) aperture flux mean in y filter.\\ 4608 %ynIncR7 & - & SMALLINT & -999 &Number of forced single epoch detections in R7 (r = 7.43\arcsec) aperture flux mean in y filter.\\ 4444 4609 %yFPSFFlux & Jy & REAL & -999 &Mean PSF flux from forced single epoch y filter detections.\\ 4445 4610 %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.\\ 4458 4623 %yFApMagErr & AB & REAL & -999 &Error in magnitude from mean aperture flux from forced single epoch y filter detections.\\ 4459 %yFmeanflxR5 & Jy & REAL & -999 &Mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00 4460 %yFmeanflxR5Err & Jy & REAL & -999 &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00 4461 %yFmeanflxR5Std & Jy & REAL & -999 &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 3.00 4462 %yFmeanflxR5Fill & - & REAL & -999 &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 3.00 4463 %yFmeanMagR5 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00 4464 %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 4465 %yFmeanflxR6 & Jy & REAL & -999 &Mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63 4466 %yFmeanflxR6Err & Jy & REAL & -999 &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63 4467 %yFmeanflxR6Std & Jy & REAL & -999 &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 4.63 4468 %yFmeanflxR6Fill & - & REAL & -999 &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 4.63 4469 %yFmeanMagR6 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63 4470 %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 4471 %yFmeanflxR7 & Jy & REAL & -999 &Mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43 4472 %yFmeanflxR7Err & Jy & REAL & -999 &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43 4473 %yFmeanflxR7Std & Jy & REAL & -999 &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 7.43 4474 %yFmeanflxR7Fill & - & REAL & -999 &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 7.43 4475 %yFmeanMagR7 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43 4476 %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 4624 %yFmeanflxR5 & Jy & REAL & -999 &Mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00\arcsec.\\ 4625 %yFmeanflxR5Err & Jy & REAL & -999 &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00\arcsec.\\ 4626 %yFmeanflxR5Std & Jy & REAL & -999 &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 3.00\arcsec.\\ 4627 %yFmeanflxR5Fill & - & REAL & -999 &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 3.00\arcsec.\\ 4628 %yFmeanMagR5 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 3.00\arcsec.\\ 4629 %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.\\ 4630 %yFmeanflxR6 & Jy & REAL & -999 &Mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63\arcsec.\\ 4631 %yFmeanflxR6Err & Jy & REAL & -999 &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63\arcsec.\\ 4632 %yFmeanflxR6Std & Jy & REAL & -999 &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 4.63\arcsec.\\ 4633 %yFmeanflxR6Fill & - & REAL & -999 &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 4.63\arcsec.\\ 4634 %yFmeanMagR6 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 4.63\arcsec.\\ 4635 %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.\\ 4636 %yFmeanflxR7 & Jy & REAL & -999 &Mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43\arcsec.\\ 4637 %yFmeanflxR7Err & Jy & REAL & -999 &Error in mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43\arcsec.\\ 4638 %yFmeanflxR7Std & Jy & REAL & -999 &Standard deviation of forced single epoch y filter detection fluxes within an aperture of radius r = 7.43\arcsec.\\ 4639 %yFmeanflxR7Fill & - & REAL & -999 &Aperture fill factor for forced single epoch y filter detections within an aperture of radius r = 7.43\arcsec.\\ 4640 %yFmeanMagR7 & AB & REAL & -999 &Magnitude from mean flux from forced single epoch y filter detections within an aperture of radius r = 7.43\arcsec.\\ 4641 %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.\\ 4477 4642 %yFlags & - & INT & 0 &Information flag bitmask indicating details of the photometry from forced single epoch y filter detections. Values listed in ObjectInfoFlags.\\ 4478 4643 %yE1 & - & REAL & -999 &\citet{Kaiser1995} polarization parameter e1 = (Mxx - Myy) / (Mxx + Myy) from forced single epoch y filter detections.\\ … … 4487 4652 4488 4653 4489 \begin{table}[ b]4654 \begin{table}[htb] 4490 4655 \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.} 4491 4656 \begin{center} … … 4503 4668 batchID & - & BIGINT & NA &Internal database batch identifier.\\ 4504 4669 processingVersion & - & TINYINT & NA &Data release version.\\ 4505 gLensObjSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced g filter detections.\\4506 gLensObjSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced g filter detections.\\4507 gLensObjSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced g filter detections.\\4508 gLensObjSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced g filter detections.\\4509 gLensObjSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced g filter detections.\\4670 gLensObjSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced g filter detections.\\ 4671 gLensObjSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced g filter detections.\\ 4672 gLensObjSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced g filter detections.\\ 4673 gLensObjSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced g filter detections.\\ 4674 gLensObjSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced g filter detections.\\ 4510 4675 gLensObjShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from forced g filter detections.\\ 4511 4676 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.\\ 4514 4679 gLensObjShearE2 & - & REAL & -999 &K95 eq. (B12) shear polarizability e2 term from forced g filter detections.\\ 4515 gLensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced g filter detections.\\4516 gLensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced g filter detections.\\4517 gLensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced g filter detections.\\4518 gLensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced g filter detections.\\4519 gLensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced g filter detections.\\4680 gLensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced g filter detections.\\ 4681 gLensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced g filter detections.\\ 4682 gLensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced g filter detections.\\ 4683 gLensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced g filter detections.\\ 4684 gLensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced g filter detections.\\ 4520 4685 gLensPSFShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from PSF model for forced g filter detections.\\ 4521 4686 gLensPSFShearX12 & - & REAL & -999 &K95 eq. (B11) shear polarizability X12 term from PSF model for forced g filter detections.\\ … … 4525 4690 rlensObjSmearX11 \\ 4526 4691 ... & & & & same entries repeated for r, i, z, and y filters \\ 4527 %rlensObjSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced r filter detections.\\4528 %rlensObjSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced r filter detections.\\4529 %rlensObjSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced r filter detections.\\4530 %rlensObjSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced r filter detections.\\4531 %rlensObjSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced r filter detections.\\4692 %rlensObjSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced r filter detections.\\ 4693 %rlensObjSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced r filter detections.\\ 4694 %rlensObjSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced r filter detections.\\ 4695 %rlensObjSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced r filter detections.\\ 4696 %rlensObjSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced r filter detections.\\ 4532 4697 %rlensObjShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from forced r filter detections.\\ 4533 4698 %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.\\ 4536 4701 %rlensObjShearE2 & - & REAL & -999 &K95 eq. (B12) shear polarizability e2 term from forced r filter detections.\\ 4537 %rlensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced r filter detections.\\4538 %rlensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced r filter detections.\\4539 %rlensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced r filter detections.\\4540 %rlensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced r filter detections.\\4541 %rlensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced r filter detections.\\4702 %rlensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced r filter detections.\\ 4703 %rlensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced r filter detections.\\ 4704 %rlensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced r filter detections.\\ 4705 %rlensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced r filter detections.\\ 4706 %rlensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced r filter detections.\\ 4542 4707 %rlensPSFShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from PSF model for forced r filter detections.\\ 4543 4708 %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.\\ 4546 4711 %rlensPSFShearE2 & - & REAL & -999 &K95 eq. (B12) shear polarizability e2 term from PSF model forced r filter detections.\\ 4547 %ilensObjSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced i filter detections.\\4548 %ilensObjSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced i filter detections.\\4549 %ilensObjSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced i filter detections.\\4550 %ilensObjSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced i filter detections.\\4551 %ilensObjSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced i filter detections.\\4712 %ilensObjSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced i filter detections.\\ 4713 %ilensObjSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced i filter detections.\\ 4714 %ilensObjSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced i filter detections.\\ 4715 %ilensObjSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced i filter detections.\\ 4716 %ilensObjSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced i filter detections.\\ 4552 4717 %ilensObjShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from forced i filter detections.\\ 4553 4718 %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.\\ 4556 4721 %ilensObjShearE2 & - & REAL & -999 &K95 eq. (B12) shear polarizability e2 term from forced i filter detections.\\ 4557 %ilensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced i filter detections.\\4558 %ilensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced i filter detections.\\4559 %ilensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced i filter detections.\\4560 %ilensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced i filter detections.\\4561 %ilensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced i filter detections.\\4722 %ilensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced i filter detections.\\ 4723 %ilensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced i filter detections.\\ 4724 %ilensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced i filter detections.\\ 4725 %ilensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced i filter detections.\\ 4726 %ilensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced i filter detections.\\ 4562 4727 %ilensPSFShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from PSF model for forced i filter detections.\\ 4563 4728 %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.\\ 4566 4731 %ilensPSFShearE2 & - & REAL & -999 &K95 eq. (B12) shear polarizability e2 term from PSF model forced i filter detections.\\ 4567 %zlensObjSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced z filter detections.\\4568 %zlensObjSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced z filter detections.\\4569 %zlensObjSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced z filter detections.\\4570 %zlensObjSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced z filter detections.\\4571 %zlensObjSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced z filter detections.\\4732 %zlensObjSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced z filter detections.\\ 4733 %zlensObjSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced z filter detections.\\ 4734 %zlensObjSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced z filter detections.\\ 4735 %zlensObjSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced z filter detections.\\ 4736 %zlensObjSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced z filter detections.\\ 4572 4737 %zlensObjShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from forced z filter detections.\\ 4573 4738 %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.\\ 4576 4741 %zlensObjShearE2 & - & REAL & -999 &K95 eq. (B12) shear polarizability e2 term from forced z filter detections.\\ 4577 %zlensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced z filter detections.\\4578 %zlensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced z filter detections.\\4579 %zlensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced z filter detections.\\4580 %zlensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced z filter detections.\\4581 %zlensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced z filter detections.\\4742 %zlensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced z filter detections.\\ 4743 %zlensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced z filter detections.\\ 4744 %zlensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced z filter detections.\\ 4745 %zlensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced z filter detections.\\ 4746 %zlensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced z filter detections.\\ 4582 4747 %zlensPSFShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from PSF model for forced z filter detections.\\ 4583 4748 %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.\\ 4586 4751 %zlensPSFShearE2 & - & REAL & -999 &K95 eq. (B12) shear polarizability e2 term from PSF model forced z filter detections.\\ 4587 %ylensObjSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced y filter detections.\\4588 %ylensObjSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced y filter detections.\\4589 %ylensObjSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced y filter detections.\\4590 %ylensObjSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced y filter detections.\\4591 %ylensObjSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced y filter detections.\\4752 %ylensObjSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced y filter detections.\\ 4753 %ylensObjSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced y filter detections.\\ 4754 %ylensObjSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced y filter detections.\\ 4755 %ylensObjSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced y filter detections.\\ 4756 %ylensObjSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced y filter detections.\\ 4592 4757 %ylensObjShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from forced y filter detections.\\ 4593 4758 %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.\\ 4596 4761 %ylensObjShearE2 & - & REAL & -999 &K95 eq. (B12) shear polarizability e2 term from forced y filter detections.\\ 4597 %ylensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced y filter detections.\\4598 %ylensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced y filter detections.\\4599 %ylensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced y filter detections.\\4600 %ylensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced y filter detections.\\4601 %ylensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced y filter detections.\\4762 %ylensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced y filter detections.\\ 4763 %ylensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced y filter detections.\\ 4764 %ylensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced y filter detections.\\ 4765 %ylensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced y filter detections.\\ 4766 %ylensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced y filter detections.\\ 4602 4767 %ylensPSFShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from PSF model for forced y filter detections.\\ 4603 4768 %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} 4615 4780 4616 \begin{table}[ b]4781 \begin{table}[htb] 4617 4782 \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.} 4618 4783 \begin{center} … … 4650 4815 psfTheta & degrees & REAL & -999 &PSF major axis orientation at image center.\\ 4651 4816 photoZero & magnitudes & REAL & -999 &Locally derived photometric zero point for this \ippstage{warp} image.\\ 4652 ctype1 & - & VARCHAR(100) & &Name of astrometric projection in R A.\\4817 ctype1 & - & VARCHAR(100) & &Name of astrometric projection in R.A..\\ 4653 4818 ctype2 & - & VARCHAR(100) & &Name of astrometric projection in Dec.\\ 4654 4819 crval1 & degrees & FLOAT & -999 &Right ascension corresponding to reference pixel.\\ 4655 4820 crval2 & degrees & FLOAT & -999 &Declination corresponding to reference pixel.\\ 4656 crpix1 & sky pixels & FLOAT & -999 &Reference pixel for R A.\\4821 crpix1 & sky pixels & FLOAT & -999 &Reference pixel for R.A..\\ 4657 4822 crpix2 & sky pixels & FLOAT & -999 &Reference pixel for Dec.\\ 4658 cdelt1 & degrees/pixel & FLOAT & -999 &Pixel scale in R A.\\4823 cdelt1 & degrees/pixel & FLOAT & -999 &Pixel scale in R.A..\\ 4659 4824 cdelt2 & degrees/pixel & FLOAT & -999 &Pixel scale in Dec.\\ 4660 pc001001 & - & FLOAT & -999 &Linear transformation matrix element between image pixel x and R A.\\4661 pc001002 & - & FLOAT & -999 &Linear transformation matrix element between image pixel y and R A.\\4825 pc001001 & - & FLOAT & -999 &Linear transformation matrix element between image pixel x and R.A..\\ 4826 pc001002 & - & FLOAT & -999 &Linear transformation matrix element between image pixel y and R.A..\\ 4662 4827 pc002001 & - & FLOAT & -999 &Linear transformation matrix element between image pixel x and Dec.\\ 4663 4828 pc002002 & - & FLOAT & -999 &Linear transformation matrix element between image pixel y and Dec.\\ … … 4672 4837 4673 4838 4674 \begin{table}[ b]4839 \begin{table}[htb] 4675 4840 \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.} 4676 4841 \begin{center} … … 4716 4881 FpsfQfPerfect & - & REAL & -999 &PSF weighted fraction of pixels totally unmasked.\\ 4717 4882 FpsfChiSq & - & REAL & -999 &Reduced chi squared value of the PSF model fit.\\ 4718 FmomentXX & $arcsec^2$ & REAL & -999 &Second moment $M_{xx}$.\\4719 FmomentXY & $arcsec^2$ & REAL & -999 &Second moment $M_{xy}$.\\4720 FmomentYY & $arcsec^2$ & REAL & -999 &Second moment $M_{yy}$.\\4883 FmomentXX & arcsec$^2$ & REAL & -999 &Second moment $M_{xx}$.\\ 4884 FmomentXY & arcsec$^2$ & REAL & -999 &Second moment $M_{xy}$.\\ 4885 FmomentYY & arcsec$^2$ & REAL & -999 &Second moment $M_{yy}$.\\ 4721 4886 FmomentR1 & arcsec & REAL & -999 &First radial moment.\\ 4722 FmomentRH & $arcsec^{0.5}$ & REAL & -999 &Half radial moment ($r^{0.5}$ weighting).\\4723 FmomentM3C & $arcsec^2$ & REAL & -999 &Cosine of trefoil second moment term: $r^2 cos(3 theta) = M_{xxx} - 3 *M_{xyy}$.\\4724 FmomentM3S & $arcsec^2$ & REAL & -999 &Sine of trefoil second moment: $r^2 sin (3 theta) = 3 *M_{xxy} - M_{yyy}$.\\4725 FmomentM4C & $arcsec^2$ & REAL & -999 &Cosine of quadrupole second moment: $r^2 cos (4 theta) = M_{xxxx} - 6 *M_{xxyy} + M_{yyyy}$.\\4726 FmomentM4S & $arcsec^2$ & REAL & -999 &Sine of quadrupole second moment: $r^2 sin (4 theta) = 4 * M_{xxxy} - 4 *M_{xyyy}$.\\4887 FmomentRH & arcsec$^{0.5}$ & REAL & -999 &Half radial moment ($r^{0.5}$ weighting).\\ 4888 FmomentM3C & arcsec$^2$ & REAL & -999 &Cosine of trefoil second moment term: $r^2 \cos(3 \theta) = M_{xxx} - 3 M_{xyy}$.\\ 4889 FmomentM3S & arcsec$^2$ & REAL & -999 &Sine of trefoil second moment: $r^2 \sin (3 \theta) = 3 M_{xxy} - M_{yyy}$.\\ 4890 FmomentM4C & arcsec$^2$ & REAL & -999 &Cosine of quadrupole second moment: $r^2 \cos (4 \theta) = M_{xxxx} - 6 M_{xxyy} + M_{yyyy}$.\\ 4891 FmomentM4S & arcsec$^2$ & REAL & -999 &Sine of quadrupole second moment: $r^2 \sin (4 \theta) = 4 M_{xxxy} - 4 M_{xyyy}$.\\ 4727 4892 FapFlux & Jy & REAL & -999 &Aperture flux.\\ 4728 4893 FapFluxErr & Jy & REAL & -999 &Error in aperture flux.\\ … … 4732 4897 FkronFluxErr & Jy & REAL & -999 &Error in Kron (1980) flux.\\ 4733 4898 FkronRad & arcsec & REAL & -999 &Kron (1980) radius.\\ 4734 Fsky & $Jy/arcsec^2$ & REAL & -999 &Background sky level.\\4735 FskyErr & $Jy/arcsec^2$ & REAL & -999 &Error in background sky level.\\4899 Fsky & Jy arcsec$^{-2}$ & REAL & -999 &Background sky level.\\ 4900 FskyErr & Jy arcsec$^{-2}$ & REAL & -999 &Error in background sky level.\\ 4736 4901 FinfoFlag & - & BIGINT & 0 &Information flag bitmask indicating details of the photometry. \\ 4737 4902 & & & & Values listed in DetectionFlags.\\ … … 4749 4914 4750 4915 4751 \begin{table}[ b]4916 \begin{table}[htb] 4752 4917 \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.} 4753 4918 \begin{center} … … 4778 4943 \end{table}% 4779 4944 4780 \begin{table}[ b]4781 \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 = 7.43arcsec) apertures \citep{Stoughton2002} for objects detected in the stacked images.}4945 \begin{table}[htb] 4946 \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.} 4782 4947 \begin{center} 4783 4948 %\resizebox{\textwidth}{!}{% … … 4802 4967 obsTime & days & FLOAT & -999 &Modified Julian Date at the midpoint of the observation.\\ 4803 4968 flxR5 & Jy & REAL & -999 &Flux from forced photometry measurement within an aperture of radius \\ 4804 & & & & r = 3.00 4969 & & & & r = 3.00\arcsec.\\ 4805 4970 flxR5Err & Jy & REAL & -999 &Error in flux from forced photometry measurement within an aperture of\\ 4806 & & & & radius r = 3.00 4971 & & & & radius r = 3.00\arcsec.\\ 4807 4972 flxR5Std & Jy & REAL & -999 &Standard deviation of flux from forced photometry measurement within \\ 4808 & & & & an aperture of radius r = 3.00 4973 & & & & an aperture of radius r = 3.00\arcsec.\\ 4809 4974 flxR5Fill & - & REAL & -999 &Aperture fill factor for forced photometry measurement within an \\ 4810 & & & & aperture of radius r = 3.00 4975 & & & & aperture of radius r = 3.00\arcsec.\\ 4811 4976 flxR6 & Jy & REAL & -999 &Flux from forced photometry measurement within an aperture of radius \\ 4812 & & & & r = 4.63 4977 & & & & r = 4.63\arcsec.\\ 4813 4978 flxR6Err & Jy & REAL & -999 &Error in flux from forced photometry measurement within an aperture of\\ 4814 & & & & radius r = 4.63 4979 & & & & radius r = 4.63\arcsec.\\ 4815 4980 flxR6Std & Jy & REAL & -999 &Standard deviation of flux from forced photometry measurement within \\ 4816 & & & & an aperture of radius r = 4.63 4981 & & & & an aperture of radius r = 4.63\arcsec.\\ 4817 4982 flxR6Fill & - & REAL & -999 &Aperture fill factor for forced photometry measurement within an \\ 4818 & & & & aperture of radius r = 4.63 4983 & & & & aperture of radius r = 4.63\arcsec.\\ 4819 4984 flxR7 & Jy & REAL & -999 &Flux from forced photometry measurement within an aperture of radius \\ 4820 & & & & r = 7.43 4985 & & & & r = 7.43\arcsec.\\ 4821 4986 flxR7Err & Jy & REAL & -999 &Error in flux from forced photometry measurement within an aperture of\\ 4822 & & & & radius r = 7.43 4987 & & & & radius r = 7.43\arcsec.\\ 4823 4988 flxR7Std & Jy & REAL & -999 &Standard deviation of flux from forced photometry measurement within \\ 4824 & & & & an aperture of radius r = 7.43 4989 & & & & an aperture of radius r = 7.43\arcsec.\\ 4825 4990 flxR7Fill & - & REAL & -999 &Aperture fill factor for forced photometry measurement within an \\ 4826 & & & & aperture of radius r = 7.43 4991 & & & & aperture of radius r = 7.43\arcsec.\\ 4827 4992 \hline 4828 4993 \end{tabular} … … 4833 4998 4834 4999 4835 \begin{table}[ b]5000 \begin{table}[htb] 4836 5001 \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.} 4837 5002 \begin{center} … … 4856 5021 dvoRegionID & - & INT & -1 &Internal DVO region identifier.\\ 4857 5022 obsTime & days & FLOAT & -999 &Modified Julian Date at the midpoint of the observation.\\ 4858 lensObjSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced photometry.\\4859 lensObjSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced photometry.\\4860 lensObjSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced photometry.\\4861 lensObjSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced photometry.\\4862 lensObjSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced photometry.\\5023 lensObjSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from forced photometry.\\ 5024 lensObjSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from forced photometry.\\ 5025 lensObjSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from forced photometry.\\ 5026 lensObjSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from forced photometry.\\ 5027 lensObjSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from forced photometry.\\ 4863 5028 lensObjShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from forced photometry.\\ 4864 5029 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.\\ 4867 5032 lensObjShearE2 & - & REAL & -999 &K95 eq. (B12) shear polarizability e2 term from forced photometry.\\ 4868 lensPSFSmearX11 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced photometry.\\4869 lensPSFSmearX12 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced photometry.\\4870 lensPSFSmearX22 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced photometry.\\4871 lensPSFSmearE1 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced photometry.\\4872 lensPSFSmearE2 & $arcsec^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced photometry.\\5033 lensPSFSmearX11 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X11 term from PSF model for forced photometry.\\ 5034 lensPSFSmearX12 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X12 term from PSF model for forced photometry.\\ 5035 lensPSFSmearX22 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A11) smear polarizability X22 term from PSF model for forced photometry.\\ 5036 lensPSFSmearE1 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e1 term from PSF model for forced photometry.\\ 5037 lensPSFSmearE2 & arcsec$^{-2}$ & REAL & -999 &K95 eq. (A12) smear polarizability e2 term from PSF model for forced photometry.\\ 4873 5038 lensPSFShearX11 & - & REAL & -999 &K95 eq. (B11) shear polarizability X11 term from PSF model for forced photometry.\\ 4874 5039 lensPSFShearX12 & - & REAL & -999 &K95 eq. (B11) shear polarizability X12 term from PSF model for forced photometry.\\ … … 4888 5053 4889 5054 4890 \begin{table}[ b]5055 \begin{table}[htb] 4891 5056 \caption{ForcedWarpToImage: Contains the mapping of which input image comprises a particular \ippstage{warp} image used for forced photometry.} 4892 5057 \begin{center} … … 4898 5063 \hline 4899 5064 forcedWarpID & - & BIGINT & NA &Unique forced \ippstage{warp} identifier.\\ 4900 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 *frameID + ccdID).\\5065 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 $\times$ frameID + ccdID).\\ 4901 5066 \hline 4902 5067 \end{tabular} … … 4907 5072 % \subsection{Forced Galaxy Tables} 4908 5073 4909 \begin{table}[ b]4910 \caption{ForcedGalaxyShape: Contains the extended source galaxy shape parameters. All filters are matched into a single row. The positions, magnitudes, fluxes, and Sersicindices 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}).}5074 \begin{table}[htb] 5075 \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}).} 4911 5076 \begin{center} 4912 5077 %\resizebox{\textwidth}{!}{% … … 4932 5097 gGalMagErr & AB & REAL & -999 &Error in galaxy fit magnitude for g filter measurement.\\ 4933 5098 gGalPhi & degrees & REAL & -999 &Major axis position angle of the model fit for the g filter measurement.\\ 4934 gGalIndex & - & REAL & -999 & Sersicindex of the model fit for the g filter measurement.\\5099 gGalIndex & - & REAL & -999 &\Sersic\ index of the model fit for the g filter measurement.\\ 4935 5100 gGalFlags & - & SMALLINT & -999 &Analysis flags for the galaxy model chi-square fit (g filter measurement, values \\ 4936 5101 & & & & defined in ForcedGalaxyShapeFlags).\\ … … 4997 5162 \subsection{Tables Related to Difference Image Analysis} 4998 5163 4999 \begin{table}[ b]5164 \begin{table}[htb] 5000 5165 \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}.} 5001 5166 \begin{center} … … 5060 5225 % \subsection{Diff Detection Tables} 5061 5226 5062 \begin{table}[ b]5227 \begin{table}[htb] 5063 5228 \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.} 5064 5229 \begin{center} … … 5124 5289 \end{table}% 5125 5290 5126 \begin{table}[ b]5291 \begin{table}[htb] 5127 5292 \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.} 5128 5293 \begin{center} … … 5176 5341 DpsfChiSq & - & REAL & -999 &Reduced chi squared value of the PSF model fit.\\ 5177 5342 DpsfLikelihood & - & REAL & -999 &Likelihood that this detection is best fit by a PSF.\\ 5178 DmomentXX & $arcsec^2$ & REAL & -999 &Second moment $M_{xx}$.\\5179 DmomentXY & $arcsec^2$ & REAL & -999 &Second moment $M_{xy}$.\\5180 DmomentYY & $arcsec^2$ & REAL & -999 &Second moment $M_{yy}$.\\5343 DmomentXX & arcsec$^2$ & REAL & -999 &Second moment $M_{xx}$.\\ 5344 DmomentXY & arcsec$^2$ & REAL & -999 &Second moment $M_{xy}$.\\ 5345 DmomentYY & arcsec$^2$ & REAL & -999 &Second moment $M_{yy}$.\\ 5181 5346 DmomentR1 & arcsec & REAL & -999 &First radial moment.\\ 5182 DmomentRH & $arcsec^{0.5}$ & REAL & -999 &Half radial moment ($r^{0.5}$ weighting).\\5347 DmomentRH & arcsec$^{0.5}$ & REAL & -999 &Half radial moment ($r^{0.5}$ weighting).\\ 5183 5348 DapFlux & Jy & REAL & -999 &Aperture flux.\\ 5184 5349 DapFluxErr & Jy & REAL & -999 &Error in aperture flux.\\ … … 5200 5365 diffPosSN & - & REAL & -999 &Signal to noise of matching source in positive image.\\ 5201 5366 diffNegSN & - & REAL & -999 &Signal to noise of matching source in negative image.\\ 5202 Dsky & $Jy/arcsec^2$ & REAL & -999 &Background sky level.\\5203 DskyErr & $Jy/arcsec^2$ & REAL & -999 &Error in background sky level.\\5367 Dsky & Jy arcsec$^{-2}$ & REAL & -999 &Background sky level.\\ 5368 DskyErr & Jy arcsec$^{-2}$ & REAL & -999 &Error in background sky level.\\ 5204 5369 DinfoFlag & - & BIGINT & 0 &Information flag bitmask indicating details of the photometry. see DetectionFlags.\\ 5205 5370 DinfoFlag2 & - & INT & 0 &Information flag bitmask indicating details of the photometry. see DetectionFlags2.\\ … … 5213 5378 5214 5379 5215 \begin{table}[ b]5380 \begin{table}[htb] 5216 5381 \caption{DiffToImage: Contains the mapping of which input images were used to construct a particular difference image.} 5217 5382 \begin{center} … … 5223 5388 \hline 5224 5389 diffImageID & - & BIGINT & NA &Unique difference identifier.\\ 5225 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 *frameID + ccdID).\\5390 imageID & - & BIGINT & NA &Unique image identifier. Constructed as (100 $\times$ frameID + ccdID).\\ 5226 5391 \hline 5227 5392 \end{tabular} … … 5230 5395 \end{table}% 5231 5396 5232 \begin{table}[ b]5397 \begin{table}[htb] 5233 5398 \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.} 5234 5399 \begin{center} … … 5282 5447 system for objects). 5283 5448 5284 \begin{table}[ b]5449 \begin{table}[htb] 5285 5450 \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.} 5286 5451 \begin{center} … … 5347 5512 \end{table}% 5348 5513 5349 \begin{table}[ b]5514 \begin{table}[htb] 5350 5515 \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}.} 5351 5516 \begin{center} … … 5383 5548 \end{table}% 5384 5549 5385 \begin{table}[ b]5550 \begin{table}[htb] 5386 5551 \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}.} 5387 5552 \begin{center}
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