Index: trunk/doc/release.2015/ps1.analysis/analysis.tex =================================================================== --- trunk/doc/release.2015/ps1.analysis/analysis.tex (revision 40727) +++ trunk/doc/release.2015/ps1.analysis/analysis.tex (revision 40728) @@ -59,5 +59,5 @@ % PS1 Builders L. Denneau,\altaffilmark{\IfA} -P. Draper,\altaffilmark{\DUR} +P.~W. Draper,\altaffilmark{\DUR} R. Jedicke,\altaffilmark{\IfA} K. W. Hodapp,\altaffilmark{\IfA} @@ -103,5 +103,5 @@ % insert additional keywords as appropriate: -\keywords{Surveys:\PSONE } +\keywords{methods: data analysis -- Surveys:\PSONE -- techniques: image processing -- techniques: photometric} \section{Introduction} @@ -172,5 +172,5 @@ source detection and photometry, including point-spread-function and extended source model fitting, and the techniques for ``forced'' -photometry measurements. The software describe here was used with a +photometry measurements. The software described here was used with a single consistent set of parameters for the complete PV3 analysis, used for both DR1 and DR2. @@ -332,5 +332,5 @@ Another variant of \ippprog{psphot} used in the PV3 analysis is called -\ippprog{psphotFullForce}. In this variant, a set of image all representing the +\ippprog{psphotFullForce}. In this variant, a set of images all representing the same pixels are processed together, with the positions of sources to be analyzed loaded from a supplied file. In this variant of the @@ -357,5 +357,5 @@ per image is combined with an error in the flat-field calibration and an error in measuring the atmospheric effects. We have set a goal for -\ippprog{psphot} of 3mmag photometric consistency for bright stars +\ippprog{psphot} of 3 mmag photometric consistency for bright stars between pairs of images obtained in photometric conditions at the same pointing, ie to remove sensitivity to flat-field errors. This goal @@ -367,9 +367,9 @@ individual measurements. The measurements from \ippprog{psphot} must be sufficiently representative of the true source position to enable -astrometric calibration at the 10mas level. The error in the +astrometric calibration at the 10 mas level. The error in the individual measurements will be folded together with the errors introduced by the optical system, the effects of seeing, and by the available reference catalogs. We have set a goal for \ippprog{psphot} -of 5mas consistency between the true source postion and the measured +of 5 mas consistency between the true source postion and the measured position given reasonable PSF variations under simulations. This level must be reached for images with 250 mas pixels, implying @@ -379,5 +379,5 @@ pixel relative to the size of a chip (since a single data value is used for X or Y). For the $4800^2$ GPC chips, this yields a limit of -about 0.25 milliarcsecond. +about 0.25 mas. % \subsection{Software System Goals} @@ -514,5 +514,5 @@ conditions which are identified by the analysis software. As part of the output data for each detected source, two fields are provided -which encode these conditions as bit values in the two 32-bin +which encode these conditions as bit values in the two 32-bit integers. The following two tables list the individual bit values in these two fields. These informational and warning bits are described @@ -827,7 +827,7 @@ \[ \chi^2 = \sum_{i,j} (F_{i,j} - f(x,y))^2 / \sigma_{i,j}^2 \] -By approximating the error per pixel as the error on just the peak, +By approximating the error per pixel as the Poisson error on just the peak, and pulling that term out of the above equation, and recognizing that -the values x,y in the 3x3 grid centered on the peak pixel have values +the values $X,Y$ in the $3 \times 3$ grid centered on the peak pixel have values of only 0 or 1, we can greatly simplify the chi-square equation to a square matrix equation with the following values: @@ -860,5 +860,5 @@ \] -Inverting the 3x3 matrix terms for $C_{00}$, $C_{20}$, and $C_{02}$, +Inverting the $3 \times 3$ matrix terms for $C_{00}$, $C_{20}$, and $C_{02}$, the location of the peak is determined from the minimum of the bi-quadratic function above, and is given by: @@ -983,11 +983,15 @@ simulated data. An image was generated with a PSF model matching the radial profile of the PS1 PSF model with $\sigma_{\rm PSF}$ -corresponding to a FWHM of 1.4 arcseconds. As the window function -$\sigma_w$ is increased, the measured FWHM for the bright simulated -stars rises to meet the truth value. For small values of $\sigma_w$, -fainter stars are biased to low measured values of the FWHM. For -large values of $\sigma_w$, the faint stars are biased to higher -values and the scatter increases. We attempt to minimize the scatter -and trends with magnitude at the cost of overall bias. +corresponding to a FWHM of 1.4 arcseconds. For bright stars, as the +window function $\sigma_w$ is increased, the measured FWHM rises from +an initially under-estimated value to meet the truth value. For faint +stars, the measured value of the FWHM is initially under-estimated as +well. However, as the value of $\sigma_w$ increases, the measured +FWHM for faint stars rises, and then over-shoots the truth value, +while the scatter increases. Thus, for large values of $\sigma_w$, +the result is both a poorly estimated FWHM for the image and a trend +this the signal-to-noise of the star. We attempt to minimize the +scatter and trends with instrumental magnitude at the cost of overall +bias. In a real image, we do not know the true value of the PSF size. If we @@ -1575,8 +1579,8 @@ We attempt to measure the radial profile of sources in order to find -the radius at which the flux of the source is matches the sky. In -this analysis, a series of up to 25 radial bins with power-law spacing -are defined and the flux of the source in each annulus is measured. -The ``sky radius'' is defined to be the radius at which the (robust +the radius at which the flux of the source matches the sky. In this +analysis, a series of up to 25 radial bins with power-law spacing are +defined and the flux of the source in each annulus is measured. The +``sky radius'' is defined to be the radius at which the (robust median) flux in the annulus is within 1 $\sigma$ of the local sky level. If this limit is not reached before the slope of the flux from @@ -1796,5 +1800,5 @@ flags the object with the bad bit \code{PM_SOURCE_MODE_FAIL}. It is also possible in this type of case for the fit to result in a very low -or negative value for the flux normalization parameter. Source for +or negative value for the flux normalization parameter. Sources for which the peak is less than 0.02 are also marked as failing the non-linear PSF fit (\code{PM_SOURCE_MODE_FAIL}). @@ -1809,5 +1813,5 @@ the flag bit (\code{PM_SOURCE_MODE_POOR}). -Sources which are pass the above tests are marked as having a valid +Sources which pass the above tests are marked as having a valid non-linear PSF model fit with the flag bit \code{PM_SOURCE_MODE_NONLINEAR_FIT}. Among these sources, those for @@ -2198,10 +2202,10 @@ depend on the filter as follows: (\grizy) = (21.5, 21.5, 21.5, 20.5, 19.5). These values were chosen to have roughly similar -signal-to-noise in a typical stack image for neutral color objects. -The magnitude limits for the Petrosian parameters were set to 25.0 for -all filters, far below the detection limits and effectively not -limiting the analysis based on apparent magnitude. For both galaxy -model fits and Petrosian parameters, the Galactic latitude cut was -defined by $|b| > b_{\rm min}$ where $b_{\rm min} = b_0 + r_b +signal-to-noise in a typical stack image for objects with colors of +typical galaxies. The magnitude limits for the Petrosian parameters +were set to 25.0 for all filters, far below the detection limits and +effectively not limiting the analysis based on apparent magnitude. For +both galaxy model fits and Petrosian parameters, the Galactic latitude +cut was defined by $|b| > b_{\rm min}$ where $b_{\rm min} = b_0 + r_b e^{\frac{-l^2}{2 \sigma_b^2}}$. For the PV3 analysis, $b_0 = $20\degree, $r_b = $15\degree, $\sigma_b = $50\degree. This contour @@ -2209,5 +2213,5 @@ the total time spent on the galaxy modeling analysis at the expense of galaxy photometry in the plane (though Kron photometry is available -for those sources). +for those sources). % galaxy model fits performed based on limits set in psphotChooseAnalysisOptions.c @@ -2678,5 +2682,14 @@ profile galaxies, with a broader light distribution for the same effective radius, are less likely to be detected for the same -magnitude than DeVaucouleur profile galaxies. +magnitude than DeVaucouleur profile galaxies. This completeness +should be compared to our earlier work \citep{2013MNRAS.435.1825M} in +which we injected a realistic population of simulated galaxies into +real PS1 images. That work found that the 50\% completeness for the +typical galaxy was roughly 0.5 magnitude brighter than the 50\% +stellar completeness limit, somewhat fainter than the completeness +shown in Figure~\ref{fig:galaxy.complete}. However, that previous +work did not explore the depedency of the completeness on the galaxy +size or profile. The difference suggests that the galaxies in the +earlier work were generally compact. % /data/kukui.1/eugene/galaxies.20190425/tap_psphot_galaxies.pro : go.bigtest.ckgalaxy @@ -2894,5 +2907,5 @@ The KSB-style analysis of object ellipticities has also been used by -several authors to search for margially-resolved binary stars +several authors to search for marginally-resolved binary stars in wide-field imaging data. The use of the lensing statistics for this application was described by \cite{2005ApJ...626.1070H} in the Index: trunk/doc/release.2015/ps1.calibration/calibration.tex =================================================================== --- trunk/doc/release.2015/ps1.calibration/calibration.tex (revision 40727) +++ trunk/doc/release.2015/ps1.calibration/calibration.tex (revision 40728) @@ -21,6 +21,6 @@ %% NOTE: 2019 Feb versions of the figures are generated in /data/kukui.1/eugene/cal.paper.20190217 -%\def\picdir{pics} -\def\picdir{.} +\def\picdir{pics} +%\def\picdir{.} % Pick a terse version of the title here; @@ -41,7 +41,9 @@ \def\MPIA{6} \def\ARI{7} -\def\Princeton{8} -\def\DUR{9} -\def\CfA{10} +\def\STScI{8} +\def\JHU{9} +\def\Princeton{10} +\def\DUR{11} +\def\CfA{12} % This example has a first author from UH: @@ -54,4 +56,5 @@ S. R\"oser,\altaffilmark{\ARI} E. Schilbach,\altaffilmark{\ARI} +S. Casertano,\altaffilmark{\STScI,\JHU} K.~C. Chambers,\altaffilmark{\IfA} H.~A. Flewelling,\altaffilmark{\IfA} @@ -62,5 +65,5 @@ % PS1 Builders L. Denneau,\altaffilmark{\IfA} -P. Draper,\altaffilmark{\DUR} +P.~W. Draper,\altaffilmark{\DUR} K. W. Hodapp,\altaffilmark{\IfA} R. Jedicke,\altaffilmark{\IfA} @@ -81,4 +84,5 @@ } % this bracket terminates author list +% The ordering here should be sequential, matching the sequence in the list of authors: \altaffiltext{\IfA}{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822} \altaffiltext{\LBL}{Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA} @@ -88,13 +92,9 @@ \altaffiltext{\MPIA}{Max Planck Institute for Astronomy, K\"onigstuhl 17, D-69117 Heidelberg, Germany} \altaffiltext{\ARI}{Astronomisches Rechen-Institut, Zentrum f\"ur Astronomie der Universit\"at Heidelberg, M\"ochhofstrasse 12-14, D-69120 Heidelberg, Germany} +\altaffiltext{\STScI}{Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA} +\altaffiltext{\JHU}{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA} \altaffiltext{\Princeton}{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA} \altaffiltext{\DUR}{Department of Physics, Durham University, South Road, Durham DH1 3LE, UK} \altaffiltext{\CfA}{Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138} - -% The ordering here should be sequential, matching the sequence in the list of authors: -% \altaffiltext{\USNO}{US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001, USA} -% \altaffiltext{\JHU}{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA} - -% \altaffiltext{\Strassborg}{ \begin{abstract} @@ -114,5 +114,5 @@ % insert additional keywords as appropriate: -\keywords{Surveys:\PSONE } +\keywords{astrometry -- methods: statistical -- proper motions -- Surveys:\PSONE -- techniques: photometric} \section{Introduction}\label{sec:intro} @@ -2966,12 +2966,13 @@ NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos -Lorand University (ELTE) and the Los Alamos National Laboratory. -Colormaps for Figures \ref{fig:photflat}, -\ref{fig:allsky.photom.sigma}, \ref{fig:photom.pv3.3v4}, -\ref{fig:astroflat.gri}, \ref{fig:astroflat.zy}, -\ref{fig:allsky.astrom.sigma}, and \ref{fig:astroflat.repair} are -based on the matplotlib ``magma'' colormap with additional guidance -from Peter Kovesi's work \citep[Good Colour Maps: How to Design - Them.][]{2015arXiv150903700K}. +Lorand University (ELTE) and the Los Alamos National Laboratory. EAM +is also supported for portions of this work by National Science +Foundation Grant No. AST-1313455. Colormaps for Figures +\ref{fig:photflat}, \ref{fig:allsky.photom.sigma}, +\ref{fig:photom.pv3.3v4}, \ref{fig:astroflat.gri}, +\ref{fig:astroflat.zy}, \ref{fig:allsky.astrom.sigma}, and +\ref{fig:astroflat.repair} are based on the matplotlib ``magma'' +colormap with additional guidance from Peter Kovesi's work \citep[Good + Colour Maps: How to Design Them.][]{2015arXiv150903700K}. \bibliographystyle{apj} Index: trunk/doc/release.2015/ps1.datasystem/datasystem.tex =================================================================== --- trunk/doc/release.2015/ps1.datasystem/datasystem.tex (revision 40727) +++ trunk/doc/release.2015/ps1.datasystem/datasystem.tex (revision 40728) @@ -51,5 +51,5 @@ %PS Builder List L. Denneau,\altaffilmark{\IfA} -P. Draper,\altaffilmark{\DUR} +P.~W. Draper,\altaffilmark{\DUR} K. W. Hodapp,\altaffilmark{\IfA} R. Jedicke,\altaffilmark{\IfA} @@ -98,5 +98,5 @@ % insert additional keywords as appropriate: -\keywords{Surveys:\PSONE } +\keywords{Surveys:\PSONE; Methods: data analysis; Techniques: image processing} \section{Introduction} Index: trunk/doc/release.2015/ps1.detrend/detrend.tex =================================================================== --- trunk/doc/release.2015/ps1.detrend/detrend.tex (revision 40727) +++ trunk/doc/release.2015/ps1.detrend/detrend.tex (revision 40728) @@ -69,5 +69,5 @@ K.~C. Chambers,\altaffilmark{\IfA} W.~S. Burgett,\altaffilmark{\IfA} -P. Draper,\altaffilmark{\DUR} +P.~W. Draper,\altaffilmark{\DUR} H.~A. Flewelling,\altaffilmark{\IfA} K. W. Hodapp,\altaffilmark{\IfA} @@ -125,5 +125,5 @@ % insert additional keywords as appropriate: -\keywords{Surveys:\PSONE } +\keywords{Surveys:\PSONE; techniques: image processing; methods: data analysis; } \section{Introduction}