Changeset 40728
- Timestamp:
- May 9, 2019, 2:37:59 PM (7 years ago)
- Location:
- trunk/doc/release.2015
- Files:
-
- 4 edited
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ps1.analysis/analysis.tex (modified) (18 diffs)
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ps1.calibration/calibration.tex (modified) (8 diffs)
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ps1.datasystem/datasystem.tex (modified) (2 diffs)
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ps1.detrend/detrend.tex (modified) (2 diffs)
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trunk/doc/release.2015/ps1.analysis/analysis.tex
r40719 r40728 59 59 % PS1 Builders 60 60 L. Denneau,\altaffilmark{\IfA} 61 P. Draper,\altaffilmark{\DUR}61 P.~W. Draper,\altaffilmark{\DUR} 62 62 R. Jedicke,\altaffilmark{\IfA} 63 63 K. W. Hodapp,\altaffilmark{\IfA} … … 103 103 104 104 % insert additional keywords as appropriate: 105 \keywords{ Surveys:\PSONE}105 \keywords{methods: data analysis -- Surveys:\PSONE -- techniques: image processing -- techniques: photometric} 106 106 107 107 \section{Introduction} … … 172 172 source detection and photometry, including point-spread-function and 173 173 extended source model fitting, and the techniques for ``forced'' 174 photometry measurements. The software describe here was used with a174 photometry measurements. The software described here was used with a 175 175 single consistent set of parameters for the complete PV3 analysis, 176 176 used for both DR1 and DR2. … … 332 332 333 333 Another variant of \ippprog{psphot} used in the PV3 analysis is called 334 \ippprog{psphotFullForce}. In this variant, a set of image all representing the334 \ippprog{psphotFullForce}. In this variant, a set of images all representing the 335 335 same pixels are processed together, with the positions of sources to 336 336 be analyzed loaded from a supplied file. In this variant of the … … 357 357 per image is combined with an error in the flat-field calibration and 358 358 an error in measuring the atmospheric effects. We have set a goal for 359 \ippprog{psphot} of 3 mmag photometric consistency for bright stars359 \ippprog{psphot} of 3 mmag photometric consistency for bright stars 360 360 between pairs of images obtained in photometric conditions at the same 361 361 pointing, ie to remove sensitivity to flat-field errors. This goal … … 367 367 individual measurements. The measurements from \ippprog{psphot} must 368 368 be sufficiently representative of the true source position to enable 369 astrometric calibration at the 10 mas level. The error in the369 astrometric calibration at the 10 mas level. The error in the 370 370 individual measurements will be folded together with the errors 371 371 introduced by the optical system, the effects of seeing, and by the 372 372 available reference catalogs. We have set a goal for \ippprog{psphot} 373 of 5 mas consistency between the true source postion and the measured373 of 5 mas consistency between the true source postion and the measured 374 374 position given reasonable PSF variations under simulations. This 375 375 level must be reached for images with 250 mas pixels, implying … … 379 379 pixel relative to the size of a chip (since a single data value is 380 380 used for X or Y). For the $4800^2$ GPC chips, this yields a limit of 381 about 0.25 m illiarcsecond.381 about 0.25 mas. 382 382 383 383 % \subsection{Software System Goals} … … 514 514 conditions which are identified by the analysis software. As part of 515 515 the output data for each detected source, two fields are provided 516 which encode these conditions as bit values in the two 32-bi n516 which encode these conditions as bit values in the two 32-bit 517 517 integers. The following two tables list the individual bit values in 518 518 these two fields. These informational and warning bits are described … … 827 827 \[ \chi^2 = \sum_{i,j} (F_{i,j} - f(x,y))^2 / \sigma_{i,j}^2 \] 828 828 829 By approximating the error per pixel as the error on just the peak,829 By approximating the error per pixel as the Poisson error on just the peak, 830 830 and pulling that term out of the above equation, and recognizing that 831 the values x,y in the 3x3grid centered on the peak pixel have values831 the values $X,Y$ in the $3 \times 3$ grid centered on the peak pixel have values 832 832 of only 0 or 1, we can greatly simplify the chi-square equation to a 833 833 square matrix equation with the following values: … … 860 860 \] 861 861 862 Inverting the 3x3matrix terms for $C_{00}$, $C_{20}$, and $C_{02}$,862 Inverting the $3 \times 3$ matrix terms for $C_{00}$, $C_{20}$, and $C_{02}$, 863 863 the location of the peak is determined from the minimum of the 864 864 bi-quadratic function above, and is given by: … … 983 983 simulated data. An image was generated with a PSF model matching the 984 984 radial profile of the PS1 PSF model with $\sigma_{\rm PSF}$ 985 corresponding to a FWHM of 1.4 arcseconds. As the window function 986 $\sigma_w$ is increased, the measured FWHM for the bright simulated 987 stars rises to meet the truth value. For small values of $\sigma_w$, 988 fainter stars are biased to low measured values of the FWHM. For 989 large values of $\sigma_w$, the faint stars are biased to higher 990 values and the scatter increases. We attempt to minimize the scatter 991 and trends with magnitude at the cost of overall bias. 985 corresponding to a FWHM of 1.4 arcseconds. For bright stars, as the 986 window function $\sigma_w$ is increased, the measured FWHM rises from 987 an initially under-estimated value to meet the truth value. For faint 988 stars, the measured value of the FWHM is initially under-estimated as 989 well. However, as the value of $\sigma_w$ increases, the measured 990 FWHM for faint stars rises, and then over-shoots the truth value, 991 while the scatter increases. Thus, for large values of $\sigma_w$, 992 the result is both a poorly estimated FWHM for the image and a trend 993 this the signal-to-noise of the star. We attempt to minimize the 994 scatter and trends with instrumental magnitude at the cost of overall 995 bias. 992 996 993 997 In a real image, we do not know the true value of the PSF size. If we … … 1575 1579 1576 1580 We attempt to measure the radial profile of sources in order to find 1577 the radius at which the flux of the source is matches the sky. In1578 this analysis, a series of up to 25 radial bins with power-law spacing 1579 are defined and the flux of the source in each annulus is measured. 1580 The``sky radius'' is defined to be the radius at which the (robust1581 the radius at which the flux of the source matches the sky. In this 1582 analysis, a series of up to 25 radial bins with power-law spacing are 1583 defined and the flux of the source in each annulus is measured. The 1584 ``sky radius'' is defined to be the radius at which the (robust 1581 1585 median) flux in the annulus is within 1 $\sigma$ of the local sky 1582 1586 level. If this limit is not reached before the slope of the flux from … … 1796 1800 flags the object with the bad bit \code{PM_SOURCE_MODE_FAIL}. It is 1797 1801 also possible in this type of case for the fit to result in a very low 1798 or negative value for the flux normalization parameter. Source for1802 or negative value for the flux normalization parameter. Sources for 1799 1803 which the peak is less than 0.02 are also marked as failing the 1800 1804 non-linear PSF fit (\code{PM_SOURCE_MODE_FAIL}). … … 1809 1813 the flag bit (\code{PM_SOURCE_MODE_POOR}). 1810 1814 1811 Sources which arepass the above tests are marked as having a valid1815 Sources which pass the above tests are marked as having a valid 1812 1816 non-linear PSF model fit with the flag bit 1813 1817 \code{PM_SOURCE_MODE_NONLINEAR_FIT}. Among these sources, those for … … 2198 2202 depend on the filter as follows: (\grizy) = (21.5, 21.5, 21.5, 20.5, 2199 2203 19.5). These values were chosen to have roughly similar 2200 signal-to-noise in a typical stack image for neutral color objects.2201 The magnitude limits for the Petrosian parameters were set to 25.0 for 2202 all filters, far below the detection limits and effectively not 2203 limiting the analysis based on apparent magnitude. For both galaxy 2204 model fits and Petrosian parameters, the Galactic latitude cut was 2205 defined by $|b| > b_{\rm min}$ where $b_{\rm min} = b_0 + r_b2204 signal-to-noise in a typical stack image for objects with colors of 2205 typical galaxies. The magnitude limits for the Petrosian parameters 2206 were set to 25.0 for all filters, far below the detection limits and 2207 effectively not limiting the analysis based on apparent magnitude. For 2208 both galaxy model fits and Petrosian parameters, the Galactic latitude 2209 cut was defined by $|b| > b_{\rm min}$ where $b_{\rm min} = b_0 + r_b 2206 2210 e^{\frac{-l^2}{2 \sigma_b^2}}$. For the PV3 analysis, $b_0 = 2207 2211 $20\degree, $r_b = $15\degree, $\sigma_b = $50\degree. This contour … … 2209 2213 the total time spent on the galaxy modeling analysis at the expense of 2210 2214 galaxy photometry in the plane (though Kron photometry is available 2211 for those sources). 2215 for those sources). 2212 2216 2213 2217 % galaxy model fits performed based on limits set in psphotChooseAnalysisOptions.c … … 2678 2682 profile galaxies, with a broader light distribution for the same 2679 2683 effective radius, are less likely to be detected for the same 2680 magnitude than DeVaucouleur profile galaxies. 2684 magnitude than DeVaucouleur profile galaxies. This completeness 2685 should be compared to our earlier work \citep{2013MNRAS.435.1825M} in 2686 which we injected a realistic population of simulated galaxies into 2687 real PS1 images. That work found that the 50\% completeness for the 2688 typical galaxy was roughly 0.5 magnitude brighter than the 50\% 2689 stellar completeness limit, somewhat fainter than the completeness 2690 shown in Figure~\ref{fig:galaxy.complete}. However, that previous 2691 work did not explore the depedency of the completeness on the galaxy 2692 size or profile. The difference suggests that the galaxies in the 2693 earlier work were generally compact. 2681 2694 2682 2695 % /data/kukui.1/eugene/galaxies.20190425/tap_psphot_galaxies.pro : go.bigtest.ckgalaxy … … 2894 2907 2895 2908 The KSB-style analysis of object ellipticities has also been used by 2896 several authors to search for margi ally-resolved binary stars2909 several authors to search for marginally-resolved binary stars 2897 2910 in wide-field imaging data. The use of the lensing statistics for 2898 2911 this application was described by \cite{2005ApJ...626.1070H} in the -
trunk/doc/release.2015/ps1.calibration/calibration.tex
r40722 r40728 21 21 %% NOTE: 2019 Feb versions of the figures are generated in /data/kukui.1/eugene/cal.paper.20190217 22 22 23 %\def\picdir{pics}24 \def\picdir{.}23 \def\picdir{pics} 24 %\def\picdir{.} 25 25 26 26 % Pick a terse version of the title here; … … 41 41 \def\MPIA{6} 42 42 \def\ARI{7} 43 \def\Princeton{8} 44 \def\DUR{9} 45 \def\CfA{10} 43 \def\STScI{8} 44 \def\JHU{9} 45 \def\Princeton{10} 46 \def\DUR{11} 47 \def\CfA{12} 46 48 47 49 % This example has a first author from UH: … … 54 56 S. R\"oser,\altaffilmark{\ARI} 55 57 E. Schilbach,\altaffilmark{\ARI} 58 S. Casertano,\altaffilmark{\STScI,\JHU} 56 59 K.~C. Chambers,\altaffilmark{\IfA} 57 60 H.~A. Flewelling,\altaffilmark{\IfA} … … 62 65 % PS1 Builders 63 66 L. Denneau,\altaffilmark{\IfA} 64 P. Draper,\altaffilmark{\DUR}67 P.~W. Draper,\altaffilmark{\DUR} 65 68 K. W. Hodapp,\altaffilmark{\IfA} 66 69 R. Jedicke,\altaffilmark{\IfA} … … 81 84 } % this bracket terminates author list 82 85 86 % The ordering here should be sequential, matching the sequence in the list of authors: 83 87 \altaffiltext{\IfA}{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822} 84 88 \altaffiltext{\LBL}{Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA} … … 88 92 \altaffiltext{\MPIA}{Max Planck Institute for Astronomy, K\"onigstuhl 17, D-69117 Heidelberg, Germany} 89 93 \altaffiltext{\ARI}{Astronomisches Rechen-Institut, Zentrum f\"ur Astronomie der Universit\"at Heidelberg, M\"ochhofstrasse 12-14, D-69120 Heidelberg, Germany} 94 \altaffiltext{\STScI}{Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA} 95 \altaffiltext{\JHU}{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA} 90 96 \altaffiltext{\Princeton}{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA} 91 97 \altaffiltext{\DUR}{Department of Physics, Durham University, South Road, Durham DH1 3LE, UK} 92 98 \altaffiltext{\CfA}{Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138} 93 94 % The ordering here should be sequential, matching the sequence in the list of authors:95 % \altaffiltext{\USNO}{US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001, USA}96 % \altaffiltext{\JHU}{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA}97 98 % \altaffiltext{\Strassborg}{99 99 100 100 \begin{abstract} … … 114 114 115 115 % insert additional keywords as appropriate: 116 \keywords{ Surveys:\PSONE}116 \keywords{astrometry -- methods: statistical -- proper motions -- Surveys:\PSONE -- techniques: photometric} 117 117 118 118 \section{Introduction}\label{sec:intro} … … 2966 2966 NASA Science Mission Directorate, the National Science Foundation 2967 2967 under Grant No. AST-1238877, the University of Maryland, and Eotvos 2968 Lorand University (ELTE) and the Los Alamos National Laboratory. 2969 Colormaps for Figures \ref{fig:photflat}, 2970 \ref{fig:allsky.photom.sigma}, \ref{fig:photom.pv3.3v4}, 2971 \ref{fig:astroflat.gri}, \ref{fig:astroflat.zy}, 2972 \ref{fig:allsky.astrom.sigma}, and \ref{fig:astroflat.repair} are 2973 based on the matplotlib ``magma'' colormap with additional guidance 2974 from Peter Kovesi's work \citep[Good Colour Maps: How to Design 2975 Them.][]{2015arXiv150903700K}. 2968 Lorand University (ELTE) and the Los Alamos National Laboratory. EAM 2969 is also supported for portions of this work by National Science 2970 Foundation Grant No. AST-1313455. Colormaps for Figures 2971 \ref{fig:photflat}, \ref{fig:allsky.photom.sigma}, 2972 \ref{fig:photom.pv3.3v4}, \ref{fig:astroflat.gri}, 2973 \ref{fig:astroflat.zy}, \ref{fig:allsky.astrom.sigma}, and 2974 \ref{fig:astroflat.repair} are based on the matplotlib ``magma'' 2975 colormap with additional guidance from Peter Kovesi's work \citep[Good 2976 Colour Maps: How to Design Them.][]{2015arXiv150903700K}. 2976 2977 2977 2978 \bibliographystyle{apj} -
trunk/doc/release.2015/ps1.datasystem/datasystem.tex
r40721 r40728 51 51 %PS Builder List 52 52 L. Denneau,\altaffilmark{\IfA} 53 P. Draper,\altaffilmark{\DUR}53 P.~W. Draper,\altaffilmark{\DUR} 54 54 K. W. Hodapp,\altaffilmark{\IfA} 55 55 R. Jedicke,\altaffilmark{\IfA} … … 98 98 99 99 % insert additional keywords as appropriate: 100 \keywords{Surveys:\PSONE 100 \keywords{Surveys:\PSONE; Methods: data analysis; Techniques: image processing} 101 101 102 102 \section{Introduction} -
trunk/doc/release.2015/ps1.detrend/detrend.tex
r40725 r40728 69 69 K.~C. Chambers,\altaffilmark{\IfA} 70 70 W.~S. Burgett,\altaffilmark{\IfA} 71 P. Draper,\altaffilmark{\DUR}71 P.~W. Draper,\altaffilmark{\DUR} 72 72 H.~A. Flewelling,\altaffilmark{\IfA} 73 73 K. W. Hodapp,\altaffilmark{\IfA} … … 125 125 126 126 % insert additional keywords as appropriate: 127 \keywords{Surveys:\PSONE }127 \keywords{Surveys:\PSONE; techniques: image processing; methods: data analysis; } 128 128 129 129 \section{Introduction}
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