Index: trunk/doc/release.2015/systematics.20140411/Makefile =================================================================== --- trunk/doc/release.2015/systematics.20140411/Makefile (revision 40097) +++ trunk/doc/release.2015/systematics.20140411/Makefile (revision 40097) @@ -0,0 +1,41 @@ +# $Id: Makefile,v 1.16 2006-01-16 01:11:40 eugene Exp $ + +# WARNING : pdflatex does not do .ps +# +DO_PDFLATEX = 0 +DO_BIBTEX = 1 + +help: + @echo "USAGE: make (target)" + @echo " targets: all pdf tgz" + +all: pdf tgz +pdf: systematics.pdf +tgz: systematics.tgz + +# if you have PDF pics, they may need to be converted to EPS +PDFPICS = +# pics/peaks.pdf \ +# pics/FWHM.smooth.trend.ps1.pdf \ +# pics/moment.class.pdf \ +# pics/radial.profiles.pdf + +FILES = \ +../inputs/astro.sty \ +../inputs/code.sty \ +../inputs/apj.bst \ +../inputs/lib.bib \ +systematics.tex + +pics/%.pdf : pics/%.ps + echo $^ + echo $< + echo $@ + echo $* + ps2pdf -dEPSCrop $< $@ + +pdfpics: $(PDFPICS) +systematics.pdf: $(FILES) +systematics.tgz: $(FILES) + +include ../Makefile.Common Index: trunk/doc/release.2015/systematics.20140411/systematics.tex =================================================================== --- trunk/doc/release.2015/systematics.20140411/systematics.tex (revision 40096) +++ trunk/doc/release.2015/systematics.20140411/systematics.tex (revision 40097) @@ -7,6 +7,11 @@ %\documentclass[preprint2]{aastex} %\documentclass[preprint2,longabstract]{aastex} + +\RequirePackage{graphicx} \RequirePackage{color} +\RequirePackage{code} \input{astro.sty} + +\usepackage[T1]{fontenc}% (2) specify encoding % online version may use color, but print version needs b/w @@ -17,6 +22,6 @@ \def\plotext{ps} -%\def\picdir{/home/eugene/chipresid.20140404} -\def\picdir{/data/kukui.2/eugene/chipresid.20140404} +\def\picdir{/home/eugene/chipresid.20140404} +%\def\picdir{/data/kukui.2/eugene/chipresid.20140404} % Pick a terse version of the title here; @@ -108,5 +113,5 @@ The 1.8m Pan-STARRS\,1 telescope (PS1), located on the summit of Haleakala on the Hawaiian island of Maui, has been surveying the sky -regularly since May 2010 \citep{chambers.2017}. From May 2010 through +regularly since May 2010 \citep{chambers2017}. From May 2010 through March 2014, PS1 was run under the aegis of the Pan-STARRS Science Consortium to perform a set of wide-field science surveys; since March @@ -118,15 +123,20 @@ observations were distributed over five filters, \grizy, and have been astrometrically and photometrically calibrated to good precision -\citep{magnier.2017.calibration}. - -The wide-field PS1 telescope optics \citep{PS1.optics} image a 3.3 -degree field of view on a 1.4 gigapixel camera \citep[GPC1][]{PS1.GPC1}, with -low distortion and generally good image quality. The median seeing -for the \TPS\ data vary somewhat by filter, with (\grizy) = (XXXX). -Routine observations are conducted remotely from the Advanced -Technology Research Center in Kula, the main facility of the -University of Hawaii's Institute for Astronomy operations on Maui. - -GPC1 \citep{PS1.GPCA}, currently the largest astronomical camera in +\citep{magnier2017.calibration}. + +% 2004SPIE.5489..667H == PS1.optics +% 2008SPIE.7014E..0DO == PS1.GPCB +% 2009amos.confE..40T == PS1.GPCA +% 2012ApJ...756..158S == ubercal +The wide-field PS1 telescope optics \citep{2004SPIE.5489..667H} image +a 3.3 degree field of view on a 1.4 gigapixel camera +\citep[GPC1][]{2009amos.confE..40T}, with low distortion and generally +good image quality. The median seeing for the \TPS\ data vary +somewhat by filter, with (\grizy) = (XXXX). Routine observations are +conducted remotely from the Advanced Technology Research Center in +Kula, the main facility of the University of Hawaii's Institute for +Astronomy operations on Maui. + +GPC1 \citep{2009amos.confE..40T}, currently the largest astronomical camera in terms of number of pixels, consists of a mosaic of 60 edge-abutted $4800\times4800$ pixel detectors, with 10~$\mu$m pixels subtending @@ -135,12 +145,16 @@ readout time of 7 seconds for a full unbinned image. \note{details about the voltages?} Initial performance assessments are presented -in \cite{PS1.GPCB}. The active, usable pixels cover $\sim 80$\% of the +in \cite{2008SPIE.7014E..0DO}. The active, usable pixels cover $\sim 80$\% of the FOV. \subsection{Data Processing and Calibration} +% PS1_IPP = \bibitem[Magnier(2006)]{PS1.IPP} Magnier, E.\ 2006, +% Proceedings of The Advanced Maui Optical and Space Surveillance +% Technologies Conference, Ed.: S. Ryan, The Maui Economic Development +% Board, p.E5 + Images obtained by PS1 are processed by the Pan-STARRS Image -Processing Pipeline (IPP; \citealp{PS1_IPP, - magnier.etal.2016.datasystem}). All observations are processed +Processing Pipeline (IPP; \citealp{PS1_IPP,magnier2017.datasystem}). All observations are processed nightly, with results sent to groups within the science consortium (i.e., PS1SC during the \TPS) performing short-term science projects @@ -157,5 +171,5 @@ The data processing and calibration operations are discussed in detail in elsewhere -\citep{magnier.etal.2017.analysis,magnier.etal.2017.calibration,waters.2017}. +\citep{magnier2017.analysis,magnier2017.calibration,waters2017}. We re-visit here a number of points that are of significance to this study. Images are processed following a fairly standard sequence of @@ -168,5 +182,13 @@ the initial analysis steps. -As discussed in \cite{waters.2017}, image detrending includes +% Magnier.belgium: +% \bibitem[Magnier(2007)]{PS1.photometry} Magnier, E.\ 2007, The Future +% of Photometric, Spectrophotometric and Polarimetric Standardization, ASP Conference Series {\bf 364}, 153 + +%IPP astrometry (NOT USED) +% \bibitem[Magnier {\it et al.}(2008)]{PS1.astrometry} Magnier, E.~A., Liu, +% M., Monet, D.~G., \& Chambers, K.~C.\ 2008, IAU Symposium, {\bf 248}, 553 + +As discussed in \cite{waters2017}, image detrending includes flat-field processing with a single epoch flat-field image for each filter. The flat-field image used for this analysis has been @@ -180,5 +202,5 @@ factors which may make the flat-field image inconsistent with stellar photometry, e.g., SED, filter band-pass variations, etc -\citep[see][]{waters.2017,magnier.cuillandre,magnier.belgium}. This +\citep[see][]{waters2017,2004PASP..116..449M,magnier.belgium}. This correction was made on a relatively coarse grid across the focal plane in order to accumulate sufficient statistics from the stars in the @@ -192,5 +214,5 @@ Photometry of the PS1 images is performed using a point-spread-function (PSF) model as well as multiple kinds of -apertures \citep{magnier.etal.2017.analysis}. In this analysis, we +apertures \citep{magnier2017.analysis}. In this analysis, we refer to aperture photometry performed using an aperture defined based on the image quality observed for a given chip. The aperture diameter @@ -201,9 +223,9 @@ photometry is re-calibrated within the databasing system based on the properties of the measured photometry. The calibration process is -discussed by \cite{ubercal,photladder,magnier.etal.2017.calibration}. +discussed by \cite{2012ApJ...756..158S,2013ApJS..205...20M,magnier2017.calibration}. As part of this process, several flat-field corrections have been determined. For the PV2 analysis discussed here, a flat-field correction determined during the ubercal analysis -\citep[see][]{ubercal} consisted of an $8\times 8$ grid of corrections +\citep[see][]{2012ApJ...756..158S} consisted of an $8\times 8$ grid of corrections for each GPC1 chip and filter for each of 4 seasons. The boundaries of those seasons are \note{tentatively} identified with modifications @@ -218,7 +240,7 @@ brighter sources (using a non-linear fitting process) and from a simple centroid (1st moment) for the fainter source -\citep{magnier.etal.2017.analysis}. These position measurements are +\citep{magnier2017.analysis}. These position measurements are used in the astrometric analysis. The astrometric calibration is -discussed by \cite{magnier.etal.2017.calibration}; for the PV2 +discussed by \cite{magnier2017.calibration}; for the PV2 dataset, the typical systematic floor is \approx 15 - 20 milliarcsecond for individual measurements of brighter stars. @@ -428,4 +450,5 @@ \end{figure*} +% 2012ApJ...750...99T = Tonry et al PS1 phot system Figure~\ref{fig:flats.by.filter} shows the high-spatial-frequency structures in the flat-field images. For this measurement, we have @@ -434,5 +457,5 @@ then observed by the PS1 telescope. These flat-field images were obtained 2011 Feb 09 as part of a campaign to study the PS1 system -response \citep{tonry.phot}. Flats were obtain in a set of 4nm steps, +response \citep{2012ApJ...750...99T}. Flats were obtain in a set of 4nm steps, with \note{XXnm} band-pass. To enhance the signal-to-noise, we have median-combined a set of 6 flats at the center of the corresponding filter. @@ -511,5 +534,5 @@ objects is biased down by the weighting function, this is not quite the same as having $\sigma_{w} = 1.6$ times the true PSF $\sigma$, see -discussion in \citealt{magnier.etal.2017.analysis}). For each stellar +discussion in \citealt{magnier2017.analysis}). For each stellar detection, we extract the values $M_{xx,xy,yy} = \sum F_i w_i (x^2, x y, y^2) / \sum F_i w_i$. For each exposure, we find the mean second @@ -522,5 +545,5 @@ Using the second moment images, we can construct certain interesting -combinations, inspired by discussions of lensing measurements \citep{kaiser.1995}: +combinations, inspired by discussions of lensing measurements \citep{1995ApJ...449..460K}: \begin{eqnarray} R^2 & = & \delta M_{xx} + \delta M_{yy} \\ @@ -828,4 +851,26 @@ deviations are correlated with the radial derivative of the smearing. +\acknowledgments + +The Pan-STARRS1 Surveys (PS1) have been made possible through +contributions of the Institute for Astronomy, the University of +Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its +participating institutes, the Max Planck Institute for Astronomy, +Heidelberg and the Max Planck Institute for Extraterrestrial Physics, +Garching, The Johns Hopkins University, Durham University, the +University of Edinburgh, Queen's University Belfast, the +Harvard-Smithsonian Center for Astrophysics, the Las Cumbres +Observatory Global Telescope Network Incorporated, the National +Central University of Taiwan, the Space Telescope Science Institute, +the National Aeronautics and Space Administration under Grant +No. NNX08AR22G issued through the Planetary Science Division of the +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. + +\bibliographystyle{apj} +\bibliography{lib}{} +%\input{analysis.bbl} + \end{document}