Changeset 40097 for trunk

Timestamp:

Jul 14, 2017, 6:27:03 AM (9 years ago)

Author:

eugene

Message:

convert to release Makefile model; update cites

Location:

trunk/doc/release.2015/systematics.20140411

Files:

• Makefile (added)
• systematics.tex (modified) (16 diffs)

trunk/doc/release.2015/systematics.20140411/systematics.tex

@@ -7 +7 @@
 %\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 +22 @@
 \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 +113 @@
 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 +123 @@
 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 +145 @@
 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 +171 @@
 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 +182 @@
 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 +202 @@
 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 +214 @@
 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 +223 @@
 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 +240 @@
 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 +450 @@
 \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 +457 @@
 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 +534 @@
 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 +545 @@
 
 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 +851 @@
 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}