Changeset 39866

Timestamp:

Dec 14, 2016, 8:37:01 PM (10 years ago)

Author:

eugene

Message:

moving lib.bib and apj.bst to common location in inputs; fix bibtex to point there

Location:

trunk/doc/release.2015

Files:

• Makefile.Common (modified) (2 diffs)
• inputs/apj.bst (moved) (moved from trunk/doc/release.2015/ps1.detrend/apj.bst )
• inputs/lib.bib (moved) (moved from trunk/doc/release.2015/ps1.detrend/lib.bib )
• ps1.analysis/analysis.tex (modified) (3 diffs)
• ps1.detrend/Makefile (modified) (3 diffs)

trunk/doc/release.2015/Makefile.Common

@@ -3 +3 @@
 PDFLATEX = env TEXINPUTS=.:..:inputs:../inputs:LaTeX:$(TEXINPUTS): pdflatex
 PSLATEX  = env TEXINPUTS=.:..:inputs:../inputs:LaTeX:$(TEXINPUTS): latex
+BIBTEX   = env BIBINPUTS=.:..:inputs:../inputs BSTINPUTS=.:..:inputs:../inputs bibtex
 
 PS2PDF_OPTS = "-dAutoFilterColorImages=false -dColorImageFilter=/FlateEncode"
@@ -8 +9 @@
 %.pdf: %.tex
         $(PSLATEX) $*.tex 
+        $(BIBTEX) $*
         $(PSLATEX) $*.tex 
 #       thumbpdf --modes=dvips $*.pdf

trunk/doc/release.2015/ps1.analysis/analysis.tex

@@ -86 +86 @@
 \begin{abstract}
 
-Lorem ipsum dolor sit amet, consectetur adipiscing elit. Vestibulum
-bibendum nisi id tristique posuere. Duis eu mollis nulla. Maecenas est
-turpis, mattis tempor urna vitae, placerat rhoncus sem. Lorem ipsum
-dolor sit amet, consectetur adipiscing elit. Sed quis velit
-nisl. Aliquam erat volutpat. Cras lacinia, nisl tristique auctor
-molestie, dolor nulla rhoncus purus, ac accumsan nunc nunc ac
-nibh. Maecenas vitae mollis mauris. Ut sollicitudin pulvinar purus,
-eget luctus lorem tincidunt vitae. Vestibulum eu mattis neque. Nulla
-in tortor id urna dapibus gravida a vel leo.
-
+Over 3 billion astronomical objects have been detected in the more
+than 22 million orthogonal transfer CCD images obtained as part of the
+Pan-STARRS\,1 $3\pi$ survey.  Over 85 billion instances of those
+objects have been automatically detected and characterized by the
+Pan-STARRS Image Processing Pipeline photometry software,
+\code{psphot}.  This fast, automatic, and reliable software was
+developed for the Pan-STARRS project, but is easily adaptable to
+images from other telescopes.  We describe the analysis of the
+astronomical objects by \code{psphot} in general as well as for the
+specific case of the 3rd processing version used for the first public
+release of the Pan-STARRS $3\pi$ survey data.
 \end{abstract}
 
@@ -103 +104 @@
 \section{INTRODUCTION}\label{sec:intro}
 
-The Pan-STARRS Image Processing Pipeline is responsible for the basic
-analysis of images from the Pan-STARRS telescopes Gigapixel Camera.
-The photometric and astrometric precision goals for the all-sky
-surveys, as well as the other survey components, are quite stringent:
-
-\begin{itemize}
-\item relative photometry: 10 millimagnitudes scatter for bright stars
-across the sky in the internal photometric system; 
-
-\item relative astrometry; 10 milliarcseconds scatter for individual
-stars between repeated images.
-
-\item absolute astrometry: 100 milliarcseconds scatter for all ICRS
-  reference stars (Tycho).
-\end{itemize}
-
-An additional constraint on the Pan-STARRS system comes from the high
-data rate.  PS1 produces typically $\sim 500$ exposures per night,
-corresponding to $\sim 750$ billion pixels of imaging data.  The
-images range from high galactic latitudes to the Galactic bulge, so
-large numbers of measurable stars can be expected in much of the data.
-The combination of the high precision goals of the astrometric and
-photometric measurements and the high data rate (and a finite
+This is the fourth in a series of seven papers describing the
+Pan-STARRS1 Surveys, the data reduction techiques and the resulting
+data products.  This paper (Paper IV) describes the details of the
+source detection and photometry, including point-spread-function and
+extended source fitting models, and the techniques for ``forced''
+photometry measurements.
+
+%Chambers et al. 2017 (Paper I)
+%The Pan-STARRS\,1 Surveys
+\citet[][Paper I]{chambers2017}
+provides an overview of the Pan-STARRS System, the design and
+execution of the Surveys, the resulting image and catalog data
+products, a discussion of the overall data quality and basic
+characteristics, and a brief summary of important results.
+
+%Magnier et al. 2017 (Paper II)
+%Pan-STARRS Data Processing Stages
+\citet[][Paper II]{magnier2017c}
+describes how the various data processing stages are organised and implemented
+in the Imaging Processing Pipeline (IPP), including details of the 
+the processing database which is a critical element in the IPP infrastructure . 
+
+%Waters et al. 2017 (Paper III) 
+%Pan-STARRS Pixel Processing : Detrending, Warping, Stacking
+\citet[][Paper III]{waters2017}
+describes the details of the pixel processing algorithms, including detrending, warping, and adding (to create stacked images) and subtracting (to create difference images) and resulting image products and their properties. 
+
+
+%Magnier et al. 2017 (Paper IV) 
+%Pan-STARRS Pixel Analysis : Source Detection 
+%\citet[][Paper IV]{magnier2017a}
+%describes the details of the source detection and photometry, including point-spread-function and extended source fitting models, and the techniques for ``forced" photometry measurements. 
+
+%Magnier et al. 2017 (Paper V) 
+%Pan-STARRS Photometric and Astrometric Calibration
+\citet[][Paper V]{magnier2017b}
+describes the final calibration process, and the resulting photometric and astrometric quality.  
+
+
+%Flewelling et al. 2017 (Paper VI)
+%Pan-STARRS 1 Database and Data Products
+\citet[][Paper VI]{flewelling2017}
+describes  the details of the resulting catalog data and its organization in the Pan-STARRS database. 
+%
+%
+\citet[][Paper VII]{huber2017}
+%Huber et al. 2017 (Paper VII)
+describes the Medium Deep Survey in detail, including the unique issues and data products specific to that survey. The Medium Deep Survey is not part of Data Release 1. (DR1) 
+
+%
+The Pan-STARRS1 filters and photometric system have already been
+described in detail in \cite{2012ApJ...750...99T}.
+
+The photometric and astrometric precision goals for the Pan-STARRS\,1
+surveys were quite stringent: photmetric accuracy of 10
+millimagnitudes, relative astrometric accuracy of 10 milliarcseconds
+and absolute astrometric accuracy of 100 milliarcseconds with respect
+to the ICRS reference stars.
+
+An additional constraint on the Pan-STARRS analysis system comes from
+the high data rate.  PS1 produces typically $\sim 500$ exposures per
+night, corresponding to $\sim 750$ billion pixels of imaging data.
+The images range from high galactic latitudes to the Galactic bulge,
+so large numbers of measurable stars can be expected in much of the
+data.  The combination of the high precision goals of the astrometric
+and photometric measurements and the high data rate (and a finite
 computing budget) mean that the process of detecting, classifying, and
 measuring the astronomical objects in the image data stream in a
@@ -1715 +1759 @@
 \end{verbatim}
 
+\bibliographystyle{apj}
+\bibliography{lib}{}
+
 \end{document}
 

trunk/doc/release.2015/ps1.detrend/Makefile

@@ -1 +1 @@
 # $Id: Makefile,v 1.16 2006-01-16 01:11:40 eugene Exp $
 PDFLATEX = env TEXINPUTS=.:..:inputs:./inputs:LaTeX:$(TEXINPUTS): pdflatex
+BIBTEX   = env BIBINPUTS=.:..:inputs:../inputs BSTINPUTS=.:..:inputs:../inputs bibtex
+
 help:
         @echo "USAGE: make (target)"
@@ -15 +17 @@
         rm -f detrend.aux detrend.bbl detrend.blg
         $(PDFLATEX) $<
-        bibtex detrend
+        $(BIBTEX) detrend
         $(PDFLATEX) $<
         $(PDFLATEX) $<
@@ -24 +26 @@
 include ../Makefile.Common
 
+FILES = \
+../inputs/astro.sty \
+../inputs/apj.bst \
+../inputs/lib.bib \
+detrend.tex \
+detrend.bbl \
+images/o5677g0123o_XY11_bt_trail.png \
+images/o5677g0124o_XY11_bt_trail.png \
+images/o5677g0123o_XY11_nobt.png \
+images/o5677g0124o_XY11_nobt.png \
+images/o5677g0123o_XY11_bt.png \
+images/o5677g0124o_XY11_bt.png \
+images/linearity_XY27_xy16.png \
+images/o5677g0123o_M_OS_NL_XY23_b1.jpg \
+images/o5677g0123o_to_DARK_XY23_b1.jpg \
+images/B_profile_ex.png \
+images/o5677g0123o_VIDEODARK_VDim_Rdark_XY22_b1.jpg \
+images/o5677g0123o_VIDEODARK_VDim_VDdark_XY22_b1.jpg \
+images/pattern_row_edit.png \
+images/o5379g0103o_XY57_nopat.png \
+images/o5379g0103o_XY57_pat.png \
+images/o5220g0025o_XY53_nofringe.png \
+images/o5220g0025o_XY53_fringe.png \
+images/gpc1_mask_indexed.png \
+images/full_fpa_ghosts.jpg \
+images/glint_example_o5379g0103o.jpg \
+images/o6802g0338o_XY51_b1.jpg \
+images/warp_1046511_sci.jpg \
+images/warp_1046511_mask.jpg \
+images/warp_1046511_wt.jpg \
+images/stack_3775944_sci.jpg \
+images/stack_3775944_mask.jpg \
+images/stack_3775944_wt.jpg \
+images/stack_3775944_num.jpg \
+images/stack_3775944_exp.jpg \
+images/stack_3775944_expwt.jpg
+
 submission : 
-        tar --transform 's%inputs/%%' -zcf waters2017.tgz detrend.tex detrend.bbl ../inputs/astro.sty images/o5677g0123o_XY11_bt_trail.png images/o5677g0124o_XY11_bt_trail.png images/o5677g0123o_XY11_nobt.png images/o5677g0124o_XY11_nobt.png images/o5677g0123o_XY11_bt.png images/o5677g0124o_XY11_bt.png images/linearity_XY27_xy16.png images/o5677g0123o_M_OS_NL_XY23_b1.jpg images/o5677g0123o_to_DARK_XY23_b1.jpg images/B_profile_ex.png images/o5677g0123o_VIDEODARK_VDim_Rdark_XY22_b1.jpg images/o5677g0123o_VIDEODARK_VDim_VDdark_XY22_b1.jpg images/pattern_row_edit.png images/o5379g0103o_XY57_nopat.png images/o5379g0103o_XY57_pat.png images/o5220g0025o_XY53_nofringe.png images/o5220g0025o_XY53_fringe.png images/gpc1_mask_indexed.png images/full_fpa_ghosts.jpg images/glint_example_o5379g0103o.jpg images/o6802g0338o_XY51_b1.jpg images/warp_1046511_sci.jpg images/warp_1046511_mask.jpg images/warp_1046511_wt.jpg images/stack_3775944_sci.jpg images/stack_3775944_mask.jpg images/stack_3775944_wt.jpg images/stack_3775944_num.jpg images/stack_3775944_exp.jpg images/stack_3775944_expwt.jpg
+        tar --transform 's%inputs/%%' -zcf waters2017.tgz $(FILES)