Index: trunk/doc/release.2015/ps1.analysis/analysis.tex =================================================================== --- trunk/doc/release.2015/ps1.analysis/analysis.tex (revision 39865) +++ trunk/doc/release.2015/ps1.analysis/analysis.tex (revision 39866) @@ -86,14 +86,15 @@ \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} @@ -103,27 +104,70 @@ \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 @@ -1715,4 +1759,7 @@ \end{verbatim} +\bibliographystyle{apj} +\bibliography{lib}{} + \end{document}