Index: /trunk/doc/release.2015/ps1.mission/mission.tex =================================================================== --- /trunk/doc/release.2015/ps1.mission/mission.tex (revision 37893) +++ /trunk/doc/release.2015/ps1.mission/mission.tex (revision 37894) @@ -1,143 +1,530 @@ -\documentclass[iop,floatfix]{emulateapj} -% \pdfoutput=1 - -% see latex.readme.txt for notes on using the PS1 template -%\documentclass[12pt,preprint]{aastex} +% PS-1 Latex template v. 7.0 C. Stubbs June 14 2011 (with thanks to Tex-gurus Michael Wood-Vasey, Gautham Narayan, and Ryan Foley) +%Please send corrections or suggestions to stubbs-at-physics.harvard.edu +% +% This Latex template file is designed to be useful to PS-1 consortium authors. +% The authorship and publication policies of the project are available at +% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1SC_Publication_Policy +% +%The template assumes the AASTex style file, and the simple AAStex bibliography format. +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +% PS1 CONVENTIONS: +% +% Note there are some conventions to which Pan-STARRS1 papers should conform: +% The survey and the survey telescope/camera/software system are Pan-STARRS1, or PS1. +% The passbands are g_p1, r_p1, etc. and it's important to use these subscripted +% terms in order to clearly distinguish the PS1 photometric system from SDSS and +% other photometric systems that have similar names. Confusion will erupt if we are +% careful about this. We urge our colleagues to adopt the terms g_sn, r_sn, etc. +% for the comparable SDSS photometric system, under release DR. +% +% The MPC observatory code for PS1 is "F51" +% +% It is of utmost importance that we conform to the IAU object naming and designation standards. +% +% The IAU designation for any new PS1 objects is "PSO JDDD.DDDD+DD.DDDD" where the +% space between PSO and the subsequent string is mandatory, as is the inclusion of the "J" (which designates J2000). +% Any shortened names, such as PSO JDDD.D-DDDD must contain the J! +% This also means coordinates in names are *truncated* rather than rounded, to x.xxxx significance in RA and x.xxxx in Dec. +% Coordinates are reported in decimal degrees (J2000) for both RA and DEC, the four digits provides for 0.2" accuracy that +% has been chosen to both exploit the absolute coordinate accuracy and to prevent confusion other than PSF blending. +% The optional is a single ASCII character that designates "child" objects derived from some primary object. This might include, for, example, +% the QSO at the center of a galaxy, or if the QSO was declared first, the galaxy underneath it. Note that the 14 characters (ignoring +% decimal point, but including "+" and "-", are intended to be part of a 64-bit integer, with the last byte reserved for the "x" character +% in order to provide efficient hashing and searching for applications. +% +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +% CHECKLIST: +% +% Here is a partial checklist for PS1 paper authors (detailed instructions at http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1SC_Publication_Policy): +% - post intended project to the appropriate Key Project wiki site, and send email to KP leads and to science_council@ps1sc.org +% - ensure that magnitudes are in g_p1, etc designation +% - check to see if your objects already have a PSO designation and if so, be sure to use it! We don't want two names for the same object! +% - ensure that any new objects have designations that conform to the IAU standard. See above. +% - double-check the author list and institutional affiliations. +% - get the most recent builder list from http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Builders_aastex. Update as needed. What's listed here is OK as of 6/14/11. +% - enter short title and short authors in appropriate place below +% - conform to journal-specific guidelines +% - Are PS1 system papers cited, as appropriate? Is relevant prior work cited (not just yours!) ? Copies of the system technical papers are available at +% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Publications +% - If the objects in your paper are likely to end up in an external database such as SIMBAD or NED, you can include an \object {} tag. Decide on this early, +% because you need to send off the objects to SIMBAD or NED so the journal can verify prior to publication. More and more journals are doing this, +% but not all. The Table example below has an illustration of this. +% - post paper draft to PS1SC through the consortium web site, at http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Publications +% - then send email to scientists@ps1sc.org announcing that draft is available, soliciting comments. Paper is still embargoed within PS1SC. +% - inform PS1 builders of the paper by sending email to builders@ps1sc.org, only positive affirmation implies inclusion. +% - decide if your project merits a press release. If so, coordinate with Ken Chambers and Gareth Winn-Williams and others as appropriate. +% standard phrasing for inclusion in Press Releases is at http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/Acknowledgment_for_PR +% - after a 3 week interval, window for comments has closed. Any builders who did not explicitly request inclusion can be dropped. +% - Revise as needed. +% - In coordination with Key Project leadership, submit the paper. +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +% +% This template has some Latex terms defined for your convenience, in the block below. +% +% Use trailing slash command after each of these to insert a space! +% +\documentclass[12pt,preprint]{aastex} %\documentclass[manuscript]{aastex} %\documentclass[preprint2]{aastex} %\documentclass[preprint2,longabstract]{aastex} -\RequirePackage{color} -\input{astro.sty} - -% online version may use color, but print version needs b/w -\def\plotmode{col} -%\def\plotmode{bw} - -% arxiv needs PDF graphics, but publishers mostly was PS -%\def\plotext{pdf} -\def\plotext{ps} - -% use this to make the figure picture path flexible: -%\def\picdir{PATH} -\def\picdir{ALTPATH} +\newcommand{\gps}{\ensuremath{g_{\rm P1}}} +\newcommand{\rps}{\ensuremath{r_{\rm P1}}} +\newcommand{\ips}{\ensuremath{i_{\rm P1}}} +\newcommand{\zps}{\ensuremath{z_{\rm P1}}} +\newcommand{\yps}{\ensuremath{y_{\rm P1}}} +\newcommand{\wps}{\ensuremath{w_{\rm P1}}} +\newcommand{\grizy}{\gps\rps\ips\zps\yps} +\newcommand{\PS}{\protect \hbox {Pan-STARRS1}} % Pick a terse version of the title here; -\shorttitle{PS1 Science Surveys} -\shortauthors{K.C. Chambers et al} +\shorttitle{Pan-STARRS Aliens} +\shortauthors{U.H. Author et al} \begin{document} -\title{The Pan-STARRS\,1 Science Surveys} - -% this is a crude trick to get the order of affiliations right. These -% names are used in the affiliations below. The user needs to (1) set -% the order and numbers to have the correct sequence in the author -% list and (2) re-order the list at the bottom (and comment-out as needed) -\def\IfA{1} -\def\CfA{2} -\def\MPIA{3} -\def\Princeton{3} -\def\USNO{4} -\def\JHU{1} - +\title{A Latex Template for the Production of Pan-STARRS1 Papers} +% +% PS1 paper authorship lists major paper contributors, followed by alphabetical list of PS1 builders, +% You'll want to shuffle the affiliation designations as needed. PS1 institutional addresses are +% provided below. Look here to get the most up-to-date list of builders and their institutional affiliations: +% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Builders_aastex +% +% Note that any authors not from PS-1 institutions, that is not a PS1 builder, needs to secure external +% scientist status. Information on that process is available at +% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/Pending_External_Scientists +% +% This example has a first author from UH: \author{ -K.~C. Chambers,\altaffilmark{\IfA} -IPP Team, -%PS Builder List -% W.~S. Burgett,\altaffilmark{\IfA} -% K.~C. Chambers,\altaffilmark{\IfA} -% L. Denneau,\altaffilmark{\IfA} -% P. Draper,\altaffilmark{\DUR} -% H.~A. Flewelling,\altaffilmark{\IfA} -% T. Grav,\altaffilmark{\IfA} -% J. N. Heasley,\altaffilmark{\IfA} -% K. W. Hodapp,\altaffilmark{\IfA} -% M. E. Huber,\altaffilmark{\IfA} -% R. Jedicke,\altaffilmark{\IfA} -% N. Kaiser,\altaffilmark{\IfA} -% R.-P. Kudritzki,\altaffilmark{\IfA} -% G. A. Luppino,\altaffilmark{\IfA} -% R. H. Lupton,\altaffilmark{\Princeton} -% E. A. Magnier,\altaffilmark{\IfA} -% N. Metcalfe,\altaffilmark{\DUH} -% D. G. Monet,\altaffilmark{\USNO} -% J.~S. Morgan,\altaffilmark{\IfA} -% P. M. Onaka,\altaffilmark{\IfA} -% P.~A. Price,\altaffilmark{\Princeton} -% C.~W. Stubbs,\altaffilmark{\CfA} -% W.~E. Sweeney,\altaffilmark{\IfA} -% J.~L. Tonry, \altaffilmark{\IfA} -% R. J. Wainscoat,\altaffilmark{\IfA} and -% C. Z. Waters,\altaffilmark{\IfA} -} % this bracket terminates author list +U.H.Firstauthor,\altaffilmark{1} +I.M. Anauthor,\altaffilmark{2} +M.E. Too,\altaffilmark{3} +%PS Builder List, delete or comment out as needed if any appear above this line. Affiliation numbers will likely need to be shuffled +% here and correspondingly in the institution list below +% List updated by S. Smartt 2013-04-30 and 2013-06-25, after Board approval of additional Builders. Now matches +%http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Builders_aastex + +W. S. Burgett\altaffilmark{1}, +K. C. Chambers\altaffilmark{1}, +L. Denneau\altaffilmark{1}, +P. Draper\altaffilmark{4}, +H. Flewelling\altaffilmark{1}, +T. Grav\altaffilmark{5}, +J. N. Heasley\altaffilmark{1}, +K. W. Hodapp\altaffilmark{1}, +M. E. Huber\altaffilmark{1}, +R. Jedicke\altaffilmark{1}, +N. Kaiser\altaffilmark{1}, +R.-P. Kudritzki\altaffilmark{1}, +G. A. Luppino\altaffilmark{1}, +R. H. Lupton\altaffilmark{6}, +E. A. Magnier\altaffilmark{1}, +N. Metcalfe\altaffilmark{2}, +D. G. Monet\altaffilmark{7}, +J. S. Morgan\altaffilmark{1}, +P. M. Onaka\altaffilmark{1}, +P. A. Price\altaffilmark{1}, +C. W. Stubbs\altaffilmark{8}, +W. Sweeney\altaffilmark{1}, +J. L. Tonry\altaffilmark{1}, +R. J. Wainscoat\altaffilmark{1}. +C. Waters\altaffilmark{1}, + +% this bracket terminates author list +} % The ordering here should be sequential, matching the sequence in the list of authors: -\altaffiltext{\IfA}{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822} -% \altaffiltext{\CfA}{Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138} -% \altaffiltext{\Princeton}{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA} -% \altaffiltext{\USNO}{US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001, USA} -% \altaffiltext{\DUH}{Durham, UK} -% \altaffiltext{\JHU}{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA} -% \altaffiltext{\MPIA}{Max Planck Institute for Astronomy, K\"onigstuhl 17, D-69117 Heidelberg, Germany} +\altaffiltext{1}{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822} +\altaffiltext{2}{Another most excellent PS1 partner institution, copy from list below} +\altaffiltext{3}{Another most excellent PS1 partner institution, copy from list below} +\altaffiltext{4}{Department of Physics, Durham University, South Road, Durham DH1 3LE, UK} +\altaffiltext{5}{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA} +\altaffiltext{6}{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA} +\altaffiltext{7}{US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001, USA} +\altaffiltext{8}{Department of Physics, Harvard University, Cambridge, MA 02138, USA} + + +% Here is a list of PS-1 Institution addresses, for inclusion above. send corrections to stubbs-at-physics.harvard.edu +% +%{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822} +%{Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138} +%{Department of Physics, Harvard University, 17 Oxford Street, Cambridge MA 02138} +%{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA} +%{Astrophysics Research Centre, School of Mathematics and Physics, QueenÕs University Belfast, Belfast, BT71NN, UK} +%{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA} +%{US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001, USA} +%{Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, Postfach 1312, 85741 Garching, Germany} +%{Max Planck Institute for Astronomy, Kšnigstuhl 17, D-69117 Heidelberg, Germany} +%{Astrophysics Research Centre, School of Mathematics and Physics, QueenÕs University Belfast, Belfast, BT7 1NN, UK} +%{Department of Physics. University of Durham Science Laboratories, South Road Durham DH1 3LE, UK} +%{Las Cumbres Observatory Global Telescope Network, Inc.,6740 Cortona Dr. Suite 102 Santa Barbara CA 93117, USA} + %{National Central University, 300 Jhongda Rd, Jhongli 32001, Taiwan } +%{SUPA, Institute for Astronomy, University of Edinburgh, Edinburgh, EH9 3HJ, UK} +%{Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA} +% +% Don't use our macros in the abstract, likely won't work right in arXiv server? \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. - +The Pan-STARRS1 survey has obtained multi-epoch imaging in 5 bands (\grizy) over +the entire sky North of declination $-$30, and we have done good things with the results. +We have detected thousands of alien civilizations, some with measurable proper motions. +They are headed towards us. \end{abstract} % insert additional keywords as appropriate: -\keywords{Surveys:\PSONE } - -\section{OUTLINE} -\begin{verbatim} -* Introduction - * Previous similar surveys - * POSS - * SDSS - * 2MASS - * Science Drivers - * Initial Proposal (PS4) -* PS1 Observatory Description - * PS1 Telescope Description - * Physical Characteristics - * Construction - * GPC1 camera -* PS1 Surveys - * 3PI - * MD - * Solar System - * STS - * M31 -* Data Quality - * Image Quality - * Observing Efficiency - * -* Science Key Projects -* Data Release -\end{verbatim} - -\section{INTRODUCTION}\label{sec:intro} - -\section{Pan-STARRS1} - -\section{PS1 Observatory Description} - -\section{PS1 Science Surveys} - -\section{Data Quality / Data Metrics?} - -\section{Science Key Projects} - -\section{Data Release} - -\section{Discussion} - -\section{Conclusion} +\keywords{Surveys:\PS } + +\vfil +\eject +\clearpage + +\section{INTRODUCTION} +\label{sec:intro} + +We present our most excellent results from \PS. + +% Note trailing slash after shorthand commands to force an appropriate space, when needed. + +The remainder of the introduction summarizes the \PS\ survey system. The observations we used are described in Section +\ref{sec:observations}. Data processing is outlined in Section \ref{sec:processing}, +and results are shown in Section \ref{sec:results}, followed by our conclusions and discussion in Section \ref{sec:discussion}. + +%%%%%%%%%%%%%%%%%%%%%%% +% Boilerplate system description begins here. This is presented to save PS1 authors some time, keep/modify as much of this as you +% think appropriate. Or write your own... You can download the PS1 technical papers from +% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Publications +% (see the bottom of the wiki page). + +\subsection{The Pan-STARRS1 Telescope, Camera, and Image Processing} + +The Pan-STARRS1 system is a high-etendue wide-field imaging system, designed for dedicated survey observations. The system +is installed on the peak of Haleakala on the island of Maui in the Hawaiian island chain. Routine observations are conducted remotely, +from the Waiakoa Laboratory in Pukalani. We provide below a terse summary of the Pan-STARRS1 survey instrumentation. +A more complete description of the Pan-STARRS1 system, both hardware and software, is provided by \cite{PS1_system}. The +survey philosophy and execution strategy are described in \cite{PS_MDRM}. + +The Pan-STARRS1 optical design \citep{PS1_optics} uses a 1.8~meter diameter $f$/4.4 primary mirror, and a 0.9~m secondary. +The resulting converging beam then passes through two refractive correctors, an +interference filter with a clear aperture diameter of 496 mm, and a final refractive corrector that is the +dewar window. The telescope illuminates a diameter of 3.3 degrees, with low distortion, +with some vignetting at the edges of this illuminated region. +The Pan-STARRS1 imager \citep{PS1_GPCA} comprises a total of 60 $4800\times4800$ pixel detectors, with 10~$\mu$m pixels that subtend 0.258~arcsec. +The detectors are back-illuminated CCDs manufactured by Lincoln Laboratory. The detectors are read out using a StarGrasp CCD controller, +with a readout time of 7 seconds for a full unbinned image. Initial performance assessments are presented in \cite{PS1_GPCB}. + +%note trailing slash command where space required after passband macros +The \PS\ observations are obtained through a set of five broadband +filters, which we have designated as \gps, \rps, \ips, \zps, and +\yps. Under certain circumstances \PS\ observations are obtained with +a sixth, ``wide'' filter designated as \wps\ that essentially spans +\gps, \rps, and \ips. Although the filter system for \PS\ has much in +common with that used in previous surveys, such as SDSS \citep{SDSS}, there +are important differences. The \gps\ filter extends 20~nm redward of +$g_{SDSS}$, paying the price of 5577\AA\ sky emission for greater +sensitivity and lower systematics for photometric redshifts, and the +\zps\ filter is cut off at 930~nm, giving it a different response than +the detector response defined $z_{SDSS}$. SDSS has no corresponding +\yps\ filter. Further information on the passband shapes is described +in \cite{PS_lasercal}. +Provisional response +functions (including 1.3 airmasses of atmosphere) are available +at the project's web site \footnote[1]{http://svn.pan-starrs.ifa.hawaii.edu/trac/ipp/wiki/PS1\_Photometric\_System}. Photometry is in the ``natural'' \PS\ +system, $m=-2.5log(flux)+m'$, with a single zeropoint adjustment $m'$ made in each band to conform to the AB magnitude scale \citep{JTphoto}. +\PS\ magnitudes are interpreted as being at the top of the atmosphere, with 1.3 airmasses of atmospheric attenuation being included in the +system response function. No correction for Galactic extinction is applied to the \PS\ magnitudes. +We stress that, like SDSS, \PS\ uses the AB +photometric system and there is no arbitrariness in the definition. Flux representations are limited +only by how accurately we know the system response function vs. wavelength. + +Images obtained by the Pan-STARRS1 system are processed through the Image Processing Pipeline (IPP) \citep{PS1_IPP}, +on a computer cluster at the Maui High Performance Computer Center. The pipeline runs the images through a succession of stages, +including flat-fielding (``de-trending''), a flux-conserving warping to a sky-based image plane, masking and artifact removal, and object detection and +photometry. The IPP also performs image subtraction to allow for the prompt detection of variables and transient phenomena. Mask and variance arrays +are carried forward at each stage of the IPP processing. Photometric and astrometric measurements performed by the IPP system are described in \cite{PS1_photometry} +and \cite{PS1_astrometry} respectively. + +The details of the photometric calibration and the \PS\ zeropoint +scale will be presented in a subsequent publication \citep{JTphoto}, +and \cite{EMphoto} will provide the application to a consistent +photometric catalog over the 3/4 sky observed by \PS. + +% Boilerplate system description ends here. +%%%%%%%%%%%%%%%%%%% + +\section{OBSERVATIONS} +\label{sec:observations} + +% define which set of PS1 observations went into your paper. +This paper uses images and photometry from the Pan-STARRS1 Medium-Deep Field survey. In addition +to covering the sky at $\delta>-30\deg$ in 5 bands, +the Pan-STARRS1 survey has obtained deeper multi-epoch images in the PS1 \gps, \rps, \ips, \zps\ and \yps\ bands of the +fields listed in Table \ref{table:fields}. The typical Medium-deep cadence of observations is presented in Table \ref{table:cadence}, +and the 5 $\sigma$ point source detection limits achieved in the various \grizy\ bands, as well as other statistics of +potential interest, are presented in Table \ref{table:depths}, for +the co-added stacks over the observing period presented here. + +% This is an illustration of a simple Table. The coordinates of the Medium-Deep fields are correct, and +% are the actual telescope boresight pointings and supersede any prior list.PS1 uses decimal degrees (J2000) for +% both RA and DEC. + +\begin{table}[htdp] +\caption{\PS\ Medium-Deep Field Centers. } +\begin{center} +\begin{tabular}{lrr} +\hline +\hline +{\bf Field} & {\bf RA (degrees, J2000)} & {\bf Dec (degrees, J2000)} \\ +\hline +MD00 & 10.675 & $ 41.267$ \\ +MD01 & 35.875 & $ -4.250$ \\ +MD02 & 53.100 & $-27.800$ \\ +MD03 & 130.592 & $ 44.317$ \\ +MD04 & 150.000 & $ 2.200$ \\ +MD05 & 161.917 & $ 58.083$ \\ +MD06 & 185.000 & $ 47.117$ \\ +MD07 & 213.704 & $ 53.083$ \\ +MD08 & 242.787 & $ 54.950$ \\ +MD09 & 334.188 & $ 0.283$ \\ +MD10 & 352.312 & $ -0.433$ \\ +MD11 & 270.000 & $ 66.561$ \\ +\hline +\end{tabular} +\end{center} +\label{table:fields} +\end{table} + + +\begin{table}[htdp] +\caption{\PS\ Medium-Deep Survey, typical cadence. FM$\pm$3 designates 3 nights on either side of Full Moon.} +\begin{center} +\begin{tabular}{ccr} +\hline +\hline +{\bf Night} & {\bf Filter} & {\bf Exposure Time} \\ +\hline +1 & \gps \& \rps & 8$\times$113s each\\ +2 & \ips & 8$\times$240s \\ +3 & \zps & 8$\times$240s \\ +4 & \gps \& \rps & 8$\times$113s each \\ +repeats... & \nodata & \nodata \\ +FM$\pm3$ & \yps & 8$\times$240s \\ +\hline +\end{tabular} +\end{center} +\label{table:cadence} +\end{table} + +% These are the detection limits for Medium-Deep analysis done by Tonry as of May 31, 2011. +\begin{table}[htdp] +\caption{\PS\ MDF Statistics, Apr 2009--Apr 2011.} +\begin{center} +\begin{tabular}{lcrcccclcrcccc} +\hline +\hline +Field&Filter& $N$ & $\log t$ & $PSF$ & $\langle w\rangle$ & $m_{lim}$ & +Field&Filter& $N$ & $\log t$ & $PSF$ & $\langle w\rangle$ & $m_{lim}$\\ +\hline +MD01 & g & 42 & 4.7 & 1.25 & 1.55 & 24.5 & MD06 & g & 38 & 4.6 & 1.25 & 1.56 & 24.4\\ +MD01 & r & 42 & 4.7 & 1.15 & 1.35 & 24.4 & MD06 & r & 39 & 4.6 & 1.18 & 1.45 & 24.2\\ +MD01 & i & 41 & 4.9 & 1.05 & 1.27 & 24.4 & MD06 & i & 41 & 4.9 & 1.14 & 1.39 & 24.3\\ +MD01 & z & 41 & 4.9 & 1.03 & 1.24 & 23.9 & MD06 & z & 38 & 4.9 & 1.05 & 1.30 & 23.7\\ +MD01 & y & 21 & 4.6 & 0.95 & 1.17 & 22.4 & MD06 & y & 24 & 4.7 & 1.00 & 1.25 & 22.4\\ +MD02 & g & 30 & 4.5 & 1.31 & 1.79 & 24.2 & MD07 & g & 36 & 4.5 & 1.23 & 1.68 & 24.3\\ +MD02 & r & 29 & 4.5 & 1.20 & 1.74 & 24.1 & MD07 & r & 39 & 4.5 & 1.13 & 1.46 & 24.2\\ +MD02 & i & 30 & 4.8 & 1.11 & 1.50 & 24.2 & MD07 & i & 39 & 4.9 & 1.14 & 1.44 & 24.2\\ +MD02 & z & 33 & 4.8 & 1.06 & 1.30 & 23.6 & MD07 & z & 43 & 4.9 & 1.08 & 1.37 & 23.7\\ +MD02 & y & 16 & 4.5 & 1.14 & 1.42 & 22.1 & MD07 & y & 30 & 4.8 & 1.01 & 1.28 & 22.5\\ +MD03 & g & 38 & 4.6 & 1.18 & 1.44 & 24.5 & MD08 & g & 38 & 4.5 & 1.27 & 1.68 & 24.3\\ +MD03 & r & 37 & 4.6 & 1.09 & 1.28 & 24.4 & MD08 & r & 38 & 4.5 & 1.14 & 1.47 & 24.2\\ +MD03 & i & 41 & 4.9 & 1.06 & 1.31 & 24.4 & MD08 & i & 33 & 4.8 & 1.07 & 1.34 & 24.2\\ +MD03 & z & 42 & 5.0 & 1.03 & 1.27 & 23.9 & MD08 & z & 40 & 4.9 & 1.09 & 1.39 & 23.7\\ +MD03 & y & 20 & 4.6 & 1.00 & 1.36 & 22.4 & MD08 & y & 32 & 4.9 & 0.98 & 1.27 & 22.7\\ +MD04 & g & 35 & 4.6 & 1.17 & 1.52 & 24.5 & MD09 & g & 34 & 4.5 & 1.26 & 1.55 & 24.3\\ +MD04 & r & 37 & 4.6 & 1.09 & 1.46 & 24.3 & MD09 & r & 33 & 4.5 & 1.15 & 1.42 & 24.1\\ +MD04 & i & 35 & 4.9 & 1.07 & 1.35 & 24.3 & MD09 & i & 34 & 4.8 & 1.02 & 1.36 & 24.3\\ +MD04 & z & 28 & 4.8 & 1.03 & 1.32 & 23.6 & MD09 & z & 34 & 4.8 & 1.02 & 1.26 & 23.7\\ +MD04 & y & 8 & 4.3 & 1.03 & 1.21 & 22.0 & MD09 & y & 12 & 4.3 & 0.94 & 1.12 & 22.0\\ +MD05 & g & 42 & 4.6 & 1.24 & 1.58 & 24.4 & MD10 & g & 30 & 4.5 & 1.26 & 1.60 & 24.2\\ +MD05 & r & 40 & 4.6 & 1.17 & 1.46 & 24.3 & MD10 & r & 33 & 4.5 & 1.18 & 1.53 & 24.2\\ +MD05 & i & 34 & 4.8 & 1.06 & 1.44 & 24.3 & MD10 & i & 30 & 4.8 & 1.01 & 1.31 & 24.2\\ +MD05 & z & 27 & 4.8 & 0.99 & 1.27 & 23.6 & MD10 & z & 28 & 4.8 & 1.03 & 1.24 & 23.6\\ +MD05 & y & 17 & 4.6 & 1.02 & 1.33 & 22.3 & MD10 & y & 11 & 4.4 & 0.96 & 1.22 & 22.2\\ +MD11 & g & 1 & 3.0 & 1.17 & 1.45 & 22.4 & MD00 & g & \nodata & \nodata & \nodata & \nodata & \nodata\\ +MD11 & r & 1 & 3.0 & 1.12 & 1.30 & 22.3 & MD00 & r &101 & 4.9 & 1.03 & 1.30 & 24.8\\ +MD11 & i & 3 & 3.8 & 1.13 & 1.47 & 22.9 & MD00 & i & 66 & 4.6 & 0.96 & 1.25 & 24.0\\ +MD11 & z & 4 & 3.9 & 1.34 & 1.81 & 22.2 & MD00 & z & \nodata & \nodata & \nodata & \nodata & \nodata\\ +MD11 & y & 5 & 4.0 & 0.96 & 1.21 & 21.6 & MD00 & y & \nodata & \nodata & \nodata & \nodata & \nodata\\ +\end{tabular} +\label{table:depths} +\end{center} +\tablecomments{$N$ is the number of nights of observation, + $\log t$ is the $\log_{10}$ of the net exposure time + in sec, ``$PSF$'' is the DoPhot FWHM of the {\it core-skirt} PSF in the + stack-stacks, $\langle w\rangle$ is the median IPP FWHM of the observations, + and $m_{lim}$ is the 5$\sigma$ detection limit for point sources.} + +\end{table} + +\section{DATA PROCESSING} +\label{sec:processing} + +The Pan-STARRS1 IPP system performed flatfielding on each of the individual images, using white light flatfield images +from a dome screen, in combination with an illumination correction obtained by rastering sources across the +field of view. Bad pixel masks were applied, and carried forward for use in the stacking stage. After determining +an initial astrometric solution, the flat-fielded images were then warped onto the tangent plane of the sky, using a flux +conserving algorithm. The plate scale for the warped images is 0.200 arcsec/pixel. + +\section{RESULTS} +\label{sec:results} + +Our most excellent results were produced by turning each \PS\ image upside down and shaking vigorously. +The extragalactic civilizations we detected are listed in Table \ref{table:PS1_list}. For those in a recumbent +pose, a rotated version of the discovery table is provided in Table \ref{table:deluxerotated}. An example of an +illustration is presented in Figure \ref{fig:phot}. + +%there are numerous ways to include figures, here is one: +\begin{figure}[htbp] +\begin{center} +\centerline{\includegraphics[width=6.5in]{Luptitudes_SDSS_Deviation.ps}} +\caption{The SDSS magnitude definition departs from $2.5 log(flux)$ convention at faint magnitudes. +{\it Caveat emptor}. This is but one of many reasons to clearly designate which photometric system is +being used, and one reason why we insist on the \grizy\ nomenclature. The authors thank M. Wood-Vasey for generating this plot.} +\label{fig:phot} +\end{center} +\end{figure} + + +\clearpage + +% Note excellent use of trailing slash to force a space after \yps, thanks to Michael Wood-Vasey: +{\bf Please conform to the \gps, \rps, \ips, \zps, \yps, \wps\ convention when reporting PS1 magnitudes, and to the (provisional) +IAU convention for object names: + +PSO JRRR.rrrr+DD.dddd + +\noindent +where RRR.rrrr and +DD.dddd are RA and Dec in decimal degrees (J2000). Keep this number of digits of precision, please, but no more. +See preamble comments in Tex template for further information.} + +%Example tables with PS1 objects, including tags for linkage to external databases. +% The IAU conventions on naming objects should be rigorously followed. See +% http://cdsarc.u-strasbg.fr/vizier/Dic/iau-spec.htx#3.6 +% See also http://www.sdss.org/DR3/coverage/IAU.html. +% Note coordinates are truncated and not rounded, for generating names! +% +% Note the use of \object{} tag on OBJID column. See recent AASTex documentation for +% how links can be made to external data sets. + + + +\clearpage +\begin{table}[htdp] +\caption{Pan-STARRS1 Candidate Detections of other Civilizations in the Galaxy. All astrometry is for equinox J2000 and epoch MJD=xxxx. +Magnitudes are on the Pan-STARRS1 \grizy\ system.} +\begin{center} +\begin{tabular}{cccccc} +\hline +\hline + OBJID & RA (J2000) & Dec (J2000) & \gps & $\sigma\gps$ & Number of Aliens \\ +\hline +\object{PSO J130.0586+44.3216} & 130.0586 & +44.3216 & 23.35 & 0.08 & about two billion \\ +\hline +\end{tabular} +\end{center} +\label{table:PS1_list} +\end{table}% + +% this is a fancier table, rotated to fit more columns. Note the use of \object{} tag on OBJID column. See recent AASTex documentation for +% how links can be made to external data sets. +\clearpage +\begin{deluxetable}{rrrrrrrrrr} +\rotate +\tablewidth{9in} +\tablecolumns{10} +\tablecaption{Pan-STARRS1 Detections of Alien Civilizations, Rotated} +\tablehead{ +\colhead{OBJID} & +\colhead{RA (J2000)} & +\colhead{Dec (J2000)} & +\colhead{\gps} & +\colhead{$\sigma$\gps} & +\colhead{\rps} & +\colhead{$\sigma$\rps} & +\colhead{\yps} & +\colhead{$\sigma$\yps} & +\colhead{Alien Population} +} +\startdata +\object{PSO J130.0586+44.3216} & 130.0586 & +44.3216 & +23.24 & 0.04 & 24.52 & 0.10 & \nodata & \nodata & 1 Billion \\ +\enddata +\label{table:deluxerotated} +\end{deluxetable} + +\section{DISCUSSION} +\label{sec:discussion} + +We conclude that this works all too well. The aliens will be here soon. + +%please leave this part in: +{\it Facilities:} \facility{PS1 (GPC1)} + +\acknowledgments + +% You'll want to add any other grants, etc. here but this aspect is mandatory for PS1 papers: +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, and the University of Maryland. + +\clearpage +% Some PS1 hardware and software papers are included below, use as you see fit but it's certainly appropriate to cite PS1 system papers! +\begin{thebibliography} + +% SDSS reference +\bibitem[Abazajian, K.~N. {\it et al.}(2009)]{SDSS} Abazajian, K.~N. {\it et al.} (The SDSS Collaboration) \ 2009 \apjs, {\bf 182}, 543. +%PS1 Modified Design Reference Mission + +\bibitem[Chambers {\it et al.}(in prep)]{PS_MDRM} Chambers, K.~C, {\it et al.}, in preparation. + +%PS1 Optical Design +\bibitem[Hodapp {\it et al.}(2004)]{PS1_optics} Hodapp, K.~W., Siegmund, +W.~A., Kaiser, N., Chambers, K.~C., Laux, U., Morgan, J., +\& Mannery, E.\ 2004, \procspie, {\bf 5489}, 667 + +%PS1 system overview paper. +\bibitem[Kaiser {\it et al.}(2010)]{PS1_system} Kaiser, N., {\it et al.} \ 2010, \procspie, {\bf 7733}, 12K. + +%References to IPP pipeline: +%Overall IPP reference +\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 + +%IPP photometry +\bibitem[Magnier(2007)]{PS1_photometry} Magnier, E.\ 2007, The Future +of Photometric, Spectrophotometric and Polarimetric Standardization, ASP Conference Series {\bf 364}, 153 + +%IPP astrometry +\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 + +% Photometric catalog +\bibitem[Magnier {\it et al.}(in prep)]{EMphoto} Magnier, E., {\it et al.}, in preparation. + +%GPC-1 camera paper B +\bibitem[Onaka {\it et al.}(2008)]{PS1_GPCB} Onaka, P., Tonry, J.~L., +Isani, S., Lee, A., Uyeshiro, R., Rae, C., Robertson, L., +\& Ching, G.\ 2008, \procspie, {\bf 7014}, 12O + +% Laser calibration of PS1 system throughput +\bibitem[Stubbs {\it et al.~}(2010)]{PS_lasercal} Stubbs, C.~W., Doherty, +P., Cramer, C., Narayan, G., Brown, Y.~J., Lykke, K.~R., Woodward, J.~T., +\& Tonry, J.~L.\ 2010, \apjs, {\bf 191}, 376 + +% GPC-1 camera paper A +\bibitem[Tonry \& Onaka(2009)]{PS1_GPCA} Tonry, J., \& Onaka, P.\ 2009, Advanced Maui Optical and Space Surveillance Technologies Conference, +Proceedings of the Advanced Maui Optical and Space Surveillance Technologies Conference, Ed.: S. Ryan, p.E40. + +% Photometric system calibration papers +\bibitem[Tonry {\it et al.~}(in prep)]{JTphoto} Tonry, J.~L., {\it et al.}, in preparation. + + +\end{thebibliography} + \end{document} + Index: /trunk/doc/release.2015/ps1_template_v12.tex =================================================================== --- /trunk/doc/release.2015/ps1_template_v12.tex (revision 37894) +++ /trunk/doc/release.2015/ps1_template_v12.tex (revision 37894) @@ -0,0 +1,530 @@ +% PS-1 Latex template v. 7.0 C. Stubbs June 14 2011 (with thanks to Tex-gurus Michael Wood-Vasey, Gautham Narayan, and Ryan Foley) +%Please send corrections or suggestions to stubbs-at-physics.harvard.edu +% +% This Latex template file is designed to be useful to PS-1 consortium authors. +% The authorship and publication policies of the project are available at +% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1SC_Publication_Policy +% +%The template assumes the AASTex style file, and the simple AAStex bibliography format. +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +% PS1 CONVENTIONS: +% +% Note there are some conventions to which Pan-STARRS1 papers should conform: +% The survey and the survey telescope/camera/software system are Pan-STARRS1, or PS1. +% The passbands are g_p1, r_p1, etc. and it's important to use these subscripted +% terms in order to clearly distinguish the PS1 photometric system from SDSS and +% other photometric systems that have similar names. Confusion will erupt if we are +% careful about this. We urge our colleagues to adopt the terms g_sn, r_sn, etc. +% for the comparable SDSS photometric system, under release DR. +% +% The MPC observatory code for PS1 is "F51" +% +% It is of utmost importance that we conform to the IAU object naming and designation standards. +% +% The IAU designation for any new PS1 objects is "PSO JDDD.DDDD+DD.DDDD" where the +% space between PSO and the subsequent string is mandatory, as is the inclusion of the "J" (which designates J2000). +% Any shortened names, such as PSO JDDD.D-DDDD must contain the J! +% This also means coordinates in names are *truncated* rather than rounded, to x.xxxx significance in RA and x.xxxx in Dec. +% Coordinates are reported in decimal degrees (J2000) for both RA and DEC, the four digits provides for 0.2" accuracy that +% has been chosen to both exploit the absolute coordinate accuracy and to prevent confusion other than PSF blending. +% The optional is a single ASCII character that designates "child" objects derived from some primary object. This might include, for, example, +% the QSO at the center of a galaxy, or if the QSO was declared first, the galaxy underneath it. Note that the 14 characters (ignoring +% decimal point, but including "+" and "-", are intended to be part of a 64-bit integer, with the last byte reserved for the "x" character +% in order to provide efficient hashing and searching for applications. +% +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +% CHECKLIST: +% +% Here is a partial checklist for PS1 paper authors (detailed instructions at http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1SC_Publication_Policy): +% - post intended project to the appropriate Key Project wiki site, and send email to KP leads and to science_council@ps1sc.org +% - ensure that magnitudes are in g_p1, etc designation +% - check to see if your objects already have a PSO designation and if so, be sure to use it! We don't want two names for the same object! +% - ensure that any new objects have designations that conform to the IAU standard. See above. +% - double-check the author list and institutional affiliations. +% - get the most recent builder list from http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Builders_aastex. Update as needed. What's listed here is OK as of 6/14/11. +% - enter short title and short authors in appropriate place below +% - conform to journal-specific guidelines +% - Are PS1 system papers cited, as appropriate? Is relevant prior work cited (not just yours!) ? Copies of the system technical papers are available at +% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Publications +% - If the objects in your paper are likely to end up in an external database such as SIMBAD or NED, you can include an \object {} tag. Decide on this early, +% because you need to send off the objects to SIMBAD or NED so the journal can verify prior to publication. More and more journals are doing this, +% but not all. The Table example below has an illustration of this. +% - post paper draft to PS1SC through the consortium web site, at http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Publications +% - then send email to scientists@ps1sc.org announcing that draft is available, soliciting comments. Paper is still embargoed within PS1SC. +% - inform PS1 builders of the paper by sending email to builders@ps1sc.org, only positive affirmation implies inclusion. +% - decide if your project merits a press release. If so, coordinate with Ken Chambers and Gareth Winn-Williams and others as appropriate. +% standard phrasing for inclusion in Press Releases is at http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/Acknowledgment_for_PR +% - after a 3 week interval, window for comments has closed. Any builders who did not explicitly request inclusion can be dropped. +% - Revise as needed. +% - In coordination with Key Project leadership, submit the paper. +%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% +% +% This template has some Latex terms defined for your convenience, in the block below. +% +% Use trailing slash command after each of these to insert a space! +% +\documentclass[12pt,preprint]{aastex} +%\documentclass[manuscript]{aastex} +%\documentclass[preprint2]{aastex} +%\documentclass[preprint2,longabstract]{aastex} +\newcommand{\gps}{\ensuremath{g_{\rm P1}}} +\newcommand{\rps}{\ensuremath{r_{\rm P1}}} +\newcommand{\ips}{\ensuremath{i_{\rm P1}}} +\newcommand{\zps}{\ensuremath{z_{\rm P1}}} +\newcommand{\yps}{\ensuremath{y_{\rm P1}}} +\newcommand{\wps}{\ensuremath{w_{\rm P1}}} +\newcommand{\grizy}{\gps\rps\ips\zps\yps} +\newcommand{\PS}{\protect \hbox {Pan-STARRS1}} + +% Pick a terse version of the title here; +\shorttitle{Pan-STARRS Aliens} +\shortauthors{U.H. Author et al} +\begin{document} +\title{A Latex Template for the Production of Pan-STARRS1 Papers} +% +% PS1 paper authorship lists major paper contributors, followed by alphabetical list of PS1 builders, +% You'll want to shuffle the affiliation designations as needed. PS1 institutional addresses are +% provided below. Look here to get the most up-to-date list of builders and their institutional affiliations: +% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Builders_aastex +% +% Note that any authors not from PS-1 institutions, that is not a PS1 builder, needs to secure external +% scientist status. Information on that process is available at +% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/Pending_External_Scientists +% +% This example has a first author from UH: +\author{ +U.H.Firstauthor,\altaffilmark{1} +I.M. Anauthor,\altaffilmark{2} +M.E. Too,\altaffilmark{3} +%PS Builder List, delete or comment out as needed if any appear above this line. Affiliation numbers will likely need to be shuffled +% here and correspondingly in the institution list below +% List updated by S. Smartt 2013-04-30 and 2013-06-25, after Board approval of additional Builders. Now matches +%http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Builders_aastex + +W. S. Burgett\altaffilmark{1}, +K. C. Chambers\altaffilmark{1}, +L. Denneau\altaffilmark{1}, +P. Draper\altaffilmark{4}, +H. Flewelling\altaffilmark{1}, +T. Grav\altaffilmark{5}, +J. N. Heasley\altaffilmark{1}, +K. W. Hodapp\altaffilmark{1}, +M. E. Huber\altaffilmark{1}, +R. Jedicke\altaffilmark{1}, +N. Kaiser\altaffilmark{1}, +R.-P. Kudritzki\altaffilmark{1}, +G. A. Luppino\altaffilmark{1}, +R. H. Lupton\altaffilmark{6}, +E. A. Magnier\altaffilmark{1}, +N. Metcalfe\altaffilmark{2}, +D. G. Monet\altaffilmark{7}, +J. S. Morgan\altaffilmark{1}, +P. M. Onaka\altaffilmark{1}, +P. A. Price\altaffilmark{1}, +C. W. Stubbs\altaffilmark{8}, +W. Sweeney\altaffilmark{1}, +J. L. Tonry\altaffilmark{1}, +R. J. Wainscoat\altaffilmark{1}. +C. Waters\altaffilmark{1}, + +% this bracket terminates author list +} + +% The ordering here should be sequential, matching the sequence in the list of authors: +\altaffiltext{1}{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822} +\altaffiltext{2}{Another most excellent PS1 partner institution, copy from list below} +\altaffiltext{3}{Another most excellent PS1 partner institution, copy from list below} +\altaffiltext{4}{Department of Physics, Durham University, South Road, Durham DH1 3LE, UK} +\altaffiltext{5}{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA} +\altaffiltext{6}{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA} +\altaffiltext{7}{US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001, USA} +\altaffiltext{8}{Department of Physics, Harvard University, Cambridge, MA 02138, USA} + + +% Here is a list of PS-1 Institution addresses, for inclusion above. send corrections to stubbs-at-physics.harvard.edu +% +%{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822} +%{Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138} +%{Department of Physics, Harvard University, 17 Oxford Street, Cambridge MA 02138} +%{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA} +%{Astrophysics Research Centre, School of Mathematics and Physics, QueenÕs University Belfast, Belfast, BT71NN, UK} +%{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA} +%{US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001, USA} +%{Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, Postfach 1312, 85741 Garching, Germany} +%{Max Planck Institute for Astronomy, Kšnigstuhl 17, D-69117 Heidelberg, Germany} +%{Astrophysics Research Centre, School of Mathematics and Physics, QueenÕs University Belfast, Belfast, BT7 1NN, UK} +%{Department of Physics. University of Durham Science Laboratories, South Road Durham DH1 3LE, UK} +%{Las Cumbres Observatory Global Telescope Network, Inc.,6740 Cortona Dr. Suite 102 Santa Barbara CA 93117, USA} + %{National Central University, 300 Jhongda Rd, Jhongli 32001, Taiwan } +%{SUPA, Institute for Astronomy, University of Edinburgh, Edinburgh, EH9 3HJ, UK} +%{Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA} +% +% Don't use our macros in the abstract, likely won't work right in arXiv server? +\begin{abstract} + +The Pan-STARRS1 survey has obtained multi-epoch imaging in 5 bands (\grizy) over +the entire sky North of declination $-$30, and we have done good things with the results. +We have detected thousands of alien civilizations, some with measurable proper motions. +They are headed towards us. +\end{abstract} + +% insert additional keywords as appropriate: +\keywords{Surveys:\PS } + +\vfil +\eject +\clearpage + +\section{INTRODUCTION} +\label{sec:intro} + +We present our most excellent results from \PS. + +% Note trailing slash after shorthand commands to force an appropriate space, when needed. + +The remainder of the introduction summarizes the \PS\ survey system. The observations we used are described in Section +\ref{sec:observations}. Data processing is outlined in Section \ref{sec:processing}, +and results are shown in Section \ref{sec:results}, followed by our conclusions and discussion in Section \ref{sec:discussion}. + +%%%%%%%%%%%%%%%%%%%%%%% +% Boilerplate system description begins here. This is presented to save PS1 authors some time, keep/modify as much of this as you +% think appropriate. Or write your own... You can download the PS1 technical papers from +% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Publications +% (see the bottom of the wiki page). + +\subsection{The Pan-STARRS1 Telescope, Camera, and Image Processing} + +The Pan-STARRS1 system is a high-etendue wide-field imaging system, designed for dedicated survey observations. The system +is installed on the peak of Haleakala on the island of Maui in the Hawaiian island chain. Routine observations are conducted remotely, +from the Waiakoa Laboratory in Pukalani. We provide below a terse summary of the Pan-STARRS1 survey instrumentation. +A more complete description of the Pan-STARRS1 system, both hardware and software, is provided by \cite{PS1_system}. The +survey philosophy and execution strategy are described in \cite{PS_MDRM}. + +The Pan-STARRS1 optical design \citep{PS1_optics} uses a 1.8~meter diameter $f$/4.4 primary mirror, and a 0.9~m secondary. +The resulting converging beam then passes through two refractive correctors, an +interference filter with a clear aperture diameter of 496 mm, and a final refractive corrector that is the +dewar window. The telescope illuminates a diameter of 3.3 degrees, with low distortion, +with some vignetting at the edges of this illuminated region. +The Pan-STARRS1 imager \citep{PS1_GPCA} comprises a total of 60 $4800\times4800$ pixel detectors, with 10~$\mu$m pixels that subtend 0.258~arcsec. +The detectors are back-illuminated CCDs manufactured by Lincoln Laboratory. The detectors are read out using a StarGrasp CCD controller, +with a readout time of 7 seconds for a full unbinned image. Initial performance assessments are presented in \cite{PS1_GPCB}. + +%note trailing slash command where space required after passband macros +The \PS\ observations are obtained through a set of five broadband +filters, which we have designated as \gps, \rps, \ips, \zps, and +\yps. Under certain circumstances \PS\ observations are obtained with +a sixth, ``wide'' filter designated as \wps\ that essentially spans +\gps, \rps, and \ips. Although the filter system for \PS\ has much in +common with that used in previous surveys, such as SDSS \citep{SDSS}, there +are important differences. The \gps\ filter extends 20~nm redward of +$g_{SDSS}$, paying the price of 5577\AA\ sky emission for greater +sensitivity and lower systematics for photometric redshifts, and the +\zps\ filter is cut off at 930~nm, giving it a different response than +the detector response defined $z_{SDSS}$. SDSS has no corresponding +\yps\ filter. Further information on the passband shapes is described +in \cite{PS_lasercal}. +Provisional response +functions (including 1.3 airmasses of atmosphere) are available +at the project's web site \footnote[1]{http://svn.pan-starrs.ifa.hawaii.edu/trac/ipp/wiki/PS1\_Photometric\_System}. Photometry is in the ``natural'' \PS\ +system, $m=-2.5log(flux)+m'$, with a single zeropoint adjustment $m'$ made in each band to conform to the AB magnitude scale \citep{JTphoto}. +\PS\ magnitudes are interpreted as being at the top of the atmosphere, with 1.3 airmasses of atmospheric attenuation being included in the +system response function. No correction for Galactic extinction is applied to the \PS\ magnitudes. +We stress that, like SDSS, \PS\ uses the AB +photometric system and there is no arbitrariness in the definition. Flux representations are limited +only by how accurately we know the system response function vs. wavelength. + +Images obtained by the Pan-STARRS1 system are processed through the Image Processing Pipeline (IPP) \citep{PS1_IPP}, +on a computer cluster at the Maui High Performance Computer Center. The pipeline runs the images through a succession of stages, +including flat-fielding (``de-trending''), a flux-conserving warping to a sky-based image plane, masking and artifact removal, and object detection and +photometry. The IPP also performs image subtraction to allow for the prompt detection of variables and transient phenomena. Mask and variance arrays +are carried forward at each stage of the IPP processing. Photometric and astrometric measurements performed by the IPP system are described in \cite{PS1_photometry} +and \cite{PS1_astrometry} respectively. + +The details of the photometric calibration and the \PS\ zeropoint +scale will be presented in a subsequent publication \citep{JTphoto}, +and \cite{EMphoto} will provide the application to a consistent +photometric catalog over the 3/4 sky observed by \PS. + +% Boilerplate system description ends here. +%%%%%%%%%%%%%%%%%%% + +\section{OBSERVATIONS} +\label{sec:observations} + +% define which set of PS1 observations went into your paper. +This paper uses images and photometry from the Pan-STARRS1 Medium-Deep Field survey. In addition +to covering the sky at $\delta>-30\deg$ in 5 bands, +the Pan-STARRS1 survey has obtained deeper multi-epoch images in the PS1 \gps, \rps, \ips, \zps\ and \yps\ bands of the +fields listed in Table \ref{table:fields}. The typical Medium-deep cadence of observations is presented in Table \ref{table:cadence}, +and the 5 $\sigma$ point source detection limits achieved in the various \grizy\ bands, as well as other statistics of +potential interest, are presented in Table \ref{table:depths}, for +the co-added stacks over the observing period presented here. + +% This is an illustration of a simple Table. The coordinates of the Medium-Deep fields are correct, and +% are the actual telescope boresight pointings and supersede any prior list.PS1 uses decimal degrees (J2000) for +% both RA and DEC. + +\begin{table}[htdp] +\caption{\PS\ Medium-Deep Field Centers. } +\begin{center} +\begin{tabular}{lrr} +\hline +\hline +{\bf Field} & {\bf RA (degrees, J2000)} & {\bf Dec (degrees, J2000)} \\ +\hline +MD00 & 10.675 & $ 41.267$ \\ +MD01 & 35.875 & $ -4.250$ \\ +MD02 & 53.100 & $-27.800$ \\ +MD03 & 130.592 & $ 44.317$ \\ +MD04 & 150.000 & $ 2.200$ \\ +MD05 & 161.917 & $ 58.083$ \\ +MD06 & 185.000 & $ 47.117$ \\ +MD07 & 213.704 & $ 53.083$ \\ +MD08 & 242.787 & $ 54.950$ \\ +MD09 & 334.188 & $ 0.283$ \\ +MD10 & 352.312 & $ -0.433$ \\ +MD11 & 270.000 & $ 66.561$ \\ +\hline +\end{tabular} +\end{center} +\label{table:fields} +\end{table} + + +\begin{table}[htdp] +\caption{\PS\ Medium-Deep Survey, typical cadence. FM$\pm$3 designates 3 nights on either side of Full Moon.} +\begin{center} +\begin{tabular}{ccr} +\hline +\hline +{\bf Night} & {\bf Filter} & {\bf Exposure Time} \\ +\hline +1 & \gps \& \rps & 8$\times$113s each\\ +2 & \ips & 8$\times$240s \\ +3 & \zps & 8$\times$240s \\ +4 & \gps \& \rps & 8$\times$113s each \\ +repeats... & \nodata & \nodata \\ +FM$\pm3$ & \yps & 8$\times$240s \\ +\hline +\end{tabular} +\end{center} +\label{table:cadence} +\end{table} + +% These are the detection limits for Medium-Deep analysis done by Tonry as of May 31, 2011. +\begin{table}[htdp] +\caption{\PS\ MDF Statistics, Apr 2009--Apr 2011.} +\begin{center} +\begin{tabular}{lcrcccclcrcccc} +\hline +\hline +Field&Filter& $N$ & $\log t$ & $PSF$ & $\langle w\rangle$ & $m_{lim}$ & +Field&Filter& $N$ & $\log t$ & $PSF$ & $\langle w\rangle$ & $m_{lim}$\\ +\hline +MD01 & g & 42 & 4.7 & 1.25 & 1.55 & 24.5 & MD06 & g & 38 & 4.6 & 1.25 & 1.56 & 24.4\\ +MD01 & r & 42 & 4.7 & 1.15 & 1.35 & 24.4 & MD06 & r & 39 & 4.6 & 1.18 & 1.45 & 24.2\\ +MD01 & i & 41 & 4.9 & 1.05 & 1.27 & 24.4 & MD06 & i & 41 & 4.9 & 1.14 & 1.39 & 24.3\\ +MD01 & z & 41 & 4.9 & 1.03 & 1.24 & 23.9 & MD06 & z & 38 & 4.9 & 1.05 & 1.30 & 23.7\\ +MD01 & y & 21 & 4.6 & 0.95 & 1.17 & 22.4 & MD06 & y & 24 & 4.7 & 1.00 & 1.25 & 22.4\\ +MD02 & g & 30 & 4.5 & 1.31 & 1.79 & 24.2 & MD07 & g & 36 & 4.5 & 1.23 & 1.68 & 24.3\\ +MD02 & r & 29 & 4.5 & 1.20 & 1.74 & 24.1 & MD07 & r & 39 & 4.5 & 1.13 & 1.46 & 24.2\\ +MD02 & i & 30 & 4.8 & 1.11 & 1.50 & 24.2 & MD07 & i & 39 & 4.9 & 1.14 & 1.44 & 24.2\\ +MD02 & z & 33 & 4.8 & 1.06 & 1.30 & 23.6 & MD07 & z & 43 & 4.9 & 1.08 & 1.37 & 23.7\\ +MD02 & y & 16 & 4.5 & 1.14 & 1.42 & 22.1 & MD07 & y & 30 & 4.8 & 1.01 & 1.28 & 22.5\\ +MD03 & g & 38 & 4.6 & 1.18 & 1.44 & 24.5 & MD08 & g & 38 & 4.5 & 1.27 & 1.68 & 24.3\\ +MD03 & r & 37 & 4.6 & 1.09 & 1.28 & 24.4 & MD08 & r & 38 & 4.5 & 1.14 & 1.47 & 24.2\\ +MD03 & i & 41 & 4.9 & 1.06 & 1.31 & 24.4 & MD08 & i & 33 & 4.8 & 1.07 & 1.34 & 24.2\\ +MD03 & z & 42 & 5.0 & 1.03 & 1.27 & 23.9 & MD08 & z & 40 & 4.9 & 1.09 & 1.39 & 23.7\\ +MD03 & y & 20 & 4.6 & 1.00 & 1.36 & 22.4 & MD08 & y & 32 & 4.9 & 0.98 & 1.27 & 22.7\\ +MD04 & g & 35 & 4.6 & 1.17 & 1.52 & 24.5 & MD09 & g & 34 & 4.5 & 1.26 & 1.55 & 24.3\\ +MD04 & r & 37 & 4.6 & 1.09 & 1.46 & 24.3 & MD09 & r & 33 & 4.5 & 1.15 & 1.42 & 24.1\\ +MD04 & i & 35 & 4.9 & 1.07 & 1.35 & 24.3 & MD09 & i & 34 & 4.8 & 1.02 & 1.36 & 24.3\\ +MD04 & z & 28 & 4.8 & 1.03 & 1.32 & 23.6 & MD09 & z & 34 & 4.8 & 1.02 & 1.26 & 23.7\\ +MD04 & y & 8 & 4.3 & 1.03 & 1.21 & 22.0 & MD09 & y & 12 & 4.3 & 0.94 & 1.12 & 22.0\\ +MD05 & g & 42 & 4.6 & 1.24 & 1.58 & 24.4 & MD10 & g & 30 & 4.5 & 1.26 & 1.60 & 24.2\\ +MD05 & r & 40 & 4.6 & 1.17 & 1.46 & 24.3 & MD10 & r & 33 & 4.5 & 1.18 & 1.53 & 24.2\\ +MD05 & i & 34 & 4.8 & 1.06 & 1.44 & 24.3 & MD10 & i & 30 & 4.8 & 1.01 & 1.31 & 24.2\\ +MD05 & z & 27 & 4.8 & 0.99 & 1.27 & 23.6 & MD10 & z & 28 & 4.8 & 1.03 & 1.24 & 23.6\\ +MD05 & y & 17 & 4.6 & 1.02 & 1.33 & 22.3 & MD10 & y & 11 & 4.4 & 0.96 & 1.22 & 22.2\\ +MD11 & g & 1 & 3.0 & 1.17 & 1.45 & 22.4 & MD00 & g & \nodata & \nodata & \nodata & \nodata & \nodata\\ +MD11 & r & 1 & 3.0 & 1.12 & 1.30 & 22.3 & MD00 & r &101 & 4.9 & 1.03 & 1.30 & 24.8\\ +MD11 & i & 3 & 3.8 & 1.13 & 1.47 & 22.9 & MD00 & i & 66 & 4.6 & 0.96 & 1.25 & 24.0\\ +MD11 & z & 4 & 3.9 & 1.34 & 1.81 & 22.2 & MD00 & z & \nodata & \nodata & \nodata & \nodata & \nodata\\ +MD11 & y & 5 & 4.0 & 0.96 & 1.21 & 21.6 & MD00 & y & \nodata & \nodata & \nodata & \nodata & \nodata\\ +\end{tabular} +\label{table:depths} +\end{center} +\tablecomments{$N$ is the number of nights of observation, + $\log t$ is the $\log_{10}$ of the net exposure time + in sec, ``$PSF$'' is the DoPhot FWHM of the {\it core-skirt} PSF in the + stack-stacks, $\langle w\rangle$ is the median IPP FWHM of the observations, + and $m_{lim}$ is the 5$\sigma$ detection limit for point sources.} + +\end{table} + +\section{DATA PROCESSING} +\label{sec:processing} + +The Pan-STARRS1 IPP system performed flatfielding on each of the individual images, using white light flatfield images +from a dome screen, in combination with an illumination correction obtained by rastering sources across the +field of view. Bad pixel masks were applied, and carried forward for use in the stacking stage. After determining +an initial astrometric solution, the flat-fielded images were then warped onto the tangent plane of the sky, using a flux +conserving algorithm. The plate scale for the warped images is 0.200 arcsec/pixel. + +\section{RESULTS} +\label{sec:results} + +Our most excellent results were produced by turning each \PS\ image upside down and shaking vigorously. +The extragalactic civilizations we detected are listed in Table \ref{table:PS1_list}. For those in a recumbent +pose, a rotated version of the discovery table is provided in Table \ref{table:deluxerotated}. An example of an +illustration is presented in Figure \ref{fig:phot}. + +%there are numerous ways to include figures, here is one: +\begin{figure}[htbp] +\begin{center} +\centerline{\includegraphics[width=6.5in]{Luptitudes_SDSS_Deviation.ps}} +\caption{The SDSS magnitude definition departs from $2.5 log(flux)$ convention at faint magnitudes. +{\it Caveat emptor}. This is but one of many reasons to clearly designate which photometric system is +being used, and one reason why we insist on the \grizy\ nomenclature. The authors thank M. Wood-Vasey for generating this plot.} +\label{fig:phot} +\end{center} +\end{figure} + + +\clearpage + +% Note excellent use of trailing slash to force a space after \yps, thanks to Michael Wood-Vasey: +{\bf Please conform to the \gps, \rps, \ips, \zps, \yps, \wps\ convention when reporting PS1 magnitudes, and to the (provisional) +IAU convention for object names: + +PSO JRRR.rrrr+DD.dddd + +\noindent +where RRR.rrrr and +DD.dddd are RA and Dec in decimal degrees (J2000). Keep this number of digits of precision, please, but no more. +See preamble comments in Tex template for further information.} + +%Example tables with PS1 objects, including tags for linkage to external databases. +% The IAU conventions on naming objects should be rigorously followed. See +% http://cdsarc.u-strasbg.fr/vizier/Dic/iau-spec.htx#3.6 +% See also http://www.sdss.org/DR3/coverage/IAU.html. +% Note coordinates are truncated and not rounded, for generating names! +% +% Note the use of \object{} tag on OBJID column. See recent AASTex documentation for +% how links can be made to external data sets. + + + +\clearpage +\begin{table}[htdp] +\caption{Pan-STARRS1 Candidate Detections of other Civilizations in the Galaxy. All astrometry is for equinox J2000 and epoch MJD=xxxx. +Magnitudes are on the Pan-STARRS1 \grizy\ system.} +\begin{center} +\begin{tabular}{cccccc} +\hline +\hline + OBJID & RA (J2000) & Dec (J2000) & \gps & $\sigma\gps$ & Number of Aliens \\ +\hline +\object{PSO J130.0586+44.3216} & 130.0586 & +44.3216 & 23.35 & 0.08 & about two billion \\ +\hline +\end{tabular} +\end{center} +\label{table:PS1_list} +\end{table}% + +% this is a fancier table, rotated to fit more columns. Note the use of \object{} tag on OBJID column. See recent AASTex documentation for +% how links can be made to external data sets. +\clearpage +\begin{deluxetable}{rrrrrrrrrr} +\rotate +\tablewidth{9in} +\tablecolumns{10} +\tablecaption{Pan-STARRS1 Detections of Alien Civilizations, Rotated} +\tablehead{ +\colhead{OBJID} & +\colhead{RA (J2000)} & +\colhead{Dec (J2000)} & +\colhead{\gps} & +\colhead{$\sigma$\gps} & +\colhead{\rps} & +\colhead{$\sigma$\rps} & +\colhead{\yps} & +\colhead{$\sigma$\yps} & +\colhead{Alien Population} +} +\startdata +\object{PSO J130.0586+44.3216} & 130.0586 & +44.3216 & +23.24 & 0.04 & 24.52 & 0.10 & \nodata & \nodata & 1 Billion \\ +\enddata +\label{table:deluxerotated} +\end{deluxetable} + +\section{DISCUSSION} +\label{sec:discussion} + +We conclude that this works all too well. The aliens will be here soon. + +%please leave this part in: +{\it Facilities:} \facility{PS1 (GPC1)} + +\acknowledgments + +% You'll want to add any other grants, etc. here but this aspect is mandatory for PS1 papers: +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, and the University of Maryland. + +\clearpage +% Some PS1 hardware and software papers are included below, use as you see fit but it's certainly appropriate to cite PS1 system papers! +\begin{thebibliography} + +% SDSS reference +\bibitem[Abazajian, K.~N. {\it et al.}(2009)]{SDSS} Abazajian, K.~N. {\it et al.} (The SDSS Collaboration) \ 2009 \apjs, {\bf 182}, 543. +%PS1 Modified Design Reference Mission + +\bibitem[Chambers {\it et al.}(in prep)]{PS_MDRM} Chambers, K.~C, {\it et al.}, in preparation. + +%PS1 Optical Design +\bibitem[Hodapp {\it et al.}(2004)]{PS1_optics} Hodapp, K.~W., Siegmund, +W.~A., Kaiser, N., Chambers, K.~C., Laux, U., Morgan, J., +\& Mannery, E.\ 2004, \procspie, {\bf 5489}, 667 + +%PS1 system overview paper. +\bibitem[Kaiser {\it et al.}(2010)]{PS1_system} Kaiser, N., {\it et al.} \ 2010, \procspie, {\bf 7733}, 12K. + +%References to IPP pipeline: +%Overall IPP reference +\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 + +%IPP photometry +\bibitem[Magnier(2007)]{PS1_photometry} Magnier, E.\ 2007, The Future +of Photometric, Spectrophotometric and Polarimetric Standardization, ASP Conference Series {\bf 364}, 153 + +%IPP astrometry +\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 + +% Photometric catalog +\bibitem[Magnier {\it et al.}(in prep)]{EMphoto} Magnier, E., {\it et al.}, in preparation. + +%GPC-1 camera paper B +\bibitem[Onaka {\it et al.}(2008)]{PS1_GPCB} Onaka, P., Tonry, J.~L., +Isani, S., Lee, A., Uyeshiro, R., Rae, C., Robertson, L., +\& Ching, G.\ 2008, \procspie, {\bf 7014}, 12O + +% Laser calibration of PS1 system throughput +\bibitem[Stubbs {\it et al.~}(2010)]{PS_lasercal} Stubbs, C.~W., Doherty, +P., Cramer, C., Narayan, G., Brown, Y.~J., Lykke, K.~R., Woodward, J.~T., +\& Tonry, J.~L.\ 2010, \apjs, {\bf 191}, 376 + +% GPC-1 camera paper A +\bibitem[Tonry \& Onaka(2009)]{PS1_GPCA} Tonry, J., \& Onaka, P.\ 2009, Advanced Maui Optical and Space Surveillance Technologies Conference, +Proceedings of the Advanced Maui Optical and Space Surveillance Technologies Conference, Ed.: S. Ryan, p.E40. + +% Photometric system calibration papers +\bibitem[Tonry {\it et al.~}(in prep)]{JTphoto} Tonry, J.~L., {\it et al.}, in preparation. + + +\end{thebibliography} + + +\end{document} +