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Timestamp:
Feb 4, 2015, 3:29:48 PM (11 years ago)
Author:
chambers
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ps1sc template paper

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  • trunk/doc/release.2015/ps1.mission/mission.tex

    r37862 r37894  
    1 \documentclass[iop,floatfix]{emulateapj}
    2 % \pdfoutput=1
    3 
    4 % see latex.readme.txt for notes on using the PS1 template
    5 %\documentclass[12pt,preprint]{aastex}
     1% 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)
     2%Please send corrections or suggestions to stubbs-at-physics.harvard.edu
     3%
     4% This Latex template file is designed to be useful to PS-1 consortium authors.
     5% The authorship and publication policies of the project are available at
     6% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1SC_Publication_Policy
     7%
     8%The template assumes the AASTex style file, and the simple AAStex bibliography format.
     9%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
     10% PS1 CONVENTIONS:
     11%
     12% Note there are some conventions to which Pan-STARRS1 papers should conform:
     13% The survey and the survey telescope/camera/software system are Pan-STARRS1, or PS1.
     14% The passbands are g_p1, r_p1, etc. and it's important to use these subscripted
     15% terms in order to clearly distinguish the PS1 photometric system from SDSS and
     16% other photometric systems that have similar names. Confusion will erupt if we are
     17% careful about this. We urge our colleagues to adopt the terms g_sn, r_sn, etc.
     18% for the comparable SDSS photometric system, under release DR<n>.
     19%
     20% The MPC observatory code for PS1 is "F51"
     21%
     22% It is of utmost importance that we conform to the IAU object naming and designation standards.
     23%
     24%          The IAU designation for any new PS1 objects is "PSO JDDD.DDDD+DD.DDDD<x>" where the
     25%          space between PSO and the subsequent string is mandatory, as is the inclusion of the "J" (which designates J2000).
     26%          Any shortened names, such as PSO JDDD.D-DDDD must contain the J!
     27%            This also means coordinates in names are *truncated* rather than rounded, to x.xxxx significance in RA and x.xxxx in Dec.
     28%            Coordinates are reported in decimal degrees (J2000) for both RA and DEC, the four digits provides for 0.2" accuracy that
     29%          has been chosen to both exploit the absolute coordinate accuracy and to prevent confusion other than PSF blending.
     30%          The optional <x> is a single ASCII character that designates "child" objects derived from some primary object. This might include, for, example,
     31%          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
     32%          decimal point, but including "+" and "-", are intended to be part of a 64-bit integer, with the last byte reserved for the "x" character
     33%          in order to provide efficient hashing and searching for applications.
     34%
     35%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
     36% CHECKLIST:
     37%
     38% Here is a partial checklist for PS1 paper authors (detailed instructions at http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1SC_Publication_Policy):
     39%       - post intended project to the appropriate Key Project wiki site, and send email to KP leads and to science_council@ps1sc.org
     40%    - ensure that magnitudes are in g_p1, etc designation
     41%    - 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!
     42%    - ensure that any new objects have designations that conform to the IAU standard. See above.
     43%    - double-check the author list and institutional affiliations.
     44%   -  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.
     45%    - enter short title and short authors in appropriate place below
     46%    - conform to journal-specific guidelines
     47%    - Are PS1 system papers cited, as appropriate? Is relevant prior work cited (not just yours!) ? Copies of the system technical papers are available at
     48%              http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Publications
     49%    - 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, 
     50%           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,
     51%           but not all. The Table example below has an illustration of this.
     52%     - post paper draft to PS1SC through the consortium web site, at http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Publications
     53%     - then send email to scientists@ps1sc.org announcing that draft is available, soliciting comments. Paper is still embargoed within PS1SC.
     54%     - inform PS1 builders of the paper by sending email to builders@ps1sc.org, only positive affirmation implies inclusion.
     55%     - decide if your project merits a press release. If so, coordinate with Ken Chambers and Gareth Winn-Williams and others as appropriate.
     56%                standard phrasing for inclusion in Press Releases is at http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/Acknowledgment_for_PR
     57%     - after a 3 week interval, window for comments has closed. Any builders who did not explicitly request inclusion can be dropped.
     58%     - Revise as needed.
     59%     - In coordination with Key Project leadership, submit the paper.
     60%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
     61%
     62% This template has some Latex terms defined for your convenience, in the block below.
     63%
     64% Use trailing slash command after each of these to insert a space!
     65%
     66\documentclass[12pt,preprint]{aastex}
    667%\documentclass[manuscript]{aastex}
    768%\documentclass[preprint2]{aastex}
    869%\documentclass[preprint2,longabstract]{aastex}
    9 \RequirePackage{color}
    10 \input{astro.sty}
    11 
    12 % online version may use color, but print version needs b/w
    13 \def\plotmode{col}
    14 %\def\plotmode{bw}
    15 
    16 % arxiv needs PDF graphics, but publishers mostly was PS
    17 %\def\plotext{pdf}
    18 \def\plotext{ps}
    19 
    20 % use this to make the figure picture path flexible:
    21 %\def\picdir{PATH}
    22 \def\picdir{ALTPATH}
     70\newcommand{\gps}{\ensuremath{g_{\rm P1}}}
     71\newcommand{\rps}{\ensuremath{r_{\rm P1}}}
     72\newcommand{\ips}{\ensuremath{i_{\rm P1}}}
     73\newcommand{\zps}{\ensuremath{z_{\rm P1}}}
     74\newcommand{\yps}{\ensuremath{y_{\rm P1}}}
     75\newcommand{\wps}{\ensuremath{w_{\rm P1}}}
     76\newcommand{\grizy}{\gps\rps\ips\zps\yps}
     77\newcommand{\PS}{\protect \hbox {Pan-STARRS1}}
    2378
    2479% Pick a terse version of the title here;
    25 \shorttitle{PS1 Science Surveys}
    26 \shortauthors{K.C. Chambers et al}
     80\shorttitle{Pan-STARRS Aliens}
     81\shortauthors{U.H. Author et al}
    2782\begin{document}
    28 \title{The Pan-STARRS\,1 Science Surveys}
    29 
    30 % this is a crude trick to get the order of affiliations right.  These
    31 % names are used in the affiliations below.  The user needs to (1) set
    32 % the order and numbers to have the correct sequence in the author
    33 % list and (2) re-order the list at the bottom (and comment-out as needed)
    34 \def\IfA{1}
    35 \def\CfA{2}
    36 \def\MPIA{3}
    37 \def\Princeton{3}
    38 \def\USNO{4}
    39 \def\JHU{1}
    40 
     83\title{A Latex Template for the Production of Pan-STARRS1 Papers}
     84%
     85% PS1 paper authorship lists major paper contributors, followed by alphabetical list of PS1 builders,
     86% You'll want to shuffle the affiliation designations as needed. PS1 institutional addresses are
     87% provided below. Look here to get the most up-to-date list of builders and their institutional affiliations:
     88% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Builders_aastex
     89%
     90% Note that any authors not from PS-1 institutions,  that is not a PS1 builder, needs to secure external
     91% scientist status. Information on that process is available at
     92% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/Pending_External_Scientists
     93%
     94% This example has a first author from UH:
    4195\author{
    42 K.~C. Chambers,\altaffilmark{\IfA}
    43 IPP Team,
    44 %PS Builder List
    45 % W.~S. Burgett,\altaffilmark{\IfA}
    46 % K.~C. Chambers,\altaffilmark{\IfA}
    47 % L. Denneau,\altaffilmark{\IfA}
    48 % P. Draper,\altaffilmark{\DUR}
    49 % H.~A. Flewelling,\altaffilmark{\IfA}
    50 % T. Grav,\altaffilmark{\IfA}
    51 % J. N. Heasley,\altaffilmark{\IfA}
    52 % K. W. Hodapp,\altaffilmark{\IfA}
    53 % M. E. Huber,\altaffilmark{\IfA}
    54 % R. Jedicke,\altaffilmark{\IfA}
    55 % N. Kaiser,\altaffilmark{\IfA}
    56 % R.-P. Kudritzki,\altaffilmark{\IfA}
    57 % G. A. Luppino,\altaffilmark{\IfA}
    58 % R. H. Lupton,\altaffilmark{\Princeton}
    59 % E. A. Magnier,\altaffilmark{\IfA}
    60 % N. Metcalfe,\altaffilmark{\DUH}
    61 % D. G. Monet,\altaffilmark{\USNO}
    62 % J.~S. Morgan,\altaffilmark{\IfA}
    63 % P. M. Onaka,\altaffilmark{\IfA}
    64 % P.~A. Price,\altaffilmark{\Princeton}
    65 % C.~W. Stubbs,\altaffilmark{\CfA}
    66 % W.~E. Sweeney,\altaffilmark{\IfA}
    67 % J.~L. Tonry, \altaffilmark{\IfA}
    68 % R. J. Wainscoat,\altaffilmark{\IfA} and
    69 % C. Z. Waters,\altaffilmark{\IfA}
    70 } % this bracket terminates author list
     96U.H.Firstauthor,\altaffilmark{1}
     97I.M. Anauthor,\altaffilmark{2}
     98M.E. Too,\altaffilmark{3}
     99%PS Builder List, delete or comment out as needed if any appear above this line. Affiliation numbers will likely need to be shuffled
     100% here and correspondingly in the institution list below
     101% List updated by S. Smartt 2013-04-30 and 2013-06-25, after Board approval of additional Builders. Now matches
     102%http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Builders_aastex
     103
     104W. S. Burgett\altaffilmark{1},
     105K. C. Chambers\altaffilmark{1},
     106L. Denneau\altaffilmark{1},
     107P. Draper\altaffilmark{4},
     108H. Flewelling\altaffilmark{1},
     109T. Grav\altaffilmark{5},
     110J. N. Heasley\altaffilmark{1},
     111K. W. Hodapp\altaffilmark{1},
     112M. E. Huber\altaffilmark{1},
     113R. Jedicke\altaffilmark{1},
     114N. Kaiser\altaffilmark{1},
     115R.-P. Kudritzki\altaffilmark{1},
     116G. A. Luppino\altaffilmark{1},
     117R. H. Lupton\altaffilmark{6},
     118E. A. Magnier\altaffilmark{1},
     119N. Metcalfe\altaffilmark{2},
     120D. G. Monet\altaffilmark{7},
     121J. S. Morgan\altaffilmark{1},
     122P. M. Onaka\altaffilmark{1},
     123P. A. Price\altaffilmark{1},
     124C. W. Stubbs\altaffilmark{8},
     125W. Sweeney\altaffilmark{1},
     126J. L. Tonry\altaffilmark{1},
     127R. J. Wainscoat\altaffilmark{1}.
     128C. Waters\altaffilmark{1},
     129
     130% this bracket terminates author list
     131}
    71132
    72133% The ordering here should be sequential, matching the sequence in the list of authors:
    73 \altaffiltext{\IfA}{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822}
    74 % \altaffiltext{\CfA}{Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138}
    75 % \altaffiltext{\Princeton}{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA}
    76 % \altaffiltext{\USNO}{US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001, USA}
    77 % \altaffiltext{\DUH}{Durham, UK}
    78 % \altaffiltext{\JHU}{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA}
    79 % \altaffiltext{\MPIA}{Max Planck Institute for Astronomy, K\"onigstuhl 17, D-69117 Heidelberg, Germany}
     134\altaffiltext{1}{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822}
     135\altaffiltext{2}{Another most excellent PS1 partner institution, copy from list below}
     136\altaffiltext{3}{Another most excellent PS1 partner institution, copy from list below}
     137\altaffiltext{4}{Department of Physics, Durham University, South Road, Durham DH1 3LE, UK}
     138\altaffiltext{5}{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA}
     139\altaffiltext{6}{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA}
     140\altaffiltext{7}{US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001, USA}
     141\altaffiltext{8}{Department of Physics, Harvard University, Cambridge, MA 02138, USA}
     142
     143
     144% Here is a list of PS-1 Institution addresses, for inclusion above. send corrections to stubbs-at-physics.harvard.edu
     145%
     146%{Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822}
     147%{Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138}
     148%{Department of Physics, Harvard University, 17 Oxford Street, Cambridge MA 02138}
     149%{Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA}
     150%{Astrophysics Research Centre, School of Mathematics and Physics, QueenÕs University Belfast, Belfast, BT71NN, UK}
     151%{Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA}
     152%{US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001, USA}
     153%{Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, Postfach 1312, 85741 Garching, Germany}
     154%{Max Planck Institute for Astronomy, Kšnigstuhl 17, D-69117 Heidelberg, Germany}
     155%{Astrophysics Research Centre, School of Mathematics and Physics, QueenÕs University Belfast, Belfast, BT7 1NN, UK}
     156%{Department of Physics. University of Durham Science Laboratories, South Road Durham DH1 3LE, UK}
     157%{Las Cumbres Observatory Global Telescope Network, Inc.,6740 Cortona Dr. Suite 102 Santa Barbara CA 93117, USA}
     158 %{National Central University, 300 Jhongda Rd, Jhongli 32001, Taiwan }
     159%{SUPA, Institute for Astronomy, University of Edinburgh, Edinburgh, EH9 3HJ, UK}
     160%{Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA}
     161%
     162% Don't use our macros in the abstract, likely won't work right in arXiv server?
    80163\begin{abstract}
    81164
    82 Lorem ipsum dolor sit amet, consectetur adipiscing elit. Vestibulum
    83 bibendum nisi id tristique posuere. Duis eu mollis nulla. Maecenas est
    84 turpis, mattis tempor urna vitae, placerat rhoncus sem. Lorem ipsum
    85 dolor sit amet, consectetur adipiscing elit. Sed quis velit
    86 nisl. Aliquam erat volutpat. Cras lacinia, nisl tristique auctor
    87 molestie, dolor nulla rhoncus purus, ac accumsan nunc nunc ac
    88 nibh. Maecenas vitae mollis mauris. Ut sollicitudin pulvinar purus,
    89 eget luctus lorem tincidunt vitae. Vestibulum eu mattis neque. Nulla
    90 in tortor id urna dapibus gravida a vel leo.
    91 
     165The Pan-STARRS1 survey has obtained multi-epoch imaging in 5 bands (\grizy) over
     166the entire sky North of declination $-$30, and we have done good things with the results.
     167We have detected thousands of alien civilizations, some with measurable proper motions.
     168They are headed towards us.
    92169\end{abstract}
    93170
    94171% insert additional keywords as appropriate:
    95 \keywords{Surveys:\PSONE }
    96 
    97 \section{OUTLINE}
    98 \begin{verbatim}
    99 * Introduction
    100  * Previous similar surveys
    101   * POSS
    102   * SDSS
    103   * 2MASS
    104  * Science Drivers
    105  * Initial Proposal (PS4)
    106 * PS1 Observatory Description
    107  * PS1 Telescope Description
    108   * Physical Characteristics
    109   * Construction
    110  * GPC1 camera
    111 * PS1 Surveys
    112  * 3PI
    113  * MD
    114  * Solar System
    115  * STS
    116  * M31
    117 * Data Quality
    118  * Image Quality
    119  * Observing Efficiency
    120  *
    121 * Science Key Projects
    122 * Data Release
    123 \end{verbatim}
    124 
    125 \section{INTRODUCTION}\label{sec:intro}
    126 
    127 \section{Pan-STARRS1}
    128 
    129 \section{PS1 Observatory Description}
    130 
    131 \section{PS1 Science Surveys}
    132 
    133 \section{Data Quality / Data Metrics?}
    134 
    135 \section{Science Key Projects}
    136 
    137 \section{Data Release}
    138 
    139 \section{Discussion}
    140 
    141 \section{Conclusion}
     172\keywords{Surveys:\PS }
     173
     174\vfil
     175\eject
     176\clearpage
     177
     178\section{INTRODUCTION}
     179\label{sec:intro}
     180
     181We present our most excellent results from \PS.   
     182
     183% Note trailing slash after shorthand commands to force an appropriate space, when needed.
     184
     185The remainder of the introduction summarizes the \PS\ survey system. The observations we used are described in Section
     186\ref{sec:observations}. Data processing is outlined in Section \ref{sec:processing},
     187and results are shown in Section \ref{sec:results}, followed by our conclusions and discussion in Section \ref{sec:discussion}.
     188
     189%%%%%%%%%%%%%%%%%%%%%%%
     190% Boilerplate system description begins here. This is presented to save PS1 authors some time, keep/modify as much of this as you
     191% think appropriate. Or write your own... You can download the PS1 technical papers from
     192% http://ps1sc.ifa.hawaii.edu/PS1wiki/index.php/PS1_Publications
     193% (see the bottom of the wiki page).
     194
     195\subsection{The Pan-STARRS1 Telescope, Camera, and Image Processing}
     196
     197The Pan-STARRS1 system is a high-etendue wide-field imaging system, designed for dedicated survey observations. The system
     198is installed on the peak of Haleakala on the island of Maui in the Hawaiian island chain. Routine observations are conducted remotely,
     199from the Waiakoa Laboratory in Pukalani.  We provide below a terse summary of the Pan-STARRS1 survey instrumentation.
     200A more complete description of the Pan-STARRS1 system, both hardware and software, is provided by \cite{PS1_system}. The
     201survey philosophy and execution strategy are described in \cite{PS_MDRM}.
     202
     203The Pan-STARRS1 optical design \citep{PS1_optics} uses a 1.8~meter diameter $f$/4.4 primary mirror, and a 0.9~m secondary.
     204The resulting converging beam then passes through two refractive correctors, an
     205interference filter with a clear aperture diameter of 496 mm, and a final refractive corrector that is the
     206dewar window. The telescope illuminates a diameter of 3.3 degrees, with low distortion,
     207with some vignetting at the edges of this illuminated region.
     208The 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. 
     209The detectors are back-illuminated CCDs manufactured by Lincoln Laboratory.  The detectors are read out using a StarGrasp CCD controller,
     210with a readout time of 7 seconds for a full unbinned image. Initial performance assessments are presented in \cite{PS1_GPCB}.
     211
     212%note trailing slash command where space required after passband macros
     213The \PS\ observations are obtained through a set of five broadband
     214filters, which we have designated as \gps, \rps, \ips, \zps, and
     215\yps. Under certain circumstances \PS\ observations are obtained with
     216a sixth, ``wide'' filter designated as \wps\ that essentially spans
     217\gps, \rps, and \ips.  Although the filter system for \PS\ has much in
     218common with that used in previous surveys, such as SDSS \citep{SDSS}, there
     219are important differences. The \gps\ filter extends 20~nm redward of
     220$g_{SDSS}$, paying the price of 5577\AA\ sky emission for greater
     221sensitivity and lower systematics for photometric redshifts, and the
     222\zps\ filter is cut off at 930~nm, giving it a different response than
     223the detector response defined $z_{SDSS}$.  SDSS has no corresponding
     224\yps\ filter.  Further information on the passband shapes is described
     225in \cite{PS_lasercal}. 
     226Provisional response
     227functions (including 1.3 airmasses of atmosphere) are available
     228at 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\ 
     229system, $m=-2.5log(flux)+m'$, with a single zeropoint adjustment $m'$ made in each band to conform to the AB magnitude scale \citep{JTphoto}.
     230\PS\ magnitudes are interpreted as being at the top of the atmosphere, with  1.3 airmasses of atmospheric attenuation being included in the
     231system response function. No correction for Galactic extinction is applied to the \PS\ magnitudes.
     232We stress that, like SDSS, \PS\ uses the AB
     233photometric system and there is no arbitrariness in the definition. Flux representations are limited
     234only by how accurately we know the system response function vs. wavelength.
     235
     236Images obtained by the Pan-STARRS1 system are processed through the Image Processing Pipeline (IPP) \citep{PS1_IPP},
     237on a computer cluster at the Maui High Performance Computer Center. The pipeline runs the images through a succession of stages,
     238including flat-fielding (``de-trending''), a flux-conserving warping to a sky-based image plane, masking and artifact removal, and object detection and
     239photometry. The IPP also performs image subtraction to allow for the prompt detection of variables and transient phenomena. Mask and variance arrays
     240are carried forward at each stage of the IPP processing. Photometric and astrometric measurements performed by the IPP system are described in \cite{PS1_photometry}
     241and \cite{PS1_astrometry} respectively.
     242
     243The details of the photometric calibration and the \PS\ zeropoint
     244scale will be presented in a subsequent publication \citep{JTphoto},
     245and \cite{EMphoto} will provide the application to a consistent
     246photometric catalog over the 3/4 sky observed by \PS. 
     247
     248% Boilerplate system description ends here.
     249%%%%%%%%%%%%%%%%%%%
     250
     251\section{OBSERVATIONS}
     252\label{sec:observations}
     253
     254% define which set of PS1 observations went into your paper.
     255This paper uses images and photometry from the Pan-STARRS1 Medium-Deep Field survey. In addition
     256to covering the sky at $\delta>-30\deg$ in 5 bands, 
     257the Pan-STARRS1 survey has obtained deeper multi-epoch images in the PS1 \gps, \rps, \ips, \zps\ and \yps\ bands of the
     258fields listed in Table \ref{table:fields}. The typical Medium-deep cadence of observations is presented in Table \ref{table:cadence},
     259and the 5 $\sigma$ point source detection limits achieved in the various \grizy\ bands, as well as other statistics of
     260potential interest, are presented in Table \ref{table:depths}, for
     261the co-added stacks over the observing period presented here.
     262
     263% This is an illustration of a simple Table. The coordinates of the Medium-Deep fields are correct, and
     264% are the actual telescope boresight pointings and supersede any prior list.PS1 uses decimal degrees (J2000) for
     265% both RA and DEC.
     266
     267\begin{table}[htdp]
     268\caption{\PS\ Medium-Deep Field Centers. }
     269\begin{center}
     270\begin{tabular}{lrr}
     271\hline
     272\hline
     273{\bf Field} & {\bf RA (degrees, J2000)} & {\bf Dec (degrees, J2000)} \\
     274\hline
     275MD00  &  10.675 & $ 41.267$ \\
     276MD01  &  35.875 & $ -4.250$ \\
     277MD02  &  53.100 & $-27.800$ \\
     278MD03  & 130.592 & $ 44.317$ \\
     279MD04  & 150.000 & $  2.200$ \\
     280MD05  & 161.917 & $ 58.083$ \\
     281MD06  & 185.000 & $ 47.117$ \\
     282MD07  & 213.704 & $ 53.083$ \\
     283MD08  & 242.787 & $ 54.950$ \\
     284MD09  & 334.188 & $  0.283$ \\
     285MD10  & 352.312 & $ -0.433$ \\
     286MD11  & 270.000 & $ 66.561$ \\
     287\hline
     288\end{tabular}
     289\end{center}
     290\label{table:fields}
     291\end{table}
     292
     293
     294\begin{table}[htdp]
     295\caption{\PS\ Medium-Deep Survey, typical cadence. FM$\pm$3 designates 3 nights on either side of Full Moon.}
     296\begin{center}
     297\begin{tabular}{ccr}
     298\hline
     299\hline
     300{\bf Night} & {\bf Filter} & {\bf Exposure Time} \\
     301\hline
     3021         & \gps \& \rps & 8$\times$113s each\\
     3032         & \ips         & 8$\times$240s \\
     3043         & \zps         & 8$\times$240s \\
     3054          & \gps \& \rps & 8$\times$113s each \\
     306repeats... & \nodata & \nodata \\
     307FM$\pm3$  & \yps         & 8$\times$240s \\
     308\hline
     309\end{tabular}
     310\end{center}
     311\label{table:cadence}
     312\end{table}
     313
     314% These are the detection limits for Medium-Deep analysis done by Tonry as of May 31, 2011.
     315\begin{table}[htdp]
     316\caption{\PS\ MDF Statistics, Apr 2009--Apr 2011.}
     317\begin{center}
     318\begin{tabular}{lcrcccclcrcccc}
     319\hline
     320\hline
     321Field&Filter& $N$ & $\log t$ & $PSF$ & $\langle w\rangle$ & $m_{lim}$ &
     322Field&Filter& $N$ & $\log t$ & $PSF$ & $\langle w\rangle$ & $m_{lim}$\\
     323\hline
     324MD01 & g & 42 & 4.7 & 1.25 & 1.55 & 24.5 & MD06 & g & 38 & 4.6 & 1.25 & 1.56 & 24.4\\
     325MD01 & r & 42 & 4.7 & 1.15 & 1.35 & 24.4 & MD06 & r & 39 & 4.6 & 1.18 & 1.45 & 24.2\\
     326MD01 & i & 41 & 4.9 & 1.05 & 1.27 & 24.4 & MD06 & i & 41 & 4.9 & 1.14 & 1.39 & 24.3\\
     327MD01 & z & 41 & 4.9 & 1.03 & 1.24 & 23.9 & MD06 & z & 38 & 4.9 & 1.05 & 1.30 & 23.7\\
     328MD01 & y & 21 & 4.6 & 0.95 & 1.17 & 22.4 & MD06 & y & 24 & 4.7 & 1.00 & 1.25 & 22.4\\
     329MD02 & g & 30 & 4.5 & 1.31 & 1.79 & 24.2 & MD07 & g & 36 & 4.5 & 1.23 & 1.68 & 24.3\\
     330MD02 & r & 29 & 4.5 & 1.20 & 1.74 & 24.1 & MD07 & r & 39 & 4.5 & 1.13 & 1.46 & 24.2\\
     331MD02 & i & 30 & 4.8 & 1.11 & 1.50 & 24.2 & MD07 & i & 39 & 4.9 & 1.14 & 1.44 & 24.2\\
     332MD02 & z & 33 & 4.8 & 1.06 & 1.30 & 23.6 & MD07 & z & 43 & 4.9 & 1.08 & 1.37 & 23.7\\
     333MD02 & y & 16 & 4.5 & 1.14 & 1.42 & 22.1 & MD07 & y & 30 & 4.8 & 1.01 & 1.28 & 22.5\\
     334MD03 & g & 38 & 4.6 & 1.18 & 1.44 & 24.5 & MD08 & g & 38 & 4.5 & 1.27 & 1.68 & 24.3\\
     335MD03 & r & 37 & 4.6 & 1.09 & 1.28 & 24.4 & MD08 & r & 38 & 4.5 & 1.14 & 1.47 & 24.2\\
     336MD03 & i & 41 & 4.9 & 1.06 & 1.31 & 24.4 & MD08 & i & 33 & 4.8 & 1.07 & 1.34 & 24.2\\
     337MD03 & z & 42 & 5.0 & 1.03 & 1.27 & 23.9 & MD08 & z & 40 & 4.9 & 1.09 & 1.39 & 23.7\\
     338MD03 & y & 20 & 4.6 & 1.00 & 1.36 & 22.4 & MD08 & y & 32 & 4.9 & 0.98 & 1.27 & 22.7\\
     339MD04 & g & 35 & 4.6 & 1.17 & 1.52 & 24.5 & MD09 & g & 34 & 4.5 & 1.26 & 1.55 & 24.3\\
     340MD04 & r & 37 & 4.6 & 1.09 & 1.46 & 24.3 & MD09 & r & 33 & 4.5 & 1.15 & 1.42 & 24.1\\
     341MD04 & i & 35 & 4.9 & 1.07 & 1.35 & 24.3 & MD09 & i & 34 & 4.8 & 1.02 & 1.36 & 24.3\\
     342MD04 & z & 28 & 4.8 & 1.03 & 1.32 & 23.6 & MD09 & z & 34 & 4.8 & 1.02 & 1.26 & 23.7\\
     343MD04 & y &  8 & 4.3 & 1.03 & 1.21 & 22.0 & MD09 & y & 12 & 4.3 & 0.94 & 1.12 & 22.0\\
     344MD05 & g & 42 & 4.6 & 1.24 & 1.58 & 24.4 & MD10 & g & 30 & 4.5 & 1.26 & 1.60 & 24.2\\
     345MD05 & r & 40 & 4.6 & 1.17 & 1.46 & 24.3 & MD10 & r & 33 & 4.5 & 1.18 & 1.53 & 24.2\\
     346MD05 & i & 34 & 4.8 & 1.06 & 1.44 & 24.3 & MD10 & i & 30 & 4.8 & 1.01 & 1.31 & 24.2\\
     347MD05 & z & 27 & 4.8 & 0.99 & 1.27 & 23.6 & MD10 & z & 28 & 4.8 & 1.03 & 1.24 & 23.6\\
     348MD05 & y & 17 & 4.6 & 1.02 & 1.33 & 22.3 & MD10 & y & 11 & 4.4 & 0.96 & 1.22 & 22.2\\
     349MD11 & g &  1 & 3.0 & 1.17 & 1.45 & 22.4 & MD00 & g &   \nodata & \nodata & \nodata & \nodata &  \nodata\\
     350MD11 & r &  1 & 3.0 & 1.12 & 1.30 & 22.3 & MD00 & r &101 & 4.9 & 1.03 & 1.30 & 24.8\\
     351MD11 & i &  3 & 3.8 & 1.13 & 1.47 & 22.9 & MD00 & i & 66 & 4.6 & 0.96 & 1.25 & 24.0\\
     352MD11 & z &  4 & 3.9 & 1.34 & 1.81 & 22.2 & MD00 & z &   \nodata & \nodata & \nodata & \nodata &  \nodata\\
     353MD11 & y &  5 & 4.0 & 0.96 & 1.21 & 21.6 & MD00 & y &  \nodata & \nodata & \nodata & \nodata &  \nodata\\
     354\end{tabular}
     355\label{table:depths}
     356\end{center}
     357\tablecomments{$N$ is the number of nights of observation,
     358  $\log t$ is the $\log_{10}$ of the net exposure time
     359  in sec, ``$PSF$'' is the DoPhot FWHM of the {\it core-skirt} PSF in the
     360  stack-stacks, $\langle w\rangle$ is the median IPP FWHM of the observations,
     361  and $m_{lim}$ is the 5$\sigma$ detection limit for point sources.}
     362
     363\end{table}
     364
     365\section{DATA PROCESSING}
     366\label{sec:processing}
     367
     368The Pan-STARRS1 IPP system performed flatfielding on each of the individual images, using white light flatfield images
     369from a dome screen, in combination with an illumination correction obtained by rastering sources across the
     370field of view. Bad pixel masks were applied, and carried forward for use in the stacking stage. After determining
     371an initial astrometric solution, the flat-fielded images were then warped onto the tangent plane of the sky, using a flux
     372conserving algorithm. The plate scale for the warped images is 0.200 arcsec/pixel.
     373
     374\section{RESULTS}
     375\label{sec:results}
     376
     377Our most excellent results were produced by turning each \PS\ image upside down and shaking vigorously.
     378The extragalactic civilizations we detected are listed in Table \ref{table:PS1_list}. For those in a recumbent
     379pose, a rotated version of the discovery table is provided in Table \ref{table:deluxerotated}. An example of an
     380illustration is presented in Figure \ref{fig:phot}.
     381
     382%there are numerous ways to include figures, here is one:
     383\begin{figure}[htbp]
     384\begin{center}
     385\centerline{\includegraphics[width=6.5in]{Luptitudes_SDSS_Deviation.ps}}
     386\caption{The SDSS magnitude definition departs from $2.5 log(flux)$ convention at faint magnitudes.
     387{\it Caveat emptor}. This is but one of many reasons to clearly designate which photometric system is
     388being used, and one reason why we insist on the \grizy\ nomenclature. The authors thank M. Wood-Vasey for generating this plot.}
     389\label{fig:phot}
     390\end{center}
     391\end{figure}
     392
     393
     394\clearpage
     395
     396% Note excellent use of trailing slash to force a space after \yps, thanks to Michael Wood-Vasey:
     397{\bf Please conform to the \gps, \rps, \ips, \zps, \yps, \wps\ convention when reporting PS1 magnitudes, and to the (provisional)
     398IAU convention for object names:
     399
     400PSO JRRR.rrrr+DD.dddd
     401
     402\noindent
     403where RRR.rrrr and +DD.dddd are RA and Dec in decimal degrees (J2000). Keep this number of digits of precision, please, but no more.
     404See preamble comments in Tex template for further information.}
     405
     406%Example tables with PS1 objects, including tags for linkage to external databases.
     407% The IAU conventions on naming objects should be rigorously followed. See
     408% http://cdsarc.u-strasbg.fr/vizier/Dic/iau-spec.htx#3.6
     409% See also http://www.sdss.org/DR3/coverage/IAU.html.
     410% Note coordinates are truncated and not rounded, for generating names!
     411%
     412% Note the use of \object{} tag on OBJID column. See recent AASTex documentation for
     413% how links can be made to external data sets.
     414
     415
     416
     417\clearpage
     418\begin{table}[htdp]
     419\caption{Pan-STARRS1 Candidate Detections of other Civilizations in the Galaxy. All astrometry is for equinox J2000 and  epoch MJD=xxxx.
     420Magnitudes are on the Pan-STARRS1 \grizy\ system.}
     421\begin{center}
     422\begin{tabular}{cccccc}
     423\hline
     424\hline
     425 OBJID &  RA (J2000)  &   Dec (J2000) &  \gps &  $\sigma\gps$ & Number of Aliens \\
     426\hline
     427\object{PSO J130.0586+44.3216} &  130.0586 & +44.3216  & 23.35 & 0.08 & about two billion \\
     428\hline
     429\end{tabular}
     430\end{center}
     431\label{table:PS1_list}
     432\end{table}%
     433
     434% this is a fancier table, rotated to fit more columns. Note the use of \object{} tag on OBJID column. See recent AASTex documentation for
     435% how links can be made to external data sets.
     436\clearpage
     437\begin{deluxetable}{rrrrrrrrrr}
     438\rotate
     439\tablewidth{9in}
     440\tablecolumns{10}
     441\tablecaption{Pan-STARRS1 Detections of Alien Civilizations, Rotated}
     442\tablehead{
     443\colhead{OBJID} &
     444\colhead{RA (J2000)}   &
     445\colhead{Dec (J2000)}    &
     446\colhead{\gps} &
     447\colhead{$\sigma$\gps}    &
     448\colhead{\rps} &
     449\colhead{$\sigma$\rps}    &
     450\colhead{\yps} &
     451\colhead{$\sigma$\yps}    &
     452\colhead{Alien Population}
     453}
     454\startdata
     455\object{PSO J130.0586+44.3216} &  130.0586 & +44.3216  &
     45623.24 & 0.04 & 24.52 & 0.10   & \nodata &  \nodata & 1 Billion \\
     457\enddata
     458\label{table:deluxerotated}
     459\end{deluxetable}
     460
     461\section{DISCUSSION}
     462\label{sec:discussion}
     463
     464We conclude that this works all too well. The aliens will be here soon.
     465
     466%please leave this part in:
     467{\it Facilities:} \facility{PS1 (GPC1)}
     468
     469\acknowledgments
     470
     471% You'll want to add any other grants, etc. here but this aspect is mandatory for PS1 papers:
     472The 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.
     473
     474\clearpage
     475% Some PS1 hardware and software papers are included below, use as you see fit but it's certainly appropriate to cite PS1 system papers!
     476\begin{thebibliography}
     477
     478% SDSS reference
     479\bibitem[Abazajian, K.~N. {\it et al.}(2009)]{SDSS} Abazajian, K.~N. {\it et al.} (The SDSS Collaboration) \ 2009 \apjs,  {\bf 182}, 543.
     480%PS1 Modified Design Reference Mission
     481
     482\bibitem[Chambers {\it et al.}(in prep)]{PS_MDRM} Chambers, K.~C,  {\it et al.}, in preparation.
     483
     484%PS1 Optical Design
     485\bibitem[Hodapp {\it et al.}(2004)]{PS1_optics} Hodapp, K.~W., Siegmund,
     486W.~A., Kaiser, N., Chambers, K.~C., Laux, U., Morgan, J.,
     487\& Mannery, E.\ 2004, \procspie, {\bf 5489}, 667
     488
     489%PS1 system overview paper.
     490\bibitem[Kaiser {\it et al.}(2010)]{PS1_system} Kaiser, N., {\it et al.} \ 2010, \procspie, {\bf 7733},  12K.
     491
     492%References to IPP pipeline:
     493%Overall IPP reference
     494\bibitem[Magnier(2006)]{PS1_IPP} Magnier, E.\ 2006, Proceedings of The Advanced
     495Maui Optical and Space Surveillance Technologies Conference, Ed.: S. Ryan, The Maui Economic Development Board, p.E5
     496
     497%IPP photometry
     498\bibitem[Magnier(2007)]{PS1_photometry} Magnier, E.\ 2007, The Future
     499of Photometric, Spectrophotometric and Polarimetric Standardization, ASP Conference Series {\bf 364}, 153
     500
     501%IPP astrometry
     502\bibitem[Magnier {\it et al.}(2008)]{PS1_astrometry} Magnier, E.~A., Liu,
     503M., Monet, D.~G., \& Chambers, K.~C.\ 2008, IAU Symposium, {\bf 248}, 553
     504
     505% Photometric catalog
     506\bibitem[Magnier {\it et al.}(in prep)]{EMphoto} Magnier, E.,  {\it et al.}, in preparation.
     507
     508%GPC-1 camera paper B
     509\bibitem[Onaka {\it et al.}(2008)]{PS1_GPCB} Onaka, P., Tonry, J.~L.,
     510Isani, S., Lee, A., Uyeshiro, R., Rae, C., Robertson, L.,
     511\& Ching, G.\ 2008, \procspie, {\bf 7014}, 12O
     512
     513% Laser calibration of PS1 system throughput
     514\bibitem[Stubbs {\it et al.~}(2010)]{PS_lasercal} Stubbs, C.~W., Doherty,
     515P., Cramer, C., Narayan, G., Brown, Y.~J., Lykke, K.~R., Woodward, J.~T.,
     516\& Tonry, J.~L.\ 2010, \apjs, {\bf 191}, 376
     517
     518% GPC-1 camera paper A
     519\bibitem[Tonry \& Onaka(2009)]{PS1_GPCA} Tonry, J., \& Onaka, P.\ 2009, Advanced Maui Optical and Space Surveillance Technologies Conference,
     520Proceedings of the Advanced Maui Optical and Space Surveillance Technologies Conference, Ed.: S. Ryan, p.E40.   
     521
     522% Photometric system calibration papers
     523\bibitem[Tonry {\it et al.~}(in prep)]{JTphoto} Tonry, J.~L.,  {\it et al.}, in preparation.
     524
     525
     526\end{thebibliography}
     527
    142528
    143529\end{document}
     530                                                                       
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