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A study of quasar selection in the supernova fields of the Dark Energy Survey

Research output: Contribution to journalArticle

  • Suk Sien Tie
  • Paul Martini
  • Dale Mudd
  • Fernanda Ostrovski
  • Sophie L. Reed
  • Christopher E. Lidman
  • Christopher S. Kochanek
  • Tamara M. Davis
  • Rob Sharp
  • S. A. Uddin
  • A. L. King
  • William Wester
  • B. E. Tucker
  • Douglas L. Tucker
  • Elizabeth J. Buckley-Geer
  • D. Carollo
  • Michael J. Childress
  • Karl Glazebrook
  • Samuel R. Hinton
  • G. Lewis
  • E. Macaulay
  • C. R. O'Neill
  • T. M. C. Abbott
  • Filipe B. Abdalla
  • J. Annis
  • A. Benoit-Lévy
  • Emmanuel Bertin
  • David Brooks
  • A. Carnero Rosell
  • M. Carrasco Kind
  • Jorge Carretero
  • Carlos E. Cunha
  • Luiz Alberto Nicolaci da Costa
  • Darren L. Depoy
  • Shantanu Desai
  • Peter Doel
  • Tim F. Eifler
  • August E. Evrard
  • David A. Finley
  • Brenna Flaugher
  • Pablo Fosalba
  • Josh Frieman
  • J. García-Bellido
  • E. Gaztanaga
  • David W. Gerdes
  • Daniel A. Goldstein
  • Daniel Gruen
  • Robert A. Gruendl
  • Gaston R. Gutierrez
  • Klaus Honscheid
  • David J. James
  • Kyler Kuehn
  • Nikolay Kuropatkin
  • Marcos Lima
  • Marcio Antonio Geimba Maia
  • Jennifer L. Marshall
  • F. Menanteau
  • Christopher J. Miller
  • Ramon Miquel
  • B. D. Nord
  • Ricardo L. C. Ogando
  • Andres A. Plazas
  • A. Kathy Romer
  • E. J. Sanchez
  • Basilio Xavier Santiago
  • Vic Scarpine
  • Michael Schubnell
  • Ignacio Sevilla-Noarbe
  • R. C. Smith
  • Marcelle Soares-Santos
  • Flavia Sobreira
  • Eric Suchyta
  • Molly E. C. Swanson
  • Gregory Tarle
  • A. R. Walker

We present a study of quasar selection using the supernova fields of the Dark Energy Survey (DES). We used a quasar catalog from an overlapping portion of the SDSS Stripe 82 region to quantify the completeness and efficiency of selection methods involving color, probabilistic modeling, variability, and combinations of color/probabilistic modeling with variability. In all cases, we considered only objects that appear as point sources in the DES images. We examine color selection methods based on the Wide-field Infrared Survey Explorer (WISE) mid-IR color, a mixture of WISE and DES colors (g - i and ), and a mixture of Vista Hemisphere Survey and DES colors (g - i and i - K). For probabilistic quasar selection, we used XDQSO, an algorithm that employs an empirical multi-wavelength flux model of quasars to assign quasar probabilities. Our variability selection uses the multi-band χ 2-probability that sources are constant in the DES Year 1 griz-band light curves. The completeness and efficiency are calculated relative to an underlying sample of point sources that are detected in the required selection bands and pass our data quality and photometric error cuts. We conduct our analyses at two magnitude limits, i < 19.8 mag and i < 22 mag. For the subset of sources with W1 and W2 detections, the color or XDQSOz method combined with variability gives the highest completenesses of >85% for both i-band magnitude limits and efficiencies of >80% to the bright limit and >60% to the faint limit; however, the giW1 and giW1+variability methods give the highest quasar surface densities. The XDQSOz method and combinations of W1W2/giW1/XDQSOz with variability are among the better selection methods when both high completeness and high efficiency are desired. We also present the OzDES Quasar Catalog of 1263 spectroscopically confirmed quasars from three years of OzDES observation in the 30 deg2 of the DES supernova fields. The catalog includes quasars with redshifts up to z ∼ 4 and brighter than i = 22 mag, although the catalog is not complete up to this magnitude limit.

Original languageEnglish
Article number107
JournalThe Astronomical Journal
Volume153
Issue number3
DOIs
Publication statusPublished - 15 Feb 2017

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  • Tie_2017_AJ_153_107

    Rights statement: The final published version of this article by S. S. Tie et al 2017 ApJ 153 107 is available online at https://doi.org/10.3847/1538-3881/aa5b8d. © 2017. The American Astronomical Society. All rights reserved.

    Final published version, 3.59 MB, PDF document

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