The SDSS-III Baryon Oscillation Spectroscopic Survey: Quasar Target Selection for Data Release Nine
Creators: name: Ross, Nicholas P.
name: Myers, Adam D.
name: Sheldon, Erin S.
name: Yèche, Christophe
name: Strauss, Michael A.
name: Bovy, Jo
name: Kirkpatrick, Jessica A.
name: Richards, Gordon T.
name: Aubourg, Eric
name: Blanton, Michael R.
name: Brandt, W. N.
name: Carithers, William C.
name: Croft, Rupert A. C.
name: da Silva, Robert
name: Dawson, Kyle
name: Eisenstein, Daniel J.
name: Hennawi, Joseph F.
name: Ho, Shirley
name: Hogg, David W.
name: Lee, Khee-Gan
name: Lundgren, Britt
name: McMahon, Richard G.
name: Miralda-Escude, Jordi
name: Palanque-Delabrouille, Nathalie
name: Paris, Isabelle
name: Petitjean, Patrick
name: Pieri, Matthew M.
name: Rich, James
name: Roe, Natalie A.
name: Schiminovich, David
name: Schlegel, David J.
name: Schneider, Donald P.
name: Slosar, Anže
name: Suzuki, Nao
name: Tinker, Jeremy L.
name: Weinberg, David H.
name: Weyant, Anya
name: White, Martin
name: Wood-Vasey, W. Michael
Publisher: name: arXiv
Year: 2011
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS), a five-year spectroscopic survey of 10,000 deg^2, achieved first light in late 2009. One of the key goals of BOSS is to measure the signature of baryon acoustic oscillations in the distribution of Ly-alpha absorption from the spectra of a sample of ~150,000 z&gt;2.2 quasars. Along with measuring the angular diameter distance at z\approx2.5, BOSS will provide the first direct measurement of the expansion rate of the Universe at z &gt; 2. One of the biggest challenges in achieving this goal is an efficient target selection algorithm for quasars over 2.2 &lt; z &lt; 3.5, where their colors overlap those of stars. During the first year of the BOSS survey, quasar target selection methods were developed and tested to meet the requirement of delivering at least 15 quasars deg^-2 in this redshift range, out of 40 targets deg^-2. To achieve these surface densities, the magnitude limit of the quasar targets was set at g &lt;= 22.0 or r&lt;=21.85. While detection of the BAO signature in the Ly-alpha absorption in quasar spectra does not require a uniform target selection, many other astrophysical studies do. We therefore defined a uniformly-selected subsample of 20 targets deg^-2, for which the selection efficiency is just over 50%. This "CORE" subsample will be fixed for Years Two through Five of the survey. In this paper we describe the evolution and implementation of the BOSS quasar target selection algorithms during the first two years of BOSS operations. We analyze the spectra obtained during the first year. 11,263 new z&gt;2.2 quasars were spectroscopically confirmed by BOSS. Our current algorithms select an average of 15 z &gt; 2.2 quasars deg^-2 from 40 targets deg^-2 using single-epoch SDSS imaging. Multi-epoch optical data and data at other wavelengths can further improve the efficiency and completeness of BOSS quasar target selection. [Abridged]
description: 33 pages, 26 figures, 12 tables and a whole bunch of quasars. Submitted to ApJ