Deep CFHT Y-band Imaging of VVDS-F22 Field. II. Quasar Selection and Quasar Luminosity Function
McGreer, Ian D.
AffiliationUniv Arizona, Steward Observ
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PublisherIOP PUBLISHING LTD
CitationDeep CFHT Y-band Imaging of VVDS-F22 Field. II. Quasar Selection and Quasar Luminosity Function 2018, 155 (3):110 The Astronomical Journal
JournalThe Astronomical Journal
Rights© 2018. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractWe report the results of a faint quasar survey in a one-square-degree field. The aim is to test the Y - K/g - z and J - K/i - Y color selection criteria for quasars at faint magnitudes to obtain a complete sample of quasars based on deep optical and near-infrared color-color selection and to measure the faint end of the quasar luminosity function (QLF) over a wide redshift range. We carried out a quasar survey based on the Y - K/g - z and J - K/i - Y quasar selection criteria, using the deep Y-band data obtained from our CFHT/WIRCam Y-band images in a two-degree field within the F22 field of the VIMOS VLT deep survey, optical co-added data from Sloan Digital Sky Survey Stripe 82 and deep near-infrared data from the UKIDSS Deep Extragalactic Survey in the same field. We discovered 25 new quasars at 0.5 < z < 4.5 and i < 22.5 mag within one-square-degree field. The survey significantly increases the number of faint quasars in this field, especially at z similar to 2-3. It confirms that our color selections are highly complete in a wide redshift range (z < 4.5), especially over the quasar number density peak at z similar to 2-3, even for faint quasars. Combining all previous known quasars and new discoveries, we construct a sample with 109 quasars and measure the binned QLF and parametric QLF. Although the sample is small, our results agree with a pure luminosity evolution at lower redshift and luminosity evolution and density evolution model at redshift z > 2.5.
VersionFinal published version
SponsorsNSFC [11373008, 11533001]; Chinese Academy of Sciences [XDB09000000]; National Key Basic Research Program of China [2014CB845700]; Ministry of Science and Technology of China [2016YFA0400703]; NSFC of China [11333001, 11173001, 11033005]; US NSF [AST 15-15115]; NASA ADAP [NNX17AF28G]; TR33 project "The Dark Universe" - DFG; Strategic Priority Research Program "The Emergence of Cosmological Structures" [XDB09000000]; National Astronomical Observatories; Chinese Academy of Sciences; Ministry of Finance in China; Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University