Target Selection and Validation of DESI Luminous Red Galaxies
Rongpu ZhouLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]Biprateep DeyDepartment of Physics and Astronomy and PITT PACC, University of Pittsburgh, Pittsburgh, PA 15260, USAJeffrey A. NewmanDepartment of Physics and Astronomy and PITT PACC, University of Pittsburgh, Pittsburgh, PA 15260, USADaniel J. EisensteinCenter for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USAKyle DawsonDepartment of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USAS. BaileyLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]A. BertiDepartment of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USAJ. GuyLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]Ting-Wen LanGraduate Institute of Astrophysics and Department of Physics, National Taiwan University, No. 1, Sec. 4, Roosevelt Road, Taipei 10617, TaiwanH. ZouNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing, 100101, People's Republic of ChinaJ. AguilarLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]S. AhlenPhysics Dept., Boston University, 590 Commonwealth Avenue, Boston, MA 02215, USAShadab AlamInstitute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UKDavid BrooksDepartment of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UKAxel de la MacorraInstituto de Física, Universidad Nacional Autónoma de México, Cd. de México C.P. 04510, MéxicoArjun DeyNSF’s National Optical-Infrared Astronomy Research Laboratory, 950 N. Cherry Avenue, Tucson, AZ 85719, USAG. DhunganaDepartment of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75275, USAE. ChaussidonCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAAndreu Font-RiberaInstitut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra Barcelona, SpainSatya Gontcho A GontchoDepartment of Physics and Astronomy, University of Rochester, 500 Joseph C. Wilson Boulevard, Rochester, NY 14627, USAK. HonscheidCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAMustapha IshakDepartment of Physics, The University of Texas at Dallas, Richardson, TX 75080, USATheodore KisnerLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]András KovácsDepartamento de Astrofísica, Universidad de La Laguna (ULL), E-38206, La Laguna, Tenerife, SpainAnthony KreminLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]Martin LandriauLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]M. E. LeviLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]C. MagnevilleUniversité Paris-SaclayMarc ManeraInstitut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra Barcelona, SpainJ. ErezaCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAAaron MeisnerNSF’s National Optical-Infrared Astronomy Research Laboratory, 950 N. Cherry Avenue, Tucson, AZ 85719, USAR. MiquelInstitució Catalana de Recerca i Estudis Avançats, Passeig de Lluís Companys, 23, E-08010 Barcelona, SpainJohn MoustakasDepartment of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USAAdam D. MyersDepartment of Physics & Astronomy, University of Wyoming, 1000 E. University, Dept. 3905, Laramie, WY 82071, USAJundan NieNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing, 100101, People's Republic of ChinaN. Palanque‐DelabrouilleIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceWill J. PercivalDepartment of Physics and Astronomy, University of Waterloo, 200 University Ave W, Waterloo, ON N2L 3G1, CanadaClaire PoppettLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]Francisco PradaInstituto de Astrofisica de Andalucía, Glorieta de la Astronomía, s/n, E-18008 Granada, SpainAnand RaichoorLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]A.J. RossCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAEdward F. SchlaflySpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USADavid J. SchlegelLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]M. SchubnellDepartment of Physics, University of Michigan, Ann Arbor, MI 48109, USAG. TarléUniversity of Michigan, Ann Arbor, MI 48109, USAB. A. WeaverNSF’s National Optical-Infrared Astronomy Research Laboratory, 950 N. Cherry Avenue, Tucson, AZ 85719, USAR.H. WechslerKavli Institute for Particle Astrophysics and Cosmology, Stanford University, Menlo Park, CA 94305, USAChristophe YècheIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceZhimin ZhouNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing, 100101, People's Republic of China
2023en
ABI
Аннотация
Abstract The Dark Energy Spectroscopic Instrument (DESI) is carrying out a five-year survey that aims to measure the redshifts of tens of millions of galaxies and quasars, including 8 million luminous red galaxies (LRGs) in the redshift range 0.4 < z ≲ 1.0. Here we present the selection of the DESI LRG sample and assess its spectroscopic performance using data from Survey Validation (SV) and the first two months of the Main Survey. The DESI LRG sample, selected using g , r , z , and W 1 photometry from the DESI Legacy Imaging Surveys, is highly robust against imaging systematics. The sample has a target density of 605 deg −2 and a comoving number density of 5 × 10 −4 h 3 Mpc −3 in 0.4 < z < 0.8; this is a significantly higher density than previous LRG surveys (such as SDSS, BOSS, and eBOSS) while also extending to z ∼ 1. After applying a bright star veto mask developed for the sample, 98.9% of the observed LRG targets yield confident redshifts (with a catastrophic failure rate of 0.2% in the confident redshifts), and only 0.5% of the LRG targets are stellar contamination. The LRG redshift efficiency varies with source brightness and effective exposure time, and we present a simple model that accurately characterizes this dependence. In the appendices, we describe the extended LRG samples observed during SV.
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