Maqola

The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation

Chang Hoon HahnDepartment of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA; [email protected]Michael J. WilsonInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, UKOmar Ruiz-MaciasInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, UKShaun ColeInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, UKDavid H. WeinbergDepartment of Astronomy and the Center for Cosmology and Astroparticle Physics, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USAJohn MoustakasDepartment of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USAAnthony KreminLawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USAJeremy L. TinkerCenter for Cosmology and Particle Physics, Department of Physics, New York University, New York, NY 10003, USAA. G. SmithIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceR.H. WechslerDepartment of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USAS. AhlenPhysics Dept., Boston University, 590 Commonwealth Avenue, Boston, MA 02215, USAShadab AlamInstitute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UKS. BaileyLawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USADavid BrooksDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UKAndrew P. CooperInstitute of Astronomy and Department of Physics, National Tsing Hua University, 101 Kuang-Fu Rd. Sec. 2, Hsinchu 30013, TaiwanT. M. DavisSchool of Mathematics and Physics, University of Queensland, 4101, AustraliaKyle DawsonDepartment of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USAArjun DeyNSF’s NOIRLab, 950 N. Cherry Avenue, Tucson, AZ 85719, USABiprateep DeyDepartment of Physics & Astronomy and Pittsburgh Particle Physics, Astrophysics, and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USASarah EftekharzadehUniversities Space Research Association, NASA Ames Research Centre, USADaniel J. EisensteinCenter for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USAKevin FanningCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAJ. E. Forero-RomeroDepartamento de Física, Universidad de los Andes, Cra. 1 No. 18A-10, Bogotá, ColombiaCarlos S. FrenkInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, UKE. GaztañagaInstitut de Cìencies de l’Espai, IEEC-CSIC, Campus UAB, Carrer de Can Magrans s/n, E-08913 Bellaterra, Barcelona, SpainSatya Gontcho A GontchoDepartment of Physics and Astronomy, University of Rochester, 500 Joseph C. Wilson Boulevard, Rochester, NY 14627, USAJ. GuyLawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USAK. HonscheidDepartment of 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, USAS. JuneauNSF’s National Optical-Infrared Astronomy Research Laboratory, 950 N. Cherry Avenue, Tucson, AZ 85719, USAR. KehoeDepartment of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75275, USATheodore KisnerLawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USATing-Wen LanDepartment of Physics, National Taiwan University, Taipei 10617, TaiwanMartin LandriauLawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USAL. Le GuillouSorbonne Université, Université Paris Diderot, CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies, LPNHE, 4 place Jussieu, F-75252 Paris, FranceM. E. LeviLawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USAChristophe MagnevilleCEA Saclay, IRFU F-91191 Gif-sur-Yvette, FranceJ. 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, 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 Rd., Chaoyang District, Beijing, 100101, People’s Republic of ChinaP. NorbergCenter for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham DH1 3LE, UKN. Palanque‐DelabrouilleCEA Saclay, IRFU F-91191 Gif-sur-Yvette, FranceWill J. PercivalDepartment of Physics and Astronomy, University of Waterloo, 200 University Avenue W, Waterloo, ON N2L 3G1, CanadaClaire PoppettLawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USAFrancisco PradaInstituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, s/n, E-18008 Granada, SpainAnand RaichoorLawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USAA.J. RossCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USASasha GainesPhysics Department, Yale University, P.O. Box 208120, New Haven, CT 06511, USAChristoph SaulderKorea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of KoreaEdward F. SchlaflyLawrence Livermore National Laboratory, P.O. Box 808 L-211, Livermore, CA 94551, USADavid J. SchlegelLawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USAD. Sierra-PortaDepartamento de Física, Universidad de los Andes, Cra. 1 No. 18A-10, Bogotá, ColombiaG. TarléDepartment of Physics, University of Michigan, Ann Arbor, MI 48109, USABenjamin A. WeaverNSF’s National Optical-Infrared Astronomy Research Laboratory, 950 N. Cherry Avenue, Tucson, AZ 85719, USAChristophe YècheCEA Saclay, IRFU F-91191 Gif-sur-Yvette, FrancePauline ZarroukSorbonne Université, Université Paris Diderot, CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies, LPNHE, 4 place Jussieu, F-75252 Paris, FranceRongpu ZhouLawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USAZhimin ZhouNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100101, People’s Republic of ChinaH. ZouNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100101, People’s Republic of China

2023en

ABI

Annotatsiya

Abstract Over the next 5 yr, the Dark Energy Spectroscopic Instrument (DESI) will use 10 spectrographs with 5000 fibers on the 4 m Mayall Telescope at Kitt Peak National Observatory to conduct the first Stage IV dark energy galaxy survey. At z < 0.6, the DESI Bright Galaxy Survey (BGS) will produce the most detailed map of the universe during the dark-energy-dominated epoch with redshifts of >10 million galaxies spanning 14,000 deg 2 . In this work, we present and validate the final BGS target selection and survey design. From the Legacy Surveys, BGS will target an r < 19.5 mag limited sample (BGS Bright), a fainter 19.5 < r < 20.175 color-selected sample (BGS Faint), and a smaller low- z quasar sample. BGS will observe these targets using exposure times scaled to achieve homogeneous completeness and cover the footprint three times. We use observations from the Survey Validation programs conducted prior to the main survey along with simulations to show that BGS can complete its strategy and make optimal use of “bright” time. BGS targets have stellar contamination <1%, and their densities do not depend strongly on imaging properties. BGS Bright will achieve >80% fiber assignment efficiency. Finally, BGS Bright and BGS Faint will achieve >95% redshift success over any observing condition. BGS meets the requirements for an extensive range of scientific applications. BGS will yield the most precise baryon acoustic oscillation and redshift-space distortion measurements at z < 0.4. It presents opportunities for new methods that require highly complete and dense samples (e.g., N -point statistics, multitracers). BGS further provides a powerful tool to study galaxy populations and the relations between galaxies and dark matter.

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DOI: 10.3847/1538-3881/accff8

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