Survey Operations for the Dark Energy Spectroscopic Instrument
Edward F. SchlaflySpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USAD. KirkbyDepartment of Physics and Astronomy, University of California, Frederick Reines Hall, Irvine, CA 92697, USADavid J. SchlegelLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAAdam D. MyersDepartment of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USAAnand RaichoorLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAKyle DawsonDepartment of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USAJessica AguilarLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USACarlos Allende PrietoInstituto de Astrofísica de Canarias, C/Vía Láctea, s/n, E-38205 La Laguna, Tenerife, SpainS. BaileyLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAS. BenZviDepartment of Physics & Astronomy, University of Rochester, Bausch and Lomb Hall, Rochester, NY 14627-0171, USAJ. R. Bermejo-ClimentDepartment of Physics & Astronomy, University of Rochester, Bausch and Lomb Hall, Rochester, NY 14627-0171, USADavid 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 NOIRLab, 950 N. Cherry Avenue, Tucson, AZ 85719, USAPeter DoelDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UKK. FanningThe Ohio State University, 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, SpainJ. E. Forero-RomeroDepartamento de Física, Universidad de los Andes, Cra. 1 No. 18A-10, Edificio Ip, CP 111711, Bogotá, ColombiaJ. García-BellidoInstituto de Física Teórica (IFT) UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049, Madrid, SpainSatya Gontcho A GontchoLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAJ. GuyLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAChang Hoon HahnDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USAMustapha IshakUniversity of Texas, Dallas, 800 W Campbell Road, Richardson, TX 75080, USAS. JuneauNSF’s NOIRLab, 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, 1 Cyclotron Road, Berkeley, CA 94720, USAAnthony KreminLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAMartin LandriauLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USADustin LangDepartment of Physics and Astronomy, University of Waterloo, 200 University Avenue W, Waterloo, ON N2L 3G1, CanadaJ. LaskerDepartment of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75275, USAM. E. LeviLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAChristophe MagnevilleIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceChristopher J. ManserAstrophysics Group, Department of Physics, Imperial College London, Prince Consort Road, London, SW7 2AZ, UKJ. ErezaCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAAaron MeisnerNSF’s NOIRLab, 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, USAJeffrey A. NewmanDepartment of Physics & Astronomy and Pittsburgh Particle Physics, Astrophysics, and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USAJundan NieNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100012, 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 Avenue W, Waterloo, ON N2L 3G1, CanadaClaire PoppettLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAConstance M. RockosiDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95065, USAA.J. RossCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAGraziano RossiDepartment of Physics and Astronomy, Sejong University, Seoul, 143-747, Republic of KoreaG. TarléUniversity of Michigan, Ann Arbor, MI 48109, USABenjamin A. WeaverNSF’s NOIRLab, 950 N. Cherry Avenue, Tucson, AZ 85719, USAChristophe YècheIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceRongpu ZhouLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA
2023en
ABI
Abstract
Abstract The Dark Energy Spectroscopic Instrument (DESI) survey is a spectroscopic survey of tens of millions of galaxies at 0 < z < 3.5 covering 14,000 sq. deg. of the sky. In its first 1.1 yr of survey operations, it has observed more than 14 million galaxies and 4 million stars. We describe the processes that govern DESI’s observations of the 15,000 fields composing the survey. This includes the planning of each night’s observations in the afternoon; automatic selection of fields to observe during the night; real-time assessment of field completeness on the basis of observing conditions during each exposure; reduction, redshifting, and quality assurance of each field of targets in the morning following observation; and updates to the list of future targets to observe on the basis of these results. We also compare the performance of the survey with historical expectations and find good agreement. Simulations of the weather and of DESI observations using the real field-selection algorithm show good agreement with the actual observations. After accounting for major unplanned shutdowns, the dark time survey is progressing about 7% faster than forecast, which is good agreement given approximations made in the simulations.
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Cited by 170 references