Article

Production of alternate realizations of DESI fiber assignment for unbiased clustering measurement in data and simulations

J. LaskerDepartment of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75275, U.S.AA. Carnero RosellDepartamento de Astrofísica, Universidad de La Laguna (ULL), E-38206, La Laguna, Tenerife, SpainAdam D. MyersDepartment of Physics & Astronomy, University of Wyoming, 1000 E. University, Dept. 3905, Laramie, WY 82071, U.S.AA.J. RossCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, U.S.ADavide BianchiDipartimento di Fisica “Aldo Pontremoli”, Università degli Studi di Milano, Via Celoria 16, I-20133 Milano, ItalyM. HanifUniversity of Michigan, Ann Arbor, MI 48109, U.S.AR. KehoeDepartment of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75275, U.S.AArnaud de MattiaIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceL. NapolitanoDepartment of Physics & Astronomy, University of Wyoming, 1000 E. University, Dept. 3905, Laramie, WY 82071, U.S.AWill J. PercivalDepartment of Physics and Astronomy, University of Waterloo, 200 University Ave W, Waterloo, ON N2L 3G1, CanadaR. StatenDepartment of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75275, U.S.AJ. AguilarLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AS. AhlenPhysics Department, Boston University, 590 Commonwealth Avenue, Boston, MA 02215, U.S.AL. BigwoodInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, U.KD. BrooksDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, U.KT. ClaybaughLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AShaun ColeInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, U.KAxel de la MacorraInstituto de Física, Universidad Nacional Autónoma de México, Cd. de México C.P. 04510, MéxicoZ. DingDepartment of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai 200240, ChinaP. DoelDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, U.KK. FanningKavli Institute for Particle Astrophysics and Cosmology, Stanford University, Menlo Park, CA 94305, U.S.AJ. E. Forero-RomeroDepartamento de Física, Universidad de los Andes, Cra. 1 No. 18A-10, Edificio Ip, CP 111711, Bogotá, ColombiaE. GaztañagaInstitut d'Estudis Espacials de Catalunya (IEEC), 08034 Barcelona, SpainSatya Gontcho A GontchoLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AG. GutiérrezFermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, U.S.ACullan HowlettSchool of Mathematics and Physics, University of Queensland, 4072, AustraliaS. JuneauNSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AAnthony KreminLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AMartin LandriauLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AL. Le GuillouSorbonne Université, CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), FR-75005 Paris, FranceM. E. LeviLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AMarc ManeraDepartament de Física, Serra Húnter, Universitat Autònoma de Barcelona, 08193 Bellaterra (Barcelona), SpainAaron MeisnerNSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AR. MiquelInstitució Catalana de Recerca i Estudis Avançats, Passeig de Lluís Companys, 23, 08010 Barcelona, SpainJohn MoustakasDepartment of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, U.S.AEva-Maria MuellerDepartment of Physics and Astronomy, University of Sussex, Brighton BN1 9QH, U.KJundan NieNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100012, P.R. ChinaGustavo NizDepartamento de Física, Universidad de Guanajuato – DCI, C.P. 37150, Leon, Guanajuato, MéxicoMin-Seok OhKorea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of KoreaN. Palanque‐DelabrouilleIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceClaire PoppettLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AFrancisco PradaInstituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, s/n, E-18008 Granada, SpainMehdi RezaieDepartment of Physics, Kansas State University, 116 Cardwell Hall, Manhattan, KS 66506, U.S.AGraziano RossiDepartment of Physics and Astronomy, Sejong University, Seoul, 143-747, KoreaE. SánchezCIEMAT, Avenida Complutense 40, E-28040 Madrid, SpainDavid J. SchlegelLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AM. SchubnellDepartment of Physics, University of Michigan, Ann Arbor, MI 48109, U.S.AHee‐Jong SeoDepartment of Physics & Astronomy, Ohio University, Athens, OH 45701, U.S.ADavid SprayberryNSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AG. TarléUniversity of Michigan, Ann Arbor, MI 48109, U.S.AM. Vargas-MagañaInstituto de Física, Universidad Nacional Autónoma de México, Cd. de México C.P. 04510, MéxicoB. A. WeaverNSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AMichael WilsonInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, U.KYun-Liang ZhengDepartment of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai 200240, China

2025en

ABI

Abstract

Abstract A critical requirement of spectroscopic large scale structure analyses is correcting for selection of which galaxies to observe from an isotropic target list. This selection is often limited by the hardware used to perform the survey which will impose angular constraints of simultaneously observable targets, requiring multiple passes to observe all of them. In SDSS this manifested solely as the collision of physical fibers and plugs placed in plates. In DESI, there is the additional constraint of the robotic positioner which controls each fiber being limited to a finite patrol radius. A number of approximate methods have previously been proposed to correct the galaxy clustering statistics for these effects, but these generally fail on small scales. To accurately correct the clustering we need to upweight pairs of galaxies based on the inverse probability that those pairs would be observed (Bianchi & Percival 2017). This paper details an implementation of that method to correct the Dark Energy Spectroscopic Instrument (DESI) survey for incompleteness. To calculate the required probabilities, we need a set of alternate realizations of DESI where we vary the relative priority of otherwise identical targets. These realizations take the form of alternate Merged Target Ledgers (AMTL), the files that link DESI observations and targets. We present the method used to generate these alternate realizations and how they are tracked forward in time using the real observational record and hardware status, propagating the survey as though the alternate orderings had been adopted. We detail the first applications of this method to the DESI One-Percent Survey (SV3) and the DESI year 1 data. We include evaluations of the pipeline outputs, estimation of survey completeness from this and other methods, and validation of the method using mock galaxy catalogs.

Identifiers

DOI: 10.1088/1475-7516/2025/01/127

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