Статья

Mitigating imaging systematics for DESI 2024 emission Line Galaxies and beyond

A. Rosado-MarinOhio U., AthensA.J. RossChicago U., KICPHee‐Jong SeoDepartment of Physics & Astronomy, Ohio University, 139 University Terrace, Athens, OH 45701, U.S.AMehdi RezaieDepartment of Physics, Kansas State University, 116 Cardwell Hall, Manhattan, KS 66506, U.S.AH. KongInstitut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Edifici Cn, Campus UAB, 08193, Bellaterra (Barcelona), SpainArnaud de MattiaIRFU, SaclayRongpu ZhouLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AJ. AguilarBoston US. AhlenMilan UO. AlvesUniversity Coll. LondonDavide BianchiDipartimento di Fisica "Aldo Pontremoli", Università degli Studi di Milano, Via Celoria 16, I-20133 Milano, ItalyD. BrooksDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, U.KE. BurtinIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceE. ChaussidonKIPAC, Menlo ParkXinyi ChenUC, Berkeley, Math. DeptT. ClaybaughLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AKyle DawsonFermilabAxel de la MacorraPrinceton UArjun DeyNSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AP. 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.AS. FerraroLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AJ. E. Forero-RomeroICREA, BarcelonaE. GaztañagaInstitut d'Estudis Espacials de Catalunya (IEEC), c/ Esteve Terradas 1, Edifici RDIT, Campus PMT-UPC, 08860 Castelldefels, SpainSatya Gontcho A GontchoLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AG. GutierrezFermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, U.S.AChang Hoon HahnSteward Observatory, University of Arizona, 933 N, Cherry Ave, Tucson, AZ 85721, U.S.AM. HanifUniversity of Michigan, 500 S. State Street, Ann Arbor, MI 48109, U.S.ACullan HowlettBarcelona, Polytechnic US. JuneauNSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AMustapha IshakMadrid, CIEMATTheodore KisnerLBL, BerkeleyAnthony KreminHiroshima Shudo UA. KrolewskiDepartment of Physics and Astronomy, University of Waterloo, 200 University Ave W, Waterloo, ON N2L 3G1, CanadaMartin 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. LeviBeijing ObservAaron MeisnerNSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AJ. Mena-FernándezPerimeter Inst. Theor. PhysJohn MoustakasLBL, BerkeleyJeffrey 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, U.S.AE. PaillasWaterloo Centre for Astrophysics, University of Waterloo, 200 University Ave W, Waterloo, ON N2L 3G1, CanadaN. Palanque‐DelabrouilleIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceWill J. PercivalPerimeter Institute for Theoretical Physics, 31 Caroline St. North, Waterloo, ON N2L 2Y5, CanadaFrancisco PradaInstituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, s/n, E-18008 Granada, SpainIgnasi Pérez-RàfolsDepartament de Física, EEBE, Universitat Politècnica de Catalunya, c/Eduard Maristany 10, 08930 Barcelona, SpainAnand RaichoorLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AGraziano RossiDepartment of Physics and Astronomy, Sejong University, 209 Neungdong-ro, Gwangjin-gu, Seoul 05006, Republic of KoreaRossana RuggeriCentre for Astrophysics & Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC 3122, AustraliaE. SánchezCIEMAT, Avenida Complutense 40, E-28040 Madrid, SpainEdward F. SchlaflySpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.ADavid J. SchlegelLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AM. SchubnellUniversity of Michigan, 500 S. State Street, Ann Arbor, MI 48109, U.S.AD. SprayberryNSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AM. Vargas-MagañaInstituto de Física, Universidad Nacional Autónoma de México, Circuito de la Investigación Científica, Ciudad Universitaria, Cd. de México C. P. 04510, MéxicoB. A. WeaverNSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AJiaxi YuInstitute of Physics, Laboratory of Astrophysics, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, Chemin Pegasi 51, CH-1290 Versoix, SwitzerlandH. ZouNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100012, P.R. China

Journal of Cosmology and Astroparticle Physicsjournal2025en

ABI

Аннотация

Abstract Emission Line Galaxies (ELGs) are one of the main tracers that the Dark Energy Spectroscopic Instrument (DESI) uses to probe the universe. However, they are afflicted by strong spurious correlations between target density and observing conditions known as imaging systematics. In this paper, we present the imaging systematics mitigation applied to the DESI Data Release 1 (DR1) large-scale structure catalogs used in the DESI 2024 cosmological analyses. We also explore extensions of the fiducial treatment. This includes a combined approach, through forward image simulations ( Obiwan ) in conjunction with neural network-based regression, to obtain an angular selection function that mitigates the imaging systematics observed in the DESI DR1 ELGs target density. We further derive a line of sight selection function from the forward model that removes the strong redshift dependence between imaging systematics and low redshift ELGs. Combining both angular and redshift-dependent systematics, we construct a three-dimensional selection function and assess the impact of all selection functions on clustering statistics. We quantify differences between these extended treatments and the fiducial treatment in terms of the measured 2-point statistics. We find that the results are generally consistent with the fiducial treatment and conclude that the differences are far less than the imaging systematics uncertainty included in DESI 2024 full-shape measurements. We extend our investigation to the ELGs at 0.6 < z < 0.8, i.e., beyond the redshift range (0.8 < z < 1.6) adopted for the DESI clustering catalog, and demonstrate that determining the full three-dimensional selection function is necessary in this redshift range. Our tests showed that all changes are consistent with statistical noise for BAO analyses indicating they are robust to even severe imaging systematics. Specific tests for the full-shape analysis will be presented in a companion paper.

Темы

Galaxies: Formation, Evolution, Phenomena Astronomy and Astrophysical Research Gamma-ray bursts and supernovae

Идентификаторы

DOI: 10.1088/1475-7516/2025/07/018

Цитирования и источники

Цитирований: 4 Использованных источников: 77

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