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The DESI One-Percent survey: exploring the Halo Occupation Distribution of Emission Line Galaxies with AbacusSummit simulations

A. RocherIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceV. Ruhlmann-KleiderIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceE. BurtinIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceSihan YuanSLAC National Accelerator Laboratory, Menlo Park, CA 94305, U.S.AArnaud de MattiaIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceA.J. RossCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, U.S.AJ. AguilarLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AS. AhlenPhysics Dept., Boston University, 590 Commonwealth Avenue, Boston, MA 02215, U.S.AShadab AlamTata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, IndiaDavide BianchiDipartimento di Fisica “Aldo Pontremoli”, Università degli Studi di Milano, Via Celoria 16, I-20133 Milano, ItalyDavid BrooksDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, U.KShaun ColeInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, U.KKyle DawsonDepartment of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, U.S.AAxel de la MacorraInstituto de Física, Universidad Nacional Autónoma de México, Cd. de México C.P. 04510, MexicoP. DoelDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, U.KDaniel J. EisensteinCenter for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, U.S.AK. FanningThe Ohio State University, Columbus, 43210 OH, U.S.AJ. E. Forero-RomeroDepartamento de Física, Universidad de los Andes, Cra. 1 No. 18A-10, Edificio Ip, CP 111711, Bogotá, ColombiaLehman H. GarrisonCenter for Computational Astrophysics, Flatiron Institute, 162 5 th Avenue, New York, NY 10010, U.S.ASatya Gontcho A GontchoLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AVioleta González-PérezCentro de Investigación Avanzada en Física Fundamental (CIAFF), Facultad de Ciencias, Universidad Autónoma de Madrid, ES-28049 Madrid, SpainJulien GuyLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.ABoryana HadzhiyskaLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AChang Hoon HahnDepartment of Astrophysical Sciences, Princeton University, Princeton NJ 08544, U.S.AK. HonscheidCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, U.S.ATheodore KisnerLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AMartin LandriauLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AJ. LaskerDepartment of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75275, U.S.AM. E. LeviLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AMarc ManeraInstitut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra Barcelona, SpainAaron MeisnerNSF's 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.KJeffrey 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.AJundan NieNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100012, P.R. ChinaWill 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, U.S.AFei QinKorea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of KoreaGraziano RossiDepartment of Physics and Astronomy, Sejong University, Seoul, 143-747, KoreaLado SamushiaAbastumani Astrophysical Observatory, Tbilisi, GE-0179, GeorgiaE. 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.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, MexicoBenjamin Alan WeaverNSF's NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AJiaxi YuEcole Polytechnique Fédérale de Lausanne, CH-1015 Lausanne, SwitzerlandH. ZhangDepartment of Physics, Kansas State University, 116 Cardwell Hall, Manhattan, KS 66506, U.S.AZheng ZhengDepartment of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, U.S.AZhimin ZhouNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100012, P.R. ChinaH. ZouNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100012, P.R. China

2023en

ABI

Annotatsiya

Abstract The One-Percent survey of the Dark Energy Spectroscopic Instrument collected ∼ 270 k emission line galaxies (ELGs) at 0.8 < z < 1.6. The high completeness of the sample allowed the clustering to be measured down to scales never probed before, 0.04 Mpc/ h in r p for the projected 2-point correlation function (2PCF) and 0.17 Mpc/ h in galaxy pair separation s for the 2PCF monopole and quadrupole. The most striking feature of the measurements is a strong signal at the smallest scales, below 0.2 Mpc/ h in r p and 1 Mpc/ h in s . We analyse these data in the halo occupation distribution framework. We consider different distributions for central galaxies, a standard power law for satellites with no condition on the presence of a central galaxy and explore several extensions of these models. For all considered models, the mean halo mass of the sample is found to be log 10 ⟨ M h ⟩ ∼ 11.9. We obtain a satellite mean occupation function which agrees with physically motivated ELG models only if we introduce central-satellite conformity, meaning that the satellite occupation is conditioned by the presence of central galaxies of the same type. To achieve in addition a good modelling of the clustering between 0.1 and 1 Mpc/ h in r p , we allow for ELG positioning outside of the halo virial radius and find 0.5% of ELGs residing in the outskirts of halos. Furthermore, the satellite velocity dispersion inside halos is found to be ∼ 30% larger than that of the halo dark matter particles. These are the main findings of our work. We investigate assembly bias as a function of halo concentration, local density or local density anisotropies and observe no significant change in our results. We split the data sample in two redshift bins and report no significant evolution with redshift. Lastly, changing the cosmology in the modelling impacts only slightly our results.

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DOI: 10.1088/1475-7516/2023/10/016

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