Maqola

The DESI one-per cent survey: exploring the halo occupation distribution of luminous red galaxies and quasi-stellar objects with <scp>AbacusSummit</scp>

Sihan YuanKavli Institute for Particle Astrophysics and Cosmology, Stanford University , 452 Lomita Mall, Stanford, CA 94305 , USAH. ZhangDepartment of Physics, Kansas State University , 116 Cardwell Hall, Manhattan, KS 66506 , USAA.J. RossDepartment of Astronomy, The Ohio State University , 140 W. 18th Avenue, Columbus, OH 43210 , USAJamie Donald-McCannInstitute of Cosmology & Gravitation, University of Portsmouth , Dennis Sciama Building, Portsmouth PO1 3FX , UKBoryana HadzhiyskaMiller Institute for Basic Research in Science, University of California , Berkeley, CA 94720 , USAR.H. WechslerKavli Institute for Particle Astrophysics and Cosmology, Stanford University , 452 Lomita Mall, Stanford, CA 94305 , USAZheng ZhengDepartment of Physics and Astronomy, University of Utah , 115 South 1400 East, Salt Lake City, UT 84112 , USAShadab AlamInstitue for Astronomy, Royal Observatory, University of Edinburgh , EH9 3HJ , UKVioleta González-PérezCentro de Investigacion Avanzada en Física Fundamental (CIAFF), Facultad de Ciencias, Universidad Autonoma de Madrid , E-28049 Madrid , SpainJ. AguilarLawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720 , USAS. AhlenPhysics Department, Boston University , 590 Commonwealth Avenue, Boston, MA 02215 , USADavide 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 , UKAxel de la MacorraInstituto de Física, Universidad Nacional Autónoma de México , Cd. de México, C.P. 04510 , MéxicoK. FanningDepartment of Astronomy, The Ohio State University , 140 W. 18th Avenue, Columbus, OH 43210 , USAJ. E. Forero-RomeroDepartamento de Física, Universidad de los Andes , Cra. 1 No. 18A-10, Edificio Ip, CP 111711, Bogotá , ColombiaK. HonscheidCenter for Cosmology and AstroParticle 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 , USAR. KehoeDepartment of Physics, Southern Methodist University , 3215 Daniel Avenue, Dallas, TX 75275 , USAJ. LaskerDepartment of Physics, Southern Methodist University , 3215 Daniel Avenue, Dallas, TX 75275 , USAMartin LandriauLawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720 , USAMarc ManeraInstitut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology , Campus UAB, E-08193 Bellaterra , SpainPaul MartiniDepartment of Astronomy, The Ohio State University , 140 W. 18th 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 , USAS. NadathurInstitute of Cosmology & Gravitation, University of Portsmouth , Dennis Sciama Building, Portsmouth PO1 3FX , UKJeffrey 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 Road, Chaoyang District, Beijing 100012 , P.R. ChinaWill J. PercivalPerimeter Institute for Theoretical Physics , 31 Caroline St. North, Waterloo, ON N2L 2Y5 , CanadaClaire PoppettLawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720 , USAA. RocherCEA, Institut de recherche sur les lois Fondamentales de l’Univers, Université Paris-Saclay , F-91191 Gif-sur-Yvette , FranceGraziano RossiDepartment of Physics and Astronomy, Sejong University , Seoul 143-747 , KoreaE. SánchezCentro de Investigaciones Energé ticas, Medioambientales y Tecnoló gicas (CIEMAT) , Madrid, 28040 , SpainLado SamushiaDepartment of Physics, Kansas State University , 116 Cardwell Hall, Manhattan, KS 66506 , USAMichael SchubnellDepartment of Physics, University of Michigan , Ann Arbor, MI 48109 , USAHee‐Jong SeoDepartment of Physics and Astronomy, Ohio University , Athens, OH 45701 , USAG. TarléDepartment of Physics, University of Michigan , Ann Arbor, MI 48109 , USABenjamin A. WeaverNSF’s NOIRLab , 950 N. Cherry Avenue, Tucson, AZ 85719 , USAJiaxi YuLaboratory of Astrophysics, École Polytechnique Fédérale de Lausanne (EPFL) , Observatoire de Sauverny, CH-1290 Versoix , SwitzerlandZhimin ZhouNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100012 , P.R. ChinaH. ZouNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100012 , P.R. China

2024en

ABI

Annotatsiya

ABSTRACT We present the first comprehensive halo occupation distribution (HOD) analysis of the Dark Energy Spectroscopic Instrument (DESI) One-Percent Survey luminous red galaxy (LRG) and Quasi Stellar Object (QSO) samples. We constrain the HOD of each sample and test possible HOD extensions by fitting the redshift-space galaxy 2-point correlation functions in 0.15 &lt; r &lt; 32 h−1 Mpc in a set of fiducial redshift bins. We use AbacusSummit cubic boxes at Planck 2018 cosmology as model templates and forward model galaxy clustering with the AbacusHOD package. We achieve good fits with a standard HOD model with velocity bias, and we find no evidence for galaxy assembly bias or satellite profile modulation at the current level of statistical uncertainty. For LRGs in 0.4 &lt; z &lt; 0.6, we infer a satellite fraction of $f_\mathrm{sat} = 11\pm 1~{y{\ \mathrm{per\,cent}}}$, a mean halo mass of $\log _{10}\overline{M}_h/M_\odot =13.40^{+0.02}_{-0.02}$, and a linear bias of $b_\mathrm{lin} = 1.93_{-0.04}^{+0.06}$. For LRGs in 0.6 &lt; z &lt; 0.8, we find $f_\mathrm{sat}=14\pm 1~{{\ \mathrm{per\,cent}}}$, $\log _{10}\overline{M}_h/M_\odot =13.24^{+0.02}_{-0.02}$, and $b_\mathrm{lin}=2.08_{-0.03}^{+0.03}$. For QSOs, we infer $f_\mathrm{sat}=3^{+8}_{-2}\mathrm{per\,cent}$, $\log _{10}\overline{M}_h/M_\odot = 12.65^{+0.09}_{-0.04}$, and $b_\mathrm{lin} = 2.63_{-0.26}^{+0.37}$ in redshift range 0.8 &lt; z &lt; 2.1. Using these fits, we generate a large suite of high fidelity galaxy mocks, forming the basis of systematic tests for DESI Y1 cosmological analyses. We also study the redshift-evolution of the DESI LRG sample from z = 0.4 up to z = 1.1, revealling significant and interesting trends in mean halo mass, linear bias, and satellite fraction.

Hali tarjima qilinmagan

Identifikatorlar

DOI: 10.1093/mnras/stae359

Iqtiboslar va manbalar

7 ta iqtibos0 ta foydalanilgan manba

Koʻrsatkichlar — AkademScholar