Статья

The DESI One-Percent Survey: exploring a generalized SHAM for multiple tracers with the UNIT simulation

Jiaxi YuLaboratory of Astrophysics, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny , CH-1290 Versoix , SwitzerlandCheng ZhaoDepartment of Astronomy, Tsinghua University , Beijing 100084 , ChinaVioleta González-PérezCentro de Investigación Avanzada en Física Fundamental (CIAFF), Facultad de Ciencias, Universidad Autónoma de Madrid , E-28049 Madrid , SpainChia-Hsun ChuangDepartment of Physics and Astronomy, University of Utah, Salt Lake City , UT 84112 , USAA. BrodzellerDepartment of Physics and Astronomy, University of Utah, Salt Lake City , UT 84112 , USAArnaud de MattiaIRFU, CEA, Université Paris-Saclay , F-91191 Gif-sur-Yvette , FranceJean‐Paul KneibLAM (Laboratoire d’Astrophysique de Marseille), Aix Marseille Université, CNRS , UMR 7326, F13388, Marseille , FranceAlex KrolewskiDepartment of Physics and Astronomy, University of Waterloo , 200 University Avenue W, Waterloo, ON N2L 3G1 , CanadaA. RocherIRFU, 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 , USAYunchong WangPhysics Department, Stanford University , 382 Via Pueblo Mall, Stanford, CA 94305 , USASihan YuanPhysics Department, Kavli Institute for Particle Astrophysics and Cosmology, Stanford University , Stanford, CA 94305 , USAH. ZhangDepartment of Physics, Kansas State University , 116 Cardwell Hall, Manhattan, KS 66506 , USARongpu ZhouLawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720 , USAJ. AguilarLawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720 , USAS. AhlenPhysics Department, Boston University , 590 Commonwealth Avenue, Boston, MA 02215 , USADavid BrooksDepartment of Physics & Astronomy, University College London , Gower Street, London, WC1E 6BT , UKKyle DawsonDepartment of Physics and Astronomy, University of Utah, Salt Lake City , UT 84112 , USAAlex de la MacorraDepartamento de Física, Universidad de Guanajuato–DCI , C.P. 37150, Leon, Guanajuato , MéxicoP. DoelDepartment of Physics & Astronomy, University College London , Gower Street, London, WC1E 6BT , UKK. FanningCenter for Cosmology and AstroParticle Physics, The Ohio State University , 191 West Woodruff Avenue, 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 , ColombiaSatya Gontcho A GontchoLawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720 , USAK. HonscheidCenter for Cosmology and AstroParticle Physics, The Ohio State University , 191 West Woodruff Avenue, Columbus, OH 43210 , 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 , USAMarc ManeraInstitut de Física d’Altes Energies(IFAE), The Barcelona Institute of Science and Technology , Campus UAB, E-08193 Bellaterra Barcelona , SpainPaul MartiniCenter for Cosmology and AstroParticle Physics, The Ohio State University , 191 West Woodruff Avenue, Columbus, OH 43210 , USAAaron MeisnerNSF’s National Optical-Infrared Astronomy Research Laboratory , 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 , USAJundan NieNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing, 100101 , People’s Republic of ChinaWill 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 , USAAnand RaichoorLawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720 , USAGraziano RossiDepartment of Physics and Astronomy, Sejong University , Seoul 143-747 , KoreaHee‐Jong SeoDepartment of Physics and Astronomy, Ohio University, Athens , OH 45701 , USAG. TarléDepartment of Physics, University of Michigan , Ann Arbor, MI 48109 , USAZhimin ZhouNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing, 100101 , People’s Republic of ChinaH. ZouNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing, 100101 , People’s Republic of China

2023en

ABI

Аннотация

ABSTRACT We perform SubHalo Abundance Matching (SHAM) studies on UNIT simulations with {σ, Vceil, vsmear}-SHAM and {σ, Vceil, fsat}-SHAM. They are designed to reproduce the clustering on 5–30 $\, {\, h^{-1}\, {\rm Mpc}}$ of luminous red galaxies (LRGs), emission-line galaxies (ELGs), and quasi-stellar objects (QSOs) at 0.4 &lt; z &lt; 3.5 from DESI (Dark Energy Spectroscopic Instrument) One Percent Survey. Vceil is the incompleteness of the massive host (sub)haloes and is the key to the generalized SHAM. vsmear models the clustering effect of redshift uncertainties, providing measurements consistent with those from repeat observations. A free satellite fraction fsat is necessary to reproduce the clustering of ELGs. We find ELGs present a more complex galaxy–halo mass relation than LRGs reflected in their weak constraints on σ. LRGs, QSOs, and ELGs show increasing Vceil values, corresponding to the massive galaxy incompleteness of LRGs, the quenched star formation of ELGs and the quenched black hole accretion of QSOs. For LRGs, a Gaussian vsmear presents a better profile for subsamples at redshift bins than a Lorentzian profile used for other tracers. The impact of the statistical redshift uncertainty on ELG clustering is negligible. The best-fitting satellite fraction for DESI ELGs is around 4 per cent, lower than previous estimations for ELGs. The mean halo mass log10(〈Mvir〉) in ${{\, h^{-1}\, \mbox{M}_\odot }}{}$ for LRGs, ELGs, and QSOs are 13.16 ± 0.01, 11.90 ± 0.06, and 12.66 ± 0.45, respectively. Our generalized SHAM algorithms facilitate the production of multitracer galaxy mocks for cosmological tests.

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Идентификаторы

DOI: 10.1093/mnras/stad3559

Цитирования и источники

Цитирований: 2Использованных источников: 0

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