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Comparing Compressed and Full-Modeling analyses with FOLPS: implications for DESI 2024 and beyond

H. E. NoriegaInstitut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB), c. Martí i Franquès, 1, 08028 Barcelona, SpainAlejandro AvilésInstituto de Ciencias Físicas, Universidad Autónoma de México, Cuernavaca, Morelos, 62210, MéxicoHéctor Gil-MarínDepartament de Física Quàntica i Astrofísica, Universitat de Barcelona, Martí i Franquès 1, E08028 Barcelona, SpainS. Ramirez-SolanoInstituto de Física, Universidad Nacional Autónoma de México, Cd. de México C.P. 04510, MéxicoS. FromenteauInstituto de Ciencias Físicas, Universidad Autónoma de México, Cuernavaca, Morelos, 62210, MéxicoM. Vargas-MagañaInstituto de Física, Universidad Nacional Autónoma de México, Cd. de México C.P. 04510, MéxicoJosé AguilarLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AS. AhlenPhysics Departament, Boston University, 590 Commonwealth Avenue, Boston, MA 02215, U.S.AO. AlvesUniversity of Michigan, Ann Arbor, MI 48109, U.S.AS. BriedenInstitute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, U.KDavid BrooksDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, U.KJorge L. Cervantes–CotaDepartamento de Física, Instituto Nacional de Investigaciones Nucleares, Carreterra México-Toluca S/N, La Marquesa, Ocoyoacac, Edo. de México C.P. 52750, MéxicoShi-Fan ChenInstitute for Advanced Study, 1 Einstein Drive, Princeton, NJ 08540, U.S.AT. 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.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, MéxicoArnaud de MattiaIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FrancePeter DoelDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, U.KN. FindlayInstitute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, U.KJ. 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.AK. HonscheidCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, U.S.AJiamin HouDepartment of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, U.S.ACullan HowlettSchool of Mathematics and Physics, University of Queensland, 4072, AustraliaMustapha IshakDepartment of Physics, The University of Texas at Dallas, Richardson, TX 75080, U.S.AS. JuneauNSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AYan LaiSchool of Mathematics and Physics, University of Queensland, 4072, AustraliaMartin LandriauLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AMarc ManeraDepartament de Física, Serra Húnter, Universitat Autònoma de Barcelona, 08193 Bellaterra (Barcelona), SpainM. MausUniversity of California, Berkeley, 110 Sproul Hall #5800 Berkeley, CA 94720, U.S.AR. MiquelInstitució Catalana de Recerca i Estudis Avançats, Passeig de Lluís Companys, 23, 08010 Barcelona, SpainGerardo Morales-NavarreteDepartamento de Física, Instituto Nacional de Investigaciones Nucleares, Carreterra México-Toluca S/N, La Marquesa, Ocoyoacac, Edo. de México C.P. 52750, MéxicoEva-Maria MuellerDepartment of Physics and Astronomy, University of Sussex, Brighton BN1 9QH, U.KA. Muñoz-GutiérrezInstituto de Física, Universidad Nacional Autónoma de México, Cd. de México C.P. 04510, MéxicoAdam D. MyersDepartment of Physics & Astronomy, University of Wyoming, 1000 E. University, Dept. 3905, Laramie, WY 82071, U.S.AS. NadathurInstitute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, U.KGustavo NizDepartamento de Física, Universidad de Guanajuato – DCI, C.P. 37150, Leon, Guanajuato, MéxicoN. Palanque‐DelabrouilleIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceWill J. PercivalDepartment of Physics and Astronomy, University of Waterloo, 200 University Ave W, Waterloo, ON N2L 3G1, CanadaC. PoppettLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, U.S.AMehdi RezaieDepartment of Physics, Kansas State University, 116 Cardwell Hall, Manhattan, KS 66506, U.S.AA. RocherCEA Paris-SaclayGraziano 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.ADavid SprayberryNSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AG. TarléUniversity of Michigan, Ann Arbor, MI 48109, U.S.ALicia VerdeInstitució Catalana de Recerca i Estudis Avançats, Passeig de Lluís Companys, 23, 08010 Barcelona, SpainSihan YuanSLAC National Accelerator Laboratory, Menlo Park, CA 94305, U.S.APauline ZarroukSorbonne Université, CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), FR-75005 Paris, FranceH. ZouNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100012, P.R. China

2025en

ABI

Annotatsiya

Abstract The Dark Energy Spectroscopic Instrument (DESI) will provide unprecedented information about the large-scale structure of our Universe. In this work, we study the robustness of the theoretical modelling of the power spectrum of Folps , a novel effective field theory-based package for evaluating the redshift space power spectrum in the presence of massive neutrinos. We perform this validation by fitting the AbacusSummit high-accuracy N -body simulations for Luminous Red Galaxies, Emission Line Galaxies and Quasar tracers, calibrated to describe DESI observations. We quantify the potential systematic error budget of Folps finding that the modelling errors are fully sub-dominant for the DESI statistical precision within the studied range of scales. Additionally, we study two complementary approaches to fit and analyse the power spectrum data, one based on direct Full-Modelling fits and the other on the ShapeFit compression variables, both resulting in very good agreement in precision and accuracy. In each of these approaches, we study a set of potential systematic errors induced by several assumptions, such as the choice of template cosmology, the effect of prior choice in the nuisance parameters of the model, or the range of scales used in the analysis. Furthermore, we show how opening up the parameter space beyond the vanilla ΛCDM model affects the DESI observables. These studies include the addition of massive neutrinos, spatial curvature, and dark energy equation of state. We also examine how relaxing the usual Cosmic Microwave Background and Big Bang Nucleosynthesis priors on the primordial spectral index and the baryonic matter abundance, respectively, impacts the inference on the rest of the parameters of interest. This paper pathways towards performing a robust and reliable analysis of the shape of the power spectrum of DESI galaxy and quasar clustering using Folps .

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DOI: 10.1088/1475-7516/2025/01/136

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