A joint analysis of 3D clustering and galaxy × CMB-lensing cross-correlations with DESI DR1 galaxies
The spectroscopic data from DESI Data Release 1 (DR1) galaxies enables the analysis of 3D clustering by fitting galaxy power spectra and reconstructed correlation functions in redshift space. Given low measurements of the amplitude of structure from cosmic shear at z ~ 1, redshift space distortions...
| Autores: | , , , , , , , , , , |
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| Formato: | artículo |
| Fecha de publicación: | 2025 |
| País: | España |
| Recursos: | Universitat Politècnica de Catalunya (UPC) |
| Repositorio: | UPCommons. Portal del coneixement obert de la UPC |
| Idioma: | inglés |
| OAI Identifier: | oai:dnet:upcommonspor::c0b30c6b9125b08b85306dc7927e142a |
| Acesso em linha: | https://hdl.handle.net/2117/461456 https://dx.doi.org/10.1088/1475-7516/2025/11/077 |
| Access Level: | acceso abierto |
| Palavra-chave: | Cosmological parameters from LSS Gravitational lensing Power spectrum Redshift surveys Àrees temàtiques de la UPC::Física::Astronomia i astrofísica |
| Resumo: | The spectroscopic data from DESI Data Release 1 (DR1) galaxies enables the analysis of 3D clustering by fitting galaxy power spectra and reconstructed correlation functions in redshift space. Given low measurements of the amplitude of structure from cosmic shear at z ~ 1, redshift space distortions (RSD) + Baryon Acoustic Oscillation (BAO) signals from DESI galaxies combined with weak lensing can break degeneracies and provide a tight alternative constraint on the z ~ 1 amplitude of structure. In this paper we perform joint analyses that combine full-shape + post-reconstruction information from the DESI DR1 BGS and LRG samples along with angular cross-correlations with Planck PR4 and ACT DR6 CMB lensing maps. We show that adding galaxy-lensing cross-correlations tightens clustering amplitude constraints, improving s8 uncertainties by 30% over RSD+BAO alone. We also include angular galaxy-galaxy and galaxy-lensing spectra using photometric samples from the DESI Legacy Survey to further improve constraints. Our headline results are s8 = 0.803 ± 0.017, Om = 0.3037 ± 0.0069, and S8 = 0.808 ± 0.017. Given DESI's preference for higher s8 compared to lower values from BOSS, we perform a catalog-level comparison of LRG samples from both surveys. We test sensitivity to dark energy assumptions by relaxing our ¿CDM prior and allowing for evolving dark energy via the w0 - wa parameterization. We find our S8 constraints to be relatively unchanged despite a 3.5s tension with the cosmological constant model when combining with the Union3 supernova likelihood. Finally we test general relativity (GR) by allowing the gravitational slip parameter (¿) to vary, and find ¿ = 1.17 ± 0.11 in mild (~ 1.5s) tension with the GR value of 1.0. |
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