Frequentist Cosmological Constraints from Full-Shape Clustering Measurements in DESI DR1
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2025
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| author | Morawetz, James Zhang, Hanyu Bonici, Marco Percival, Will Crespi, Andrea Aguilar, Jessica Nicole Ahlen, Steven Bianchi, Davide Brooks, David Castander, Francisco Javier Claybaugh, Todd Cole, Shaun Cuceu, Andrei de la Macorra, Axel de Mattia, Arnaud Dey, Biprateep Doel, Peter Ferraro, Simone Font-Ribera, Andreu Forero-Romero, Jaime E. Gaztañaga, Enrique Gontcho, Satya Gontcho A Gutierrez, Gaston Hahn, ChangHoon Honscheid, Klaus Huterer, Dragan Ishak, Mustapha Joyce, Dick Kehoe, Robert Kirkby, David Kisner, Theodore Lahav, Ofer Lambert, Andrew Landriau, Martin Guillou, Laurent Le Manera, Marc Miquel, Ramon Mueller, Eva-Maria Nadathur, Seshadri Newman, Jeffrey A. Niz, Gustavo Palanque-Delabrouille, Nathalie Prada, Francisco Pérez-Ràfols, Ignasi Rossi, Graziano Samushia, Lado Sanchez, Eusebio Schlegel, David Schubnell, Michael Silber, Joseph Harry Sprayberry, David Tarlé, Gregory Weaver, Benjamin Alan Zarrouk, Pauline Zhou, Rongpu Zou, Hu |
| author_facet | Morawetz, James Zhang, Hanyu Bonici, Marco Percival, Will Crespi, Andrea Aguilar, Jessica Nicole Ahlen, Steven Bianchi, Davide Brooks, David Castander, Francisco Javier Claybaugh, Todd Cole, Shaun Cuceu, Andrei de la Macorra, Axel de Mattia, Arnaud Dey, Biprateep Doel, Peter Ferraro, Simone Font-Ribera, Andreu Forero-Romero, Jaime E. Gaztañaga, Enrique Gontcho, Satya Gontcho A Gutierrez, Gaston Hahn, ChangHoon Honscheid, Klaus Huterer, Dragan Ishak, Mustapha Joyce, Dick Kehoe, Robert Kirkby, David Kisner, Theodore Lahav, Ofer Lambert, Andrew Landriau, Martin Guillou, Laurent Le Manera, Marc Miquel, Ramon Mueller, Eva-Maria Nadathur, Seshadri Newman, Jeffrey A. Niz, Gustavo Palanque-Delabrouille, Nathalie Prada, Francisco Pérez-Ràfols, Ignasi Rossi, Graziano Samushia, Lado Sanchez, Eusebio Schlegel, David Schubnell, Michael Silber, Joseph Harry Sprayberry, David Tarlé, Gregory Weaver, Benjamin Alan Zarrouk, Pauline Zhou, Rongpu Zou, Hu |
| contents | We perform a frequentist analysis using the standard profile likelihood method for clustering measurements from Data Release 1 of the Dark Energy Spectroscopic Instrument (DESI). While Bayesian inferences for Effective Field Theory models of galaxy clustering can be highly sensitive to the choice of priors for extended cosmological models, frequentist inferences are not susceptible to such effects. We compare Bayesian and frequentist constraints for the parameter set $\{σ_8, H_0, Ω_{\rm{m}}, w_0, w_a\}$ when fitting to the full-shape of the power spectrum multipoles, the post-reconstruction Baryon Acoustic Oscillation (BAO) measurements, as well as external datasets from the CMB and type Ia supernovae measurements. Bayesian prior effects are very significant for the $w_0w_a$CDM model; while the $1 σ$ frequentist confidence intervals encompass the maximum a posteriori (MAP), the Bayesian credible intervals almost always exclude the maximum likelihood estimate (MLE) and the MAP - indicating strong prior volume projection effects - unless supernovae data are included. We observe limited prior effects for the $Λ$CDM model, due to the reduced number of parameters. When DESI full-shape and BAO data are jointly fit, we obtain the following $1σ$ frequentist confidence intervals for $Λ$CDM ($w_0w_a$CDM): $σ_8 = 0.867^{+0.048}_{-0.041} , \ H_0 = 68.91^{+0.80}_{-0.79} \ \rm{km \ s^{-1}Mpc^{-1}} , \ Ω_{\rm{m}} = 0.3038\pm0.0110$ ($σ_8 = 0.793^{+0.069}_{-0.048} , \ H_0 = 64.9^{+4.8}_{-2.8} \ \rm{km \ s^{-1}Mpc^{-1}} , \ Ω_{\rm{m}} = 0.369^{+0.029}_{-0.059}$ , $w_0 = -0.24^{+0.17}_{-0.64}$ , $w_a = -2.5^{+1.9}_{}$), corresponding to 0.7$σ$, 0.3$σ$, 0.7$σ$ (1.9$σ$, 3.4$σ$, 5.6$σ$, 5.5$σ$, 5.6$σ$) shifts between the MLE relative to the Bayesian posterior mean for $Λ$CDM ($w_0w_a$CDM) respectively. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2508_11811 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Frequentist Cosmological Constraints from Full-Shape Clustering Measurements in DESI DR1 Morawetz, James Zhang, Hanyu Bonici, Marco Percival, Will Crespi, Andrea Aguilar, Jessica Nicole Ahlen, Steven Bianchi, Davide Brooks, David Castander, Francisco Javier Claybaugh, Todd Cole, Shaun Cuceu, Andrei de la Macorra, Axel de Mattia, Arnaud Dey, Biprateep Doel, Peter Ferraro, Simone Font-Ribera, Andreu Forero-Romero, Jaime E. Gaztañaga, Enrique Gontcho, Satya Gontcho A Gutierrez, Gaston Hahn, ChangHoon Honscheid, Klaus Huterer, Dragan Ishak, Mustapha Joyce, Dick Kehoe, Robert Kirkby, David Kisner, Theodore Lahav, Ofer Lambert, Andrew Landriau, Martin Guillou, Laurent Le Manera, Marc Miquel, Ramon Mueller, Eva-Maria Nadathur, Seshadri Newman, Jeffrey A. Niz, Gustavo Palanque-Delabrouille, Nathalie Prada, Francisco Pérez-Ràfols, Ignasi Rossi, Graziano Samushia, Lado Sanchez, Eusebio Schlegel, David Schubnell, Michael Silber, Joseph Harry Sprayberry, David Tarlé, Gregory Weaver, Benjamin Alan Zarrouk, Pauline Zhou, Rongpu Zou, Hu Cosmology and Nongalactic Astrophysics We perform a frequentist analysis using the standard profile likelihood method for clustering measurements from Data Release 1 of the Dark Energy Spectroscopic Instrument (DESI). While Bayesian inferences for Effective Field Theory models of galaxy clustering can be highly sensitive to the choice of priors for extended cosmological models, frequentist inferences are not susceptible to such effects. We compare Bayesian and frequentist constraints for the parameter set $\{σ_8, H_0, Ω_{\rm{m}}, w_0, w_a\}$ when fitting to the full-shape of the power spectrum multipoles, the post-reconstruction Baryon Acoustic Oscillation (BAO) measurements, as well as external datasets from the CMB and type Ia supernovae measurements. Bayesian prior effects are very significant for the $w_0w_a$CDM model; while the $1 σ$ frequentist confidence intervals encompass the maximum a posteriori (MAP), the Bayesian credible intervals almost always exclude the maximum likelihood estimate (MLE) and the MAP - indicating strong prior volume projection effects - unless supernovae data are included. We observe limited prior effects for the $Λ$CDM model, due to the reduced number of parameters. When DESI full-shape and BAO data are jointly fit, we obtain the following $1σ$ frequentist confidence intervals for $Λ$CDM ($w_0w_a$CDM): $σ_8 = 0.867^{+0.048}_{-0.041} , \ H_0 = 68.91^{+0.80}_{-0.79} \ \rm{km \ s^{-1}Mpc^{-1}} , \ Ω_{\rm{m}} = 0.3038\pm0.0110$ ($σ_8 = 0.793^{+0.069}_{-0.048} , \ H_0 = 64.9^{+4.8}_{-2.8} \ \rm{km \ s^{-1}Mpc^{-1}} , \ Ω_{\rm{m}} = 0.369^{+0.029}_{-0.059}$ , $w_0 = -0.24^{+0.17}_{-0.64}$ , $w_a = -2.5^{+1.9}_{}$), corresponding to 0.7$σ$, 0.3$σ$, 0.7$σ$ (1.9$σ$, 3.4$σ$, 5.6$σ$, 5.5$σ$, 5.6$σ$) shifts between the MLE relative to the Bayesian posterior mean for $Λ$CDM ($w_0w_a$CDM) respectively. |
| title | Frequentist Cosmological Constraints from Full-Shape Clustering Measurements in DESI DR1 |
| topic | Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2508.11811 |