We present the first independent reanalysis of the galaxy clustering data from DESI Data Release 1, utilizing an effective field theory full-shape model. We analyze the power spectra and bispectra of the public catalogs using a custom-built pipeline based on window-deconvolved quasioptimal estimators, accounting for a number of systematic effects. Compared to the official collaboration analysis, we add the galaxy power spectrum hexadecapole and the bispectrum monopole, and also introduce a novel stochastic estimator for fiber collisions, which facilitates robust bispectrum analyses. As a first application, we perform a full-shape analysis of the DESI power spectra and bispectra in the context of the standard cosmological model, $\mathrm{\Lambda }$ cold dark matter ($\mathrm{\Lambda }\mathrm{CDM}$). Using external priors on the physical baryon density and the primordial power spectrum tilt, we constrain the matter density fraction to ${\mathrm{\Omega }}_m=0.284\pm 0.011$, the Hubble constant to $H_0=70.7\pm 1.1\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$, and the mass fluctuation amplitude to ${\sigma }_8=0.811\pm 0.030$. The bispectrum sharpens constraints on ${\sigma }_8$ and ${\mathrm{\Omega }}_m$ by $\approx 10\%$ and shifts ${\mathrm{\Omega }}_m$ by $\approx 1\sigma$ toward the Planck $\mathrm{\Lambda }\mathrm{CDM}$ value. Combining our full-shape likelihood with the official DESI DR2 baryon acoustic oscillation (BAO) measurements, cosmological parameters shift further toward the Planck values, with ${\mathrm{\Omega }}_m=0.296\pm 0.007$, $H_0=68.8\pm 0.6\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$, ${\sigma }_8=0.818\pm 0.029$ (with tighter constraints obtained in joint analyses). Similar results are obtained in a joint analysis with DR1 BAO, accounting for the cross-covariance. Finally, the bispectrum data improves measurements of quadratic bias parameters, which are consistent with predictions from halo occupation distribution models. Our work highlights the importance of higher-order statistics and sets the stage for upcoming full-shape analyses of nonminimal cosmological models.

Close

PrevNext

View figure in article

• 
• 
• 
• 
• 
• 
• 
• 
• 
• 
• 
• 
• 
• 
• 

• Cosmological parameters
• Large scale structure of the Universe
• Data analysis