Results from the Dark Energy Spectroscopic Instrument (DESI) year-one data release.

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• Héctor Gil-Marín (ICC, Barcelona U.)
• Monday 03 February 2025, 13:00-14:00
• CMS, Pav. B, CTC Common Room (B1.19) [Potter Room].

If you have a question about this talk, please contact Thomas Colas.

DESI represents the culmination of multi-years efforts and advanced spectroscopic techniques. Placed at Mayall 4-meter Telescope, DESI harnesses the power of 5,000 robotic fiber positioners, coupled with state-of-the-art spectrographs, to capture the spectral signatures of millions of galaxies and quasars with unprecedented precision. DESI success is also based on the collaborative spirit of its community, more than 400 scientists over 70 institutions in 5 continents.

This data release (DR1) corresponds to the first year of observations; it holds immense scientific promise across a multitude of fronts: from constraining cosmological parameters, mapping the expansion history of the Universe, to the properties of dark energy, gravity and neutrinos.

In this talk I will focus on the results from the first data release of DESI based on the baryon acoustic oscillations (BAO) and redshift space distortions (RSD) analyses, and their impact in cosmology. On one hand, the BAO signal allows us to trace the expansion history of the universe through the last 11 billion years; and on the other hand the RSD allows us to test GR at cosmological scales over a similar period of time. In addition if baryon density information is added, DESI can also infer the rate of expansion today, the Hubble constant at 1% level (H0=68.56 ± 0.75) km/s/Mpc. All these results seem to be in good agreement with the standard model of cosmology, the LCDM model. When combined with external datasets such as the SuperNovae data and Cosmic Microwave Background anisotropy observations (CMB), we have observed in some cases interesting hints towards evolving dark energy. Furthermore, DESI data in combination with CMB is able to put constraints on the sum of neutrino masses reaching an upper bound of 0.071 eV at 95% confidence level within the LCDM model.

This talk is part of the Cosmology Lunch series.

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