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Table · dataset · 2025

Elemental abundances from DESI EDR spectra

Listed in IVOA Registry (Virtual Observatory)

Stellar abundances for a large number of stars provide key information for the study of Galactic formation history.

Description

Large spectroscopic surveys such as the Dark Energy Spectroscopic Instrument (DESI) and LAMOST take median-to-low-resolution (R<~5000) spectra in the full optical wavelength range for millions of stars. However, the line-blending effect in these spectra causes great challenges for elemental abundance determination.

Here we employ DD-Payne, a data-driven method regularized by differential spectra from stellar physical models, to the DESI early data release spectra for stellar abundance determination. Our implementation delivers 15 labels, including effective temperature Teff, surface gravity logg, microturbulence velocity v_mic_, and the abundances for 12 individual elements, namely C, N, O, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, and Ni.

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Given a spectral signal-to-noise ratio of 100 per pixel, the internal precisions of the label estimates are about 20K for Teff, 0.05dex for logg, and 0.05dex for most elemental abundances. These results agree with the theoretical limits from the Cramer-Rao bound calculation within a factor of 2. The majority of the accreted halo stars contributed by the Gaia-Enceladus-Sausage are discernible from the disk and in situ halo populations in the resultant [Mg/Fe]-[Fe/H] and [Al/Fe]-[Fe/H] abundance spaces.

We also provide distance and orbital parameters for the sample stars, which spread over a distance out to ~100kpc. The DESI sample has a significantly higher fraction of distant (or metal- poor) stars than the other existing spectroscopic surveys, making it a powerful data set for studying the Galactic outskirts.

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Catalogue records · 2

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