000006058 001__ 6058
000006058 005__ 20240108165934.0
000006058 0247_ $$2DOI$$a10.1051/0004-6361/202243919
000006058 037__ $$aSCART-2023-0019
000006058 100__ $$aFouesneau, M.
000006058 245__ $$aGaia Data Release 3: Apsis II -- Stellar Parameters
000006058 260__ $$c2023
000006058 520__ $$aContext. The third Gaia data release (Gaia DR3) contains, beyond the astrometry and photometry, dispersed light for hundreds of millions of sources from the Gaia prism spectra (BP and RP) and the spectrograph (RVS). This data release opens a new window on the chemo-dynamical properties of stars in our Galaxy, essential knowledge for understanding the structure, formation, and evolution of the Milky Way. Aims. To provide insight into the physical properties of Milky Way stars, we used these data to produce a uniformly-derived, all-sky catalog of stellar astrophysical parameters (APs): atmospheric properties (Teff, log g, [M/H], [alpha/Fe], activity index, emission lines, rotation), 13 chemical abundance estimates, evolution characteristics (radius, age, mass, bolometric luminosity), distance, and dust extinction. Methods. We developed the astrophysical parameters inference system (Apsis) pipeline to infer APs of Gaia objects by analyzing their astrometry, photometry, BP/RP, and RVS spectra. We validate our results against other works in the literature, including benchmark stars, interferometry, and asteroseismology. Here we assessed the stellar analysis performance from Apsis statistically. Results. We describe the quantities we obtained, including the underlying assumptions and the limitations of our results. We provide guidance and identify regimes in which our parameters should and should not be used. Conclusions. Despite some limitations, this is the most extensive catalog of uniformly-inferred stellar parameters to date. These comprise Te, log g, and [M=H] (470 million using BP/RP, 6 million using RVS), radius (470 million), mass (140 million), age (120 million), chemical abundances (5 million), diffuse interstellar band analysis (1/2 million), activity indices (2 million), Halpha equivalent widths (200 million), and further classification of spectral types (220 million) and emission-line stars (50 thousand). More precise and detailed astrophysical parameters based on epoch BP, RP, and RVS spectrophotometry are planned for the next Gaia data release. Our catalog is available from the Gaia Archive and partner data centers.
000006058 536__ $$aGaia PRODEX/$$cGaia PRODEX/$$fGaia PRODEX
000006058 594__ $$aNO
000006058 6531_ $$astars: distances
000006058 6531_ $$astars: fundamental parameters
000006058 6531_ $$amethods: statistical
000006058 6531_ $$aGalaxy: stellar content
000006058 6531_ $$aISM: dust extinction
000006058 6531_ $$aCatalogs
000006058 700__ $$aFrémat, Y.
000006058 700__ $$aAndrae, R.
000006058 700__ $$aKorn, A. J.
000006058 700__ $$aSoubiran, C.
000006058 700__ $$aKordopatis, G.
000006058 700__ $$aVallenari, A.
000006058 700__ $$aHeiter, U.
000006058 700__ $$aCreevey, O. L.
000006058 700__ $$aSarro, L. M.
000006058 700__ $$ade Laverny, P.
000006058 700__ $$aLanzafame, A. C.
000006058 700__ $$aLobel, A.
000006058 700__ $$aSordo, R.
000006058 700__ $$aRybizki, J.
000006058 700__ $$aSlezak, I.
000006058 700__ $$aÁlvarez, M. A.
000006058 700__ $$aDrimmel, R.
000006058 700__ $$aGarabato, D.
000006058 700__ $$aDelchambre, L.
000006058 700__ $$aBailer-Jones, C. A. L.
000006058 700__ $$aHatzidimitriou, D.
000006058 700__ $$aLorca, A.
000006058 700__ $$aLe Fustec, Y.
000006058 700__ $$aPailler, F.
000006058 700__ $$aMary, N.
000006058 700__ $$aRobin, C.
000006058 700__ $$aUtrilla, E.
000006058 700__ $$aAbreu Aramburu, A.
000006058 700__ $$aBakker, J.
000006058 700__ $$aBellas-Velidis, I.
000006058 700__ $$aBijaoui, A.
000006058 700__ $$aBlomme, R.
000006058 700__ $$aBouret, J. -C.
000006058 700__ $$aBrouillet, N.
000006058 700__ $$aBrugaletta, E.
000006058 700__ $$aBurlacu, A.
000006058 700__ $$aCarballo, R.
000006058 700__ $$aCasamiquela, L.
000006058 700__ $$aChaoul, L.
000006058 700__ $$aChiavassa, A.
000006058 700__ $$aContursi, G.
000006058 700__ $$aCooper, W. J.
000006058 700__ $$aDafonte, C.
000006058 700__ $$aDemouchy, C.
000006058 700__ $$aDharmawardena, T. E.
000006058 700__ $$aGarcía-Lario, P.
000006058 700__ $$aGarcía-Torres, M.
000006058 700__ $$aGomez, A.
000006058 700__ $$aGonzález-Santamaría, I.
000006058 700__ $$aJean-Antoine Piccolo, A.
000006058 700__ $$aKontizas, M.
000006058 700__ $$aLebreton, Y.
000006058 700__ $$aLicata, E. L.
000006058 700__ $$aLindstrøm, H. E. P.
000006058 700__ $$aLivanou, E.
000006058 700__ $$aMagdaleno Romeo, A.
000006058 700__ $$aManteiga, M.
000006058 700__ $$aMarocco, F.
000006058 700__ $$aMartayan, C.
000006058 700__ $$aMarshall, D. J.
000006058 700__ $$aNicolas, C.
000006058 700__ $$aOrdenovic, C.
000006058 700__ $$aPalicio, P. A.
000006058 700__ $$aPallas-Quintela, L.
000006058 700__ $$aPichon, B.
000006058 700__ $$aPoggio, E.
000006058 700__ $$aRecio-Blanco, A.
000006058 700__ $$aRiclet, F.
000006058 700__ $$aSantoveña, R.
000006058 700__ $$aSchultheis, M. S.
000006058 700__ $$aSegol, M.
000006058 700__ $$aSilvelo, A.
000006058 700__ $$aSmart, R. L.
000006058 700__ $$aSüveges, M.
000006058 700__ $$aThévenin, F.
000006058 700__ $$aTorralba Elipe, G.
000006058 700__ $$aUlla, A.
000006058 700__ $$avan Dillen, E.
000006058 700__ $$aZhao, H.
000006058 700__ $$aZorec, J.
000006058 773__ $$cA28 (36pp)$$pAstronomy & Astrophysics$$v674$$y2023
000006058 8560_ $$fronny.blomme@observatoire.be
000006058 85642 $$ahttps://ui.adsabs.harvard.edu/abs/2022arXiv220605992F/abstract
000006058 85642 $$ahttps://arxiv.org/abs/2206.05992
000006058 905__ $$apublished in
000006058 980__ $$aREFERD