000006075 001__ 6075
000006075 005__ 20240108164542.0
000006075 0247_ $$2DOI$$a10.1051/0004-6361/202243750
000006075 037__ $$aSCART-2023-0036
000006075 100__ $$aRecio-Blanco, A.
000006075 245__ $$aGaia Data Release 3: Analysis of RVS spectra using the General Stellar Parametriser from spectroscopy
000006075 260__ $$c2023
000006075 520__ $$aContext. The chemo-physical parametrisation of stellar spectra is essential for understanding the nature and evolution of stars and of Galactic stellar populations. A worldwide observational effort from the ground has provided, in one century, an extremely heterogeneous collection of chemical abundances for about two million stars in total, with fragmentary sky coverage. Aims. This situation is revolutionised by the Gaia third data release (DR3), which contains the parametrisation of Radial Velocity Spectrometer (RVS) data performed by the General Stellar Parametriser-spectroscopy, GSP-Spec, module. Here we describe the parametrisation of the first 34 months of Gaia RVS observations. Methods. GSP-Spec estimates the chemo-physical parameters from combined RVS spectra of single stars, without additional inputs from astrometric, photometric, or spectro-photometric BP/RP data. The main analysis workflow described here, MatisseGauguin, is based on projection and optimisation methods and provides the stellar atmospheric parameters; the individual chemical abundances of N, Mg, Si, S, Ca, Ti, Cr, Fe i, Fe ii, Ni, Zr, Ce and Nd; the differential equivalent width of a cyanogen line; and the parameters of a diuse interstellar band (DIB) feature. Another workflow, based on an artificial neural network (ANN) and referred to with the same acronym, provides a second set of atmospheric parameters that are useful for classification control. For both workflows, we implement a detailed quality flag chain considering different error sources. Results. With about 5.6 million stars, the Gaia DR3 GSP-Spec all-sky catalogue is the largest compilation of stellar chemo-physical parameters ever published and the first one from space data. Internal and external biases have been studied taking into account the implemented flags. In some cases, simple calibrations with low degree polynomials are suggested. The homogeneity and quality of the estimated parameters enables chemo-dynamical studies of Galactic stellar populations, interstellar extinction studies from individual spectra, and clear constraints on stellar evolution models. We highly recommend that users adopt the provided quality flags for scientific exploitation. Conclusions. The Gaia DR3 GSP-Spec catalogue is a major step in the scientific exploration of Milky Way stellar populations. It will be followed by increasingly large and higher quality catalogues in future data releases, confirming the Gaia promise of a new Galactic vision.
000006075 536__ $$aGa/$$cGa/$$fGa
000006075 594__ $$aNO
000006075 6531_ $$aStars: fundamental parameters
000006075 6531_ $$aStars: abundances
000006075 6531_ $$aISM: lines and bands
000006075 6531_ $$aGalaxy: stellar content
000006075 6531_ $$aGalaxy: abundances
000006075 6531_ $$aMethods:data analysis
000006075 700__ $$ade Laverny, P.
000006075 700__ $$aPalicio, P. A.
000006075 700__ $$aKordopatis, G.
000006075 700__ $$aÁlvarez, M. A.
000006075 700__ $$aSchultheis, M.
000006075 700__ $$aContursi, G.
000006075 700__ $$aZhao, H.
000006075 700__ $$aTorralba Elipe, G.
000006075 700__ $$aOrdenovic, C.
000006075 700__ $$aManteiga, M.
000006075 700__ $$aDafonte, C.
000006075 700__ $$aOreshina-Slezak, I.
000006075 700__ $$aBijaoui, A.
000006075 700__ $$aFremat, Y.
000006075 700__ $$aSeabroke, G.
000006075 700__ $$aPailler, F.
000006075 700__ $$aSpitoni, E.
000006075 700__ $$aPoggio, E.
000006075 700__ $$aCreevey, O. L.
000006075 700__ $$aAbreu Aramburu, A.
000006075 700__ $$aAccart, S.
000006075 700__ $$aAndrae, R.
000006075 700__ $$aBailer-Jones, C. A. L.
000006075 700__ $$aBellas-Velidis, I.
000006075 700__ $$aBrouillet, N.
000006075 700__ $$aBrugaletta, E.
000006075 700__ $$aBurlacu, A.
000006075 700__ $$aCarballo, R.
000006075 700__ $$aCasamiquela, L.
000006075 700__ $$aChiavassa, A.
000006075 700__ $$aCooper, W. J.
000006075 700__ $$aDapergolas, A.
000006075 700__ $$aDelchambre, L.
000006075 700__ $$aDharmawardena, T. E.
000006075 700__ $$aDrimmel, R.
000006075 700__ $$aEdvardsson, B.
000006075 700__ $$aFouesneau, M.
000006075 700__ $$aGarabato, D.
000006075 700__ $$aGarcia-Lario, P.
000006075 700__ $$aGarcia-Torres, M.
000006075 700__ $$aGavel, A.
000006075 700__ $$aGomez, A.
000006075 700__ $$aGonzalez-Santamaria, I.
000006075 700__ $$aHatzidimitriou, D.
000006075 700__ $$aHeiter, U.
000006075 700__ $$aJean-Antoine Piccolo, A.
000006075 700__ $$aKontizas, M.
000006075 700__ $$aKorn, A. J.
000006075 700__ $$aLanzafame, A. C.
000006075 700__ $$aLebreton, Y.
000006075 700__ $$aLe Fustec, Y.
000006075 700__ $$aLicata, E. L.
000006075 700__ $$aLindstrom, H. E. P.
000006075 700__ $$aLivanou, E.
000006075 700__ $$aLobel, A.
000006075 700__ $$aLorca, A.
000006075 700__ $$aMagdaleno Romeo, A.
000006075 700__ $$aMarocco, F.
000006075 700__ $$aMarshall, D. J.
000006075 700__ $$aMary, N.
000006075 700__ $$aNicolas, C.
000006075 700__ $$aPallas-Quintela, L.
000006075 700__ $$aPanem, C.
000006075 700__ $$aPichon, B.
000006075 700__ $$aRiclet, F.
000006075 700__ $$aRobin, C.
000006075 700__ $$aRybizki, J.
000006075 700__ $$aSantovena, R.
000006075 700__ $$aSilvelo, A.
000006075 700__ $$aSmart, R. L.
000006075 700__ $$aSarro, L. M.
000006075 700__ $$aSordo, R.
000006075 700__ $$aSoubiran, C.
000006075 700__ $$aSuvege, M.
000006075 700__ $$aUlla, A.
000006075 700__ $$aVallenari, A.
000006075 700__ $$aZorec, J.
000006075 700__ $$aUtrilla, E.
000006075 700__ $$aBakker, J.
000006075 773__ $$cA29 (43pp)$$pAstronomy & Astrophysics$$v674$$y2023
000006075 8560_ $$fronny.blomme@observatoire.be
000006075 85642 $$ahttps://ui.adsabs.harvard.edu/abs/2022arXiv220605541R/abstract
000006075 85642 $$ahttps://arxiv.org/abs/2206.05541
000006075 905__ $$apublished in
000006075 980__ $$aREFERD