000006072 001__ 6072
000006072 005__ 20240108164748.0
000006072 0247_ $$2DOI$$a10.1051/0004-6361/202243462
000006072 037__ $$aSCART-2023-0033
000006072 100__ $$aAndrae, R.
000006072 245__ $$aGaia Data Release 3: Analysis of the Gaia BP/RP spectra using the General Stellar Parameterizer from Photometry 
000006072 260__ $$c2023
000006072 520__ $$aContext. The astrophysical characterisation of sources is among the major new data products in the third Gaia data release (DR3). In particular, there are stellar parameters for 471 million sources estimated from low-resolution BP/RP spectra. Aims. We present the General Stellar Parameterizer from Photometry (GSP-Phot), which is part of the astrophysical parameters inference system (Apsis). GSP-Phot is designed to produce a homogeneous catalogue of parameters for hundreds of millions of single non-variable stars based on their astrometry, photometry, and low-resolution BP/RP spectra. These parameters are eective temperature, surface gravity, metallicity, absolute MG magnitude, radius, distance, and extinction for each star. Methods. GSP-Phot uses a Bayesian forward-modelling approach to simultaneously fit the BP/RP spectrum, parallax, and apparent G magnitude. A major design feature of GSP-Phot is the use of the apparent flux levels of BP/RP spectra to derive, in combination with isochrone models, tight observational constraints on radii and distances.We carefully validate the uncertainty estimates by exploiting repeat Gaia observations of the same source. Results. The data release includes GSP-Phot results for 471 million sources with G < 19. Typical dierences to literature values are 110 K for Teff and 0.2-0.25 for log g, but these depend strongly on data quality. In particular, GSP-Phot results are significantly better for stars with good parallax measurements (varpi/sigma_varpi > 20), mostly within 2kpc. Metallicity estimates exhibit substantial biases compared to literature values and are only useful at a qualitative level. However, we provide an empirical calibration of our metallicity estimates that largely removes these biases. Extinctions A0 and ABP show typical dierences from reference values of 0.07-0.09 mag. MCMC samples of the parameters are also available for 95% of the sources. Conclusions. GSP-Phot provides a homogeneous catalogue of stellar parameters, distances, and extinctions that can be used for various purposes, such as sample selections (OB stars, red giants, solar analogues etc.). In the context of asteroseismology or ground-based interferometry, where targets are usually bright and have good parallax measurements, GSP-Phot results should be particularly useful for combined analysis or target selection.
000006072 536__ $$aGaia PRODEX/$$cGaia PRODEX/$$fGaia PRODEX
000006072 594__ $$aNO
000006072 6531_ $$astars: fundamental parameters
000006072 6531_ $$amethods: data analysis
000006072 6531_ $$astatistical
000006072 6531_ $$asurveys
000006072 6531_ $$acatalogs
000006072 700__ $$aFouesneau, M.
000006072 700__ $$aSordo, R.
000006072 700__ $$aBailer-Jones, C. A. L.
000006072 700__ $$aDharmawardena, T. E.
000006072 700__ $$aRybizki, J.
000006072 700__ $$aDe Angeli, F.
000006072 700__ $$aLindstrøm, H. E. P.
000006072 700__ $$aMarshall, D. J.
000006072 700__ $$aDrimmel, R.
000006072 700__ $$aKorn, A. J.
000006072 700__ $$aSoubiran, C.
000006072 700__ $$aBrouillet, N.
000006072 700__ $$aCasamiquela, L.
000006072 700__ $$aRix, H. -W.
000006072 700__ $$aAbreu Aramburu, A.
000006072 700__ $$aÁlvarez, M. A.
000006072 700__ $$aBakker, J.
000006072 700__ $$aBellas-Velidis, I.
000006072 700__ $$aBijaoui, A.
000006072 700__ $$aBrugaletta, E.
000006072 700__ $$aBurlacu, A.
000006072 700__ $$aCarballo, R.
000006072 700__ $$aChaoul, L.
000006072 700__ $$aChiavassa, A.
000006072 700__ $$aContursi, G.
000006072 700__ $$aCooper, W. J.
000006072 700__ $$aCreevey, O. L.
000006072 700__ $$aDafonte, C.
000006072 700__ $$aDapergolas, A.
000006072 700__ $$ade Laverny, P.
000006072 700__ $$aDelchambre, L.
000006072 700__ $$aDemouchy, C.
000006072 700__ $$aEdvardsson, B.
000006072 700__ $$aFrémat, Y.
000006072 700__ $$aGarabato, D.
000006072 700__ $$aGarcía-Lario, P.
000006072 700__ $$aGarcía-Torres, M.
000006072 700__ $$aGavel, A.
000006072 700__ $$aGomez, A.
000006072 700__ $$aGonzález-Santamaría, I.
000006072 700__ $$aHatzidimitriou, D.
000006072 700__ $$aHeiter, U.
000006072 700__ $$aJean-Antoine Piccolo, A.
000006072 700__ $$aKontizas, M.
000006072 700__ $$aKordopatis, G.
000006072 700__ $$aLanzafame, A. C.
000006072 700__ $$aLebreton, Y.
000006072 700__ $$aLicata, E. L.
000006072 700__ $$aLivanou, E.
000006072 700__ $$aLobel, A.
000006072 700__ $$aLorca, A.
000006072 700__ $$aMagdaleno Romeo, A.
000006072 700__ $$aManteiga, M.
000006072 700__ $$aMarocco, F.
000006072 700__ $$aMary, N.
000006072 700__ $$aNicolas, C.
000006072 700__ $$aOrdenovic, C.
000006072 700__ $$aPailler, F.
000006072 700__ $$aPalicio, P. A.
000006072 700__ $$aPallas-Quintela, L.
000006072 700__ $$aPanem, C.
000006072 700__ $$aPichon, B.
000006072 700__ $$aPoggio, E.
000006072 700__ $$aRecio-Blanco, A.
000006072 700__ $$aRiclet, F.
000006072 700__ $$aRobin, C.
000006072 700__ $$aSantoveña, R.
000006072 700__ $$aSarro, L. M.
000006072 700__ $$aSchultheis, M. S.
000006072 700__ $$aSegol, M.
000006072 700__ $$aSilvelo, A.
000006072 700__ $$aSlezak, I.
000006072 700__ $$aSmart, R. L.
000006072 700__ $$aSüveges, M.
000006072 700__ $$aThévenin, F.
000006072 700__ $$aTorralba Elipe, G.
000006072 700__ $$aUlla, A.
000006072 700__ $$aUtrilla, E.
000006072 700__ $$aVallenari, A.
000006072 700__ $$avan Dillen, E.
000006072 700__ $$aZhao, H.
000006072 700__ $$aZorec, J.
000006072 773__ $$cA27 (22p)$$pAstronomy & Astrophysics$$v674$$y2023
000006072 8560_ $$fronny.blomme@observatoire.be
000006072 85642 $$ahttps://ui.adsabs.harvard.edu/abs/2022arXiv220606138A/abstract
000006072 85642 $$ahttps://arxiv.org/abs/2206.06138
000006072 905__ $$apublished in
000006072 980__ $$aREFERD