000006066 001__ 6066
000006066 005__ 20240108165245.0
000006066 0247_ $$2DOI$$a10.1051/0004-6361/202243685
000006066 037__ $$aSCART-2023-0027
000006066 100__ $$aBlomme, R.
000006066 245__ $$aGaia Data Release 3: Hot-star radial velocities
000006066 260__ $$c2023
000006066 520__ $$aContext. The second Gaia data release, DR2, contained radial velocities of stars with effective temperatures up to Teff = 6900 K. The third data release, Gaia DR3, extends this up to Teff = 14 500 K. Aims. We derive the radial velocities for hot stars (i.e. in the Teff = 6900 - 14 500 K range) from data obtained with the Radial Velocity Spectrometer (RVS) on board Gaia. Methods. The radial velocities were determined by the standard technique of measuring the Doppler shift of a template spectrum that was compared to the observed spectrum. The RVS wavelength range is very limited. The proximity to and systematic blueward offset of the calcium infrared triplet to the hydrogen Paschen lines in hot stars can result in a systematic offset in radial velocity. For the hot stars, we developed a specific code to improve the selection of the template spectrum, thereby avoiding this systematic offset. Results. With the improved code, and with the correction we propose to the DR3 archive radial velocities, we obtain values that agree with reference values to within 3 km/s (in median). Because of the required S/N for applying the improved code, the hot star radial velocities in DR3 are mostly limited to stars with a magnitude in the RVS wavelength band <= 12 mag.
000006066 536__ $$aGaia PRODEX/$$cGaia PRODEX/$$fGaia PRODEX
000006066 594__ $$aNO
000006066 6531_ $$aTechniques: spectroscopic
000006066 6531_ $$aTechniques: radial velocities
000006066 6531_ $$aMethods: data analysis
000006066 6531_ $$aCatalogs
000006066 6531_ $$aSurveys
000006066 6531_ $$aStars: massive
000006066 700__ $$aFremat, Y.
000006066 700__ $$aSartoretti, P.
000006066 700__ $$aGuerrier, A.
000006066 700__ $$aPanuzzo, P.
000006066 700__ $$aKatz, D.
000006066 700__ $$aSeabroke, G. M.
000006066 700__ $$aThevenin, F.
000006066 700__ $$aCropper, M.
000006066 700__ $$aBenson, K.
000006066 700__ $$aDamerdji, Y.
000006066 700__ $$aHaigron, R.
000006066 700__ $$aMarchal, O.
000006066 700__ $$aSmith, M.
000006066 700__ $$aBaker, S.
000006066 700__ $$aChemin, L.
000006066 700__ $$aDavid, M.
000006066 700__ $$aDolding, C.
000006066 700__ $$aGosset, E.
000006066 700__ $$aJanssen, K.
000006066 700__ $$aJasniewicz, G.
000006066 700__ $$aLobel, A.
000006066 700__ $$aPlum, G.
000006066 700__ $$aSamaras, N.
000006066 700__ $$aSnaith, O.
000006066 700__ $$aSoubiran, C.
000006066 700__ $$aVanel, O.
000006066 700__ $$aZwitter, T.
000006066 700__ $$aBrouillet, N.
000006066 700__ $$aCaffau, E.
000006066 700__ $$aCrifo, F.
000006066 700__ $$aFabre, C.
000006066 700__ $$aFragkoudi, F.
000006066 700__ $$aHuckle, H. E.
000006066 700__ $$aJean-Antoine Piccolo, A.
000006066 700__ $$aLasne, Y.
000006066 700__ $$aLeclerc, N.
000006066 700__ $$aMastrobuono-Battisti, A.
000006066 700__ $$aRoyer, F.
000006066 700__ $$aViala, Y.
000006066 700__ $$aZorec, J.
000006066 773__ $$cA7 (12pp)$$pAstronomy & Astrophysics$$v674$$y2023
000006066 8560_ $$fronny.blomme@observatoire.be
000006066 85642 $$ahttps://ui.adsabs.harvard.edu/abs/2022arXiv220605486B/abstract
000006066 85642 $$ahttps://arxiv.org/abs/2206.05486
000006066 905__ $$apublished in
000006066 980__ $$aREFERD