000006062 001__ 6062
000006062 005__ 20240108165557.0
000006062 0247_ $$2DOI$$a10.1051/0004-6361/202243615
000006062 037__ $$aSCART-2023-0023
000006062 100__ $$aSartoretti, P.
000006062 245__ $$aGaia Data Release 3: G_RVS photometry from the RVS spectra 
000006062 260__ $$c2023
000006062 520__ $$aContext. Gaia Data Release 3 (DR3) contains the first release of magnitudes estimated from the integration of Radial Velocity Spectrometer (RVS) spectra for a sample of about 32.2 million stars brighter than GRVS ~ 14 mag (or G ~ 15 mag). Aims. In this paper, we describe the data used and the approach adopted to derive and validate the GRVS magnitudes published in DR3. We also provide estimates of the GRVS passband and associated GRVS zero-point. Methods. We derived GRVS photometry from the integration of RVS spectra over the wavelength range from 846 to 870 nm. We processed these spectra following a procedure similar to that used for DR2, but incorporating several improvements that allow a better estimation of GRVS. These improvements pertain to the stray-light background estimation, the line spread function calibration, and the detection of spectra contaminated by nearby relatively bright sources. We calibrated the GRVS zero-point every 30 hours based on the reference magnitudes of constant stars from the Hipparcos catalogue, and used them to transform the integrated flux of the cleaned and calibrated spectra into epoch magnitudes. The GRVS magnitude of a star published in DR3 is the median of the epoch magnitudes for that star. We estimated the GRVS passband by comparing the RVS spectra of 108 bright stars with their flux-calibrated spectra from external spectrophotometric libraries. Results. The GRVS magnitude provides information that is complementary to that obtained from the G, GBP, and GRP magnitudes, which is useful for constraining stellar metallicity and interstellar extinction. The median precision of GRVS measurements ranges from about 0.006 mag for the brighter stars (i.e. with 3.5 <= GRVS <= 6.5 mag) to 0.125 mag at the faint end. The derived GRVS passband shows that the effective transmittance of the RVS is approximately 1.23 times better than the pre-launch estimate.
000006062 536__ $$aGaia PRODEX/$$cGaia PRODEX/$$fGaia PRODEX
000006062 594__ $$aNO
000006062 6531_ $$aTechniques: spectroscopic
000006062 6531_ $$aTechniques: photometric
000006062 6531_ $$aCatalogues
000006062 6531_ $$aSurveys
000006062 700__ $$aMarchal, O.
000006062 700__ $$aBabusiaux, C.
000006062 700__ $$aJordi, C.
000006062 700__ $$aGuerrier, A.
000006062 700__ $$aPanuzzo, P.
000006062 700__ $$aKatz, D.
000006062 700__ $$aSeabroke, G. M.
000006062 700__ $$aThévenin, F.
000006062 700__ $$aCropper, M.
000006062 700__ $$aBenson, K.
000006062 700__ $$aBlomme, R.
000006062 700__ $$aHaigron, R.
000006062 700__ $$aSmith, M.
000006062 700__ $$aBaker, S.
000006062 700__ $$aChemin, L.
000006062 700__ $$aDavid, M.
000006062 700__ $$aDolding, C.
000006062 700__ $$aFrémat, Y.
000006062 700__ $$aJanssen, K.
000006062 700__ $$aJasniewicz, G.
000006062 700__ $$aLobel, A.
000006062 700__ $$aPlum, G.
000006062 700__ $$aSamaras, N.
000006062 700__ $$aSnaith, O.
000006062 700__ $$aSoubiran, C.
000006062 700__ $$aVanel, O.
000006062 700__ $$aZwitter, T.
000006062 700__ $$aBrouillet, N.
000006062 700__ $$aCaffau, E.
000006062 700__ $$aCrifo, F.
000006062 700__ $$aFabre, C.
000006062 700__ $$aFragkoudi, F.
000006062 700__ $$aJean-Antoine Piccolo, A.
000006062 700__ $$aHuckle, H. E.
000006062 700__ $$aLasne, Y.
000006062 700__ $$aLeclerc, N.
000006062 700__ $$aMastrobuono-Battisti, A.
000006062 700__ $$aRoyer, F.
000006062 700__ $$aViala, Y.
000006062 700__ $$aZorec, J.
000006062 773__ $$cA6 (15pp)$$pAstronomy & Astrophysics$$v674$$y2023
000006062 8560_ $$fronny.blomme@observatoire.be
000006062 85642 $$ahttps://ui.adsabs.harvard.edu/abs/2022arXiv220605725S/abstract
000006062 85642 $$ahttps://arxiv.org/abs/2206.05725
000006062 905__ $$apublished in
000006062 980__ $$aREFERD