|Gaia Data Release 2: Processing the spectroscopic data |
Auteur(s): Sartoretti P., Katz D., Cropper M., Panuzzo P., Seabroke G. m., Viala Y., Benson K., Blomme R., Jasniewicz G., Jean-antoine A., Huckle H., Smith M., Baker S., Crifo F., Damerdji Y., David M., Dolding C., Fremat Y., Gosset E., Guerrier A., Guy L. p., Haigron R., Janssen K., Marchal O., Plum G., Soubiran C., Thevenin F., Ajaj M., Prieto C. allende, Zurbach C.
(Document sans référence bibliographique) 2018-04-25
Ref Arxiv: 1804.09371
Ref. & Cit.: NASA ADS
The Gaia Data Release 2 contains the 1st release of radial velocities complementing the kinematic data of a sample of about 7 million relatively bright, late-type stars. Aims: This paper provides a detailed description of the Gaia spectroscopic data processing pipeline, and of the approach adopted to derive the radial velocities presented in DR2. Methods: The pipeline must perform four main tasks: (i) clean and reduce the spectra observed with the Radial Velocity Spectrometer (RVS); (ii) calibrate the RVS instrument, including wavelength, straylight, line-spread function, bias non-uniformity, and photometric zeropoint; (iii) extract the radial velocities; and (iv) verify the accuracy and precision of the results. The radial velocity of a star is obtained through a fit of the RVS spectrum relative to an appropriate synthetic template spectrum. An additional task of the spectroscopic pipeline was to provide 1st-order estimates of the stellar atmospheric parameters required to select such template spectra. We describe the pipeline features and present the detailed calibration algorithms and software solutions we used to produce the radial velocities published in DR2. Results: The spectroscopic processing pipeline produced median radial velocities for Gaia stars with narrow-band near-IR magnitude Grvs < 12 (i.e. brighter than V~13). Stars identified as double-lined spectroscopic binaries were removed from the pipeline, while variable stars, single-lined, and non-detected double-lined spectroscopic binaries were treated as single stars. The scatter in radial velocity among different observations of a same star, also published in DR2, provides information about radial velocity variability. For the hottest (Teff > 7000 K) and coolest (Teff < 3500 K) stars, the accuracy and precision of the stellar parameter estimates are not sufficient to allow selection of appropriate templates. [Abridged]
Commentaires: 25 pages, 17 figures, accepted for publication in A&A as part of the Gaia 2nd data release special issue