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Gaia Data Release 3 : Hot-star radial velocities

Blomme, R. ; Frémat, Y. ; Sartoretti, P. ; Guerrier, A. ; Panuzzo, P. ; Katz, D. ; Seabroke, G. M. ; Thévenin, F. ; Cropper, M. and Benson, K. , et al. (2023) In Astronomy and Astrophysics 674.
Abstract

Context. 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 500K 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... (More)

Context. 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 500K 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..1 (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.

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organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
Catalogs, Methods: data analysis, Stars: massive, Surveys, Techniques: radial velocities, Techniques: spectroscopic
in
Astronomy and Astrophysics
volume
674
article number
A7
publisher
EDP Sciences
external identifiers
  • scopus:85163663838
ISSN
0004-6361
DOI
10.1051/0004-6361/202243685
language
English
LU publication?
yes
id
3ca6af3f-be7f-43c6-beed-0f732155b036
date added to LUP
2023-09-18 14:42:30
date last changed
2024-03-22 00:40:25
@article{3ca6af3f-be7f-43c6-beed-0f732155b036,
  abstract     = {{<p>Context. 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 500K 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..1 (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 &amp;le;12 mag.</p>}},
  author       = {{Blomme, R. and Frémat, Y. and Sartoretti, P. and Guerrier, A. and Panuzzo, P. and Katz, D. and Seabroke, G. M. and Thévenin, F. and Cropper, M. and Benson, K. and Damerdji, Y. and Haigron, R. and Marchal, O. and Smith, M. and Baker, S. and Chemin, L. and David, M. and Dolding, C. and Gosset, E. and Janaben, K. and Jasniewicz, G. and Lobel, A. and Plum, G. and Samaras, N. and Snaith, O. and Soubiran, C. and Vanel, O. and Zwitter, T. and Brouillet, N. and Caffau, E. and Crifo, F. and Fabre, C. and Fragkoudi, F. and Huckle, H. E. and Jean-Antoine Piccolo, A. and Lasne, Y. and Leclerc, N. and Mastrobuono-Battisti, A. and Royer, F. and Viala, Y. and Zorec, J.}},
  issn         = {{0004-6361}},
  keywords     = {{Catalogs; Methods: data analysis; Stars: massive; Surveys; Techniques: radial velocities; Techniques: spectroscopic}},
  language     = {{eng}},
  publisher    = {{EDP Sciences}},
  series       = {{Astronomy and Astrophysics}},
  title        = {{Gaia Data Release 3 : Hot-star radial velocities}},
  url          = {{http://dx.doi.org/10.1051/0004-6361/202243685}},
  doi          = {{10.1051/0004-6361/202243685}},
  volume       = {{674}},
  year         = {{2023}},
}