Radial Velocity Spectrometer Design and Performance

Details Radial Velocity Spectrometer Design and Performance Radial Velocity Spectrometer Design and Performance

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005esasp.576...51k&link_type=abstract

"Proceedings of the Gaia Symposium "The Three-Dimensional Universe with Gaia" (ESA SP-576). Held at the Observatoire de Paris-Me

Astronomy and Astrophysics

Astronomy

Gaia, Space Vehicles Instruments, Instrumentation Spectrographs, Techniques Spectroscopic, Techniques Radial Velocities

Scientific paper

The Radial Velocity Spectrometer (RVS) is an integral field spectrograph dispersing all the light entering its ˜2.5×1.6 deg2 field of view, with a resolving power R = λ/μλ = 11 500. The wavelength range of the RVS, [848-874] nm, contains strong spectral features (Ca II triplet in intermediate and late-type stars and Hydrogen Paschen lines in early-type stars) as well as measurable weak lines (e.g., Si I or Mg I). The RVS will collect the spectra of about 100-150 million stars down to magnitude V 17-18. Each source will be observed on average, at 93 successive epochs. The main aim of the RVS is the acquisition of the radial velocities. As third components of the velocity vectors, the radial velocities are crucial to study the kinematical and dynamical history of the Milky Way. Multi-epoch radial velocities will also be very useful to identify and characterise double and multiple systems. Moreover, the radial velocities are necessary to correct the astrometric measurements from perspective acceleration. The RVS should derive radial velocities with precisions, at the end of the mission, for e.g., a solar metallicity G5 dwarf, of ˜3.5 km s-1 at V = 16 and ˜9.5 km s-1 at V = 17. The RVS will also provide rotational velocities, atmospheric parameters, individual abundances, interstellar reddening as well as numerous stellar diagnostics (e.g., variability, mass loss).

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