http://arxiv.org/abs/2105.09014
Under certain conditions, stellar radial velocities can be determined from astrometry, without any use of spectroscopy. This enables to identify phenomena other than the Doppler effect, that are displacing spectral lines. We aim to use the change of stellar proper motions over time (perspective acceleration) to determine radial velocities from accurate astrometric data, now available from the Gaia and Hipparcos missions. Positions and proper motions at the epoch of Hipparcos are compared with values propagated back from the epoch of the Gaia Early Data Release 3. This propagation depends on the radial velocity, which obtains its value from an optimal fit, assuming space motion to be uniform relative to the solar system barycentre. For 926 nearby stars we obtain astrometric radial velocities with formal uncertainties better than 100 km/s; for 55 stars the uncertainty is below 10 km/s, and for seven it is below 1 km/s. Most stars that are not components of double or multiple systems show good agreement with available spectroscopic radial velocities. Astrometry offers geometric methods to determine stellar radial velocity, irrespective of complexities in stellar spectra. This enables to segregate wavelength displacements caused by the radial motion of the stellar centre-of-mass from those induced by other effects, such as gravitational redshifts in white dwarfs.
L. Lindegren and D. Dravins
Thu, 20 May 21
24/56
Comments: 6 pages, 2 figures, 2 tables. Submitted to Astronomy & Astrophysics
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