paper

Hypervelocity star candidates from Gaia DR2 and DR3 proper motions and parallaxes

arXiv:2402.10714 · doi:10.1051/0004-6361/202348430

Abstract

Hypervelocity stars (HVSs) unbound to the Galaxy can be formed with extreme stellar interactions. Observational evidence comes from measurements of radial velocities (RVs) of objects crossing the Galactic halo and of tangential velocities based on high proper motions (HPMs) and distances of relatively nearby stars. I searched for new HVS candidates and reviewed known objects using their Gaia astrometric measurements. Candidates were selected with significant Gaia parallaxes of >0.1mas, proper motions of >20mas/yr, and computed Galactocentric tangential velocities >500km/s. The DR2 and DR3 samples of several thousand HVS candidates were studied with respect to their proper motions, sky distribution, number of observations, location in crowded fields, colour-magnitude diagrams, selection effects with magnitude, and RVs in DR3. The most extreme (>700km/s) and nearest (within 4kpc) 72 DR3 HVS candidates were investigated with respect to detected close neighbours, flags and astrometric quality parameters of objects of similar magnitudes in DR3. The quality checks involved HPM objects in a global comparison and all objects in the vicinity of each target. Spurious HPMs in the Galactic centre region led to false HVS interpretations in Gaia DR2 and are still present in DR3, although to a lesser extent. Otherwise there is good agreement between the HPMs of HVS candidates in DR2 and DR3. However, HVS candidates selected from DR2 tend to have larger parallaxes hence lower tangential velocities in DR3. Most DR3 RVs are much lower than the tangential velocities, indicating that the DR3 HVS candidates are still affected by underestimated parallaxes. None of the 72 extreme nearby DR3 HVS candidates, including three D stars, passed all quality checks. Their tangential velocities may turn out to be smaller, but at least some of them still appear unbound to the Galaxy. (abbreviated)

22 pages, 25 figures, accepted for publication in Astronomy and Astrophysics

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