Comparing hypervelocity star populations from the Large Magellanic Cloud and the Milky Way

TL;DR

This study predicts and compares hyper-velocity star populations ejected from the Milky Way and Large Magellanic Cloud, highlighting differences in their distributions and potential observability in future surveys like Gaia and LSST.

Contribution

It introduces a model for hyper-velocity star ejections from both galaxies and predicts their observable properties and distributions in upcoming survey data.

Findings

LMC HVSs outnumber MW HVSs by a factor of ~2.5 in deep surveys.

Estimated detectable HVSs: ~125 from LMC and ~50 from MW in future data releases.

Distinct kinematic and spatial distributions for LMC and MW HVSs.

Abstract

We predict and compare the distributions and properties of hyper-velocity stars (HVSs) ejected from the centres of the Milky Way (MW) and the Large Magellanic Cloud (LMC). In our model, HVSs are ejected at a constant rate -- equal in both galaxies -- via the Hills mechanism and are propagated in a combined potential, where the LMC orbits the MW on its first infall. By selecting $m>2\, \mathrm{M_\odot}$ HVSs well-separated from the Magellanic Clouds and Galactic midplane, we identify mock HVSs which would stand out from ordinary stars in the stellar halo in future data releases from the Gaia satellite and the Vera C. Rubin Observatory's Legacy Survey of Space and Time (LSST). We find that in these deep surveys, LMC HVSs will outnumber MW ones by a factor $\sim 2.5$, as HVSs can more easily escape from the shallower potential of the LMC. At an assumed HVS ejection rate of $10^{-4} \, \mathrm{yr^{-1}}$, HVSs detectable in the final Gaia data release and LSST from the LMC (MW) will number $125_{-12}^{+11}$ ($50_{-8}^{+7}$) and $140_{-11}^{+10}$ ($42_{-7}^{+6}$), respectively. The MW and LMC HVS populations show different kinematics and spatial distributions. While LMC HVSs have more modest total velocities and larger Galactocentric distances clustered around those of the LMC itself, HVSs from the MW show broader distributions, including a prominent high-velocity tail above $500 \, \mathrm{km \ s^{-1}}$ that contains at least half of the stars. These predictions are robust against reasonable variation of the Galactic potential and of the LMC central black hole mass.