Kinematics of Luminous Blue Variables in the Large Magellanic Cloud
  We study the kinematics of luminous blue variables (LBVs) in the Large
Magellanic Cloud (LMC). Using high-resolution spectra, we measure the systemic
radial velocities for a sample of 16 LBVs and LBV candidates. In order to
measure the net motion of LBVs compared to their local environments, we
subtract the projected line-of-sight velocity at the same location derived from
the rotation curve model of the LMC \citep{C22}. Using Bayesian inference, we
infer a velocity dispersion for LBVs of $40.96^{+9.61}_{-7.24}$ km s$^{-1}$. To
put LBVs in context with other evolved massive stars, we compare this to red
supergiants (RSGs) in the LMC, which have a significantly smaller velocity
dispersion of $16.48^{+0.41}_{-0.61}$ km s$^{-1}$. Moreover, 6 out of 16 LBVs
($\sim$38%) have radial velocities of more than 25 km s$^{-1}$, while only 9%
of RSG have such high velocities. This suggests that LBVs include more runaways
than the population of stars that evolves to become RSGs, indicating that LBVs
are preferentially kicked by a companion's supernova explosion as compared to
other evolved massive stars. Our investigation reveals other interesting clues
about LBVs in the LMC as well. We find that radial velocities and widths of
emission lines for each target remain constant over several epochs, whereas
measured absorption lines exhibit highly variable radial velocities for R110,
R81, S Dor, Sk-69$^\circ$142a, and Sk-69$^\circ$279. These five LBVs probably
have a binary companion. Additionally, we find that Sk-69$^\circ$142a
experienced its second outburst in 2019 September, shifting its status from
candidate to confirmed LBV.
