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Galactic, young massive star clusters are approximately coeval aggregates ofstars, close enough to resolve the individual stars, massive enough to haveproduced large numbers of massive stars, and young enough for these stars to bein a pre-supernova state. As such these objects represent powerful naturallaboratories in which to study the evolution of massive stars. To be used inthis way, it is crucial that accurate and precise distances are known, sincethis affects both the inferred luminosities of the cluster members and the ageestimate for the cluster itself. Here we present distance estimates for threestar clusters rich in Red Supergiants ($\chi$ Per, NGC 7419 and Westerlund 1)based on their average astrometric parallaxes $\bar{\pi}$ in Gaia Data Release2, where the measurement of $\bar{\pi}$ is obtained from a proper-motionscreened sample of spectroscopically-confirmed cluster members. We determinedistances of $d=2.25^{+0.16}_{-0.14}$kpc, $d=3.00^{+0.35}_{-0.29}$kpc, and$d=3.87^{+0.95}_{-0.64}$kpc for the three clusters respectively. We find thatthe dominant source of error is that in Gaia's zero-point parallax offset$\pi_{\rm ZP}$, and we argue that more precise distances cannot be determinedwithout an improved characterization of this quantity.

The distances to star-clusters hosting Red Supergiants: $\chi$ Per, NGC 7419, and Westerlund 1