Hubble Space Telescope proper motions of Large Magellanic Cloud star clusters -- I. Catalogues and results for NGC 1850

TL;DR

This paper presents high-precision proper motion measurements for 23 Large Magellanic Cloud star clusters using HST data, enabling detailed kinematic analysis and catalogues for future research.

Contribution

It provides the first comprehensive proper motion catalogues for LMC clusters, demonstrating the potential of HST data for extragalactic stellar kinematics.

Findings

NGC 1850 has a distinct center-of-mass motion from surrounding stars.

Velocity dispersion of field stars is 0.128 mas/yr.

Centrally concentrated fast-rotating stars suggest radial segregation.

Abstract

We present proper motion (PM) measurements for a sample of 23 massive star clusters within the Large Magellanic Cloud using multi-epoch data from the Hubble Space Telescope (HST). We combined archival data from the ACS/WFC and WFC3/UVIS instruments with observations from a dedicated HST programme, resulting in time baselines between 4.7 and 18.2 yr available for PM determinations. For bright well-measured stars, we achieved nominal PM precisions of 55 $\mu$as/yr down to 11 $\mu$as/yr . To demonstrate the potential and limitations of our PM data set, we analysed the cluster NGC 1850 and showcase a selection of different science applications. The precision of the PM measurements allows us to disentangle the kinematics of the various stellar populations that are present in the HST field. The cluster has a centre-of-mass motion that is different from the surrounding old field stars and also differs from the mean motion of a close-by group of very young stars. We determined the velocity dispersion of field stars to be 0.128 +/- 0.003 mas/yr (corresponding to 30.3 +/- 0.7 km/s). The velocity dispersion of the cluster inferred from the PM data set most probably overestimates the true value, suggesting that the precision of the measurements at this stage is not sufficient for a reliable analysis of the internal kinematics of extra-galactic star clusters. Finally, we exploit the PM-cleaned catalogue of likely cluster members to determine any radial segregation between fast and slowly-rotating stars, finding that the former are more centrally concentrated. With this paper, we also release the astro-photometric catalogues for each cluster.