Evidence for temporal evolution in the M33 disc as traced by its star clusters

TL;DR

This study analyzes star clusters in M33, revealing their age-metallicity relation, disc membership, and evidence of temporal evolution in the galaxy's metallicity gradient, along with insights into cluster kinematics and composition.

Contribution

It provides the first detailed evidence of temporal evolution in M33's disc metallicity gradient using a large sample of star clusters spanning a wide age range.

Findings

Younger clusters are more metal-rich and associated with the disc.

The metallicity gradient in M33's disc has evolved over time.

Cluster velocity dispersions increase with age, indicating disc heating.

Abstract

We present precision radial velocities and stellar population parameters for 77 star clusters in the Local Group galaxy M33. Our GTC and WHT observations sample both young, massive clusters and known/candidate globular clusters, spanning ages ~ 10^6 - 10^10 yr, and metallicities, [M/H] ~-1.7 to solar. The cluster system exhibits an age-metallicity relation; the youngest clusters are the most metal-rich. When compared to HI data, clusters with [M/H] ~ -1.0 and younger than ~ 4 Gyr are clearly identified as a disc population. The clusters show evidence for strong time evolution in the disc radial metallicity gradient (d[M/H]dt / dR = 0.03 dex/kpc/Gyr). The oldest clusters have stronger, more negative gradients than the youngest clusters in M33. The clusters also show a clear age-velocity dispersion relation. The line of sight velocity dispersions of the clusters increases with age similar to Milky Way open clusters and stars. The general shape of the relation is reproduced by disc heating simulations, and the similarity between the relations in M33 and the Milky Way suggests that heating by substructure, and cooling of the ISM both play a role in shaping this relation. We identify 12 "classical" GCs, six of which are newly identified GC candidates. The GCs are more metal-rich than Milky Way halo clusters, and show weak rotation. The inner (R < 4.5 kpc) GCs exhibit a steep radial metallicity gradient (d[M/H]/dR = -0.29+-0.11 dex/kpc) and an exponential-like surface density profile. We argue that these inner GCs are thick disc rather than halo objects.