2007AJ....134..447S

We present a new catalog of star cluster candidates in the nearby spiral galaxy M33. It is based on eight existing catalogs wherein we have cross-referenced identifications and endeavored to resolve inconsistencies between them. Our catalog contains 451 candidates, of which 255 are confirmed clusters based on Hubble Space Telescope and high-resolution ground-based imaging. The catalog contains precise cluster positions (right ascension and declination), magnitudes and colors in the UBVRIJHK_S filters, metallicities, radial velocities, masses and ages, where available, and galactocentric distances for each cluster. The color distribution of the M33 clusters appears to be similar to those in the Large Magellanic Cloud, with major peaks at (B-V)₀∼0.15 and (B-V)₀∼0.65. The intrinsic colors are correlated with cluster ages, which range from 10^7.5 to 10^10.3 yr. The age distribution of the star clusters supports the notion of rapid cluster disruption with a slope of α=-1.09±0.07 in the dN_clus/dτ∝τ^α relation. In addition, comparison to theoretical single stellar population models suggests the presence of an age-metallicity relation among these clusters, with younger clusters being more metal-rich. Analysis of the radial distribution of the clusters yields some evidence that younger clusters (age ≲1 Gyr) may be more concentrated toward the center of M33 than older ones. A similar comparison with the radial profile of the M33 field stars shows the clusters to be more centrally concentrated at the greater than 99.9% confidence level. Possible reasons for this are presented and discussed; however, the overwhelming conclusion seems to be that a more complete and thorough cluster search is needed, covering at least 4 deg² centered on M33.