SCYON Abstract

Received on May 30 2007

ACS imaging of star clusters in M51. I. Identification and radius distribution

Authors	R.A. Scheepmaker (¹), M.R. Haas (^1,2), M. Gieles (¹), N. Bastian (³), S.S. Larsen (¹), and H.J.G.L.M. Lamers (¹)
Affiliation	(¹) Astronomical Institute, Utrecht University, The Netherlands (²) Leiden Observatory, Leiden University, The Netherlands (³) Department of Physics and Astronomy, University College London, United Kingdom
Accepted by	Astronomy & Astrophysics
Contact	scheepmaker@astro.uu.nl
URL	http://xxx.lanl.gov/abs/0704.3604
Links

Abstract

We use HST/ACS observations of the spiral galaxy M51 in F435W, F555W and F814W to select a large sample of star clusters with accurate effective radius measurements in an area covering the complete disc of M51. We present the dataset and study the radius distribution and relations between radius, colour, arm/interarm region, galactocentric distance, mass and age. We select a sample of 7698 (F435W), 6846 (F555W) and 5024 (F814W) slightly resolved clusters and derive their effective radii (R_eff) by fitting the spatial profiles with analytical models convolved with the point spread function. The radii of 1284 clusters are studied in detail. We find cluster radii between 0.5 and ~ 10pc, and one exceptionally large cluster candidate with R_eff = 21.6pc. The median R_eff is 2.1pc. We find 70 clusters in our sample which have colours consistent with being old GC candidates and we find 6 new "faint fuzzy" clusters in, or projected onto, the disc of M51. The radius distribution can not be fitted with a power law similar to the one for star-forming clouds. We find an increase in R_eff with colour as well as a higher fraction of clusters with B - V >~ 0.05 in the interarm regions. We find a correlation between R_eff and galactocentric distance (R_G) of the form R_eff ∝ R_G^0.12±0.02, which is considerably weaker than the observed correlation for old Milky Way GCs. We find weak relations between cluster luminosity and radius: R_eff ∝ L^0.15±0.02 for the interarm regions and R_eff ∝ L^-0.11±0.01 for the spiral arm regions, but we do not observe a correlation between cluster mass and radius. The observed radius distribution indicates that shortly after the formation of the clusters from a fractal gas, the radii of the clusters have changed in a non-uniform way. We find tentative evidence suggesting that clusters in spiral arms are more compact.