Rupali Chandar (The University of Toledo), Bradley C. Whitmore (Space Telescope Science Institute), Hwihyun Kim (Arizona State University), Catherine Kaleida (Arizona State University), Max Mutchler (Space Telescope Science Institute), Daniela Calzetti (University of Massachusetts), Abhijit Saha (NOAO), Robert O'Connell (University of Virginia), Bruce Balick (University of Washington), Howard Bond (Space Telescope Science Institute), Marcella Carollo (Institute of Astronomy, ETH-Zurich), Michael Disney (Cardiff University), Michael A. Dopita (The Australian National University), Jay A. Frogel (AURA, Washington, DC), Donald Hall (Institute for Astronomy, Honolulu), Jon A. Holtzman (New Mexico State University), Randy A. Kimble (Goddard Space Flight Center), Patrick McCarthy (Carnegie Institute of Washington), Francesco Paresce (ESTEC, Noordwijk), Joe Silk (University of Oxford), John Trauger (NASA JPL), Alistair R. Walker (Cerro Tololo Inter-American Observatory), Rogier A. Windhorst (Arizona State University), Erick Young (NASA-Ames Research Center)
ArXiv #: 1007.5237 (PDF, PS, ADS, Papers, Other)
Comments: 36 pages, 13 figures, 1 table; accepted for publication in the Astrophysical Journal
The newly installed Wide Field Camera 3 (WFC3) on the Hubble Space Telescope has been used to obtain multi-band images of the nearby spiral galaxy M83. These new observations are the deepest and highest resolution images ever taken of a grand-design spiral, particularly in the near ultraviolet, and allow us to better differentiate compact star clusters from individual stars and to measure the luminosities of even faint clusters in the U band. We find that the luminosity function for clusters outside of the very crowded starburst nucleus can be approximated by a power law, dN/dL \propto L^{alpha}, with alpha = -2.04 +/- 0.08, down to M_V ~ -5.5. We test the sensitivity of the luminosity function to different selection techniques, filters, binning, and aperture correction determinations, and find that none of these contribute significantly to uncertainties in alpha. We estimate ages and masses for the clusters by comparing their measured UBVI,Halpha colors with predictions from single stellar population models. The age distribution of the clusters can be approximated by a power-law, dN/dt propto t^{gamma}, with gamma=-0.9 +/- 0.2, for M > few x 10^3 Msun and t < 4×10^8 yr. This indicates that clusters are disrupted quickly, with ~80-90% disrupted each decade in age over this time. The mass function of clusters over the same M-t range is a power law, dN/dM propto M^{beta}, with beta=-1.94 +/- 0.16, and does not have bends or show curvature at either high or low masses. Therefore, we do not find evidence for a physical upper mass limit, M_C, or for the earlier disruption of lower mass clusters when compared with higher mass clusters, i.e. mass-dependent disruption. We briefly discuss these implications for the formation and disruption of the clusters.
