|Authors||R. de Grijs 1, U. Fritze-v. Alvensleben 2, P. Anders 2, J.S. Gallagher III 3, N. Bastian 4, V.A. Taylor 5, R.A. Windhorst 5|
|Affiliation||1 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK|
2 Universitätssternwarte, University of Göttingen, Geismarlandstr. 11, 37083 Göttingen, Germany,
3 Astronomy Department, University of Wisconsin-Madison, 475 N. Charter St., Madison, WI 53706, USA,
4 Astronomical Institute, Utrecht University, Princetonplein 5, 3584 CC Utrecht, The Netherlands,
5 Department of Physics & Astronomy, Arizona State University, Box 871504, Tempe, AZ 85287-1504, USA
|Accepted by||Monthly Notices of the Royal Astronomical Society|
We simultaneously obtain ages, metallicities and extinction values for ~ 300 clusters in the nearby starburst galaxy NGC 3310, based on archival Hubble Space Telescope observations from the ultraviolet (UV) to the near-infrared (NIR). We show that, for ages 6 < log(age/yr) < 9, and if one can only obtain partial coverage of the spectral energy distribution (SED), an optical passband combination of at least four filters including both blue and red passbands results in the most representative age distribution, as compared to the better constrained ages obtained from the full UV-NIR SED coverage. We find that while blue-selected passband combinations lead to age distributions that are slightly biased towards younger ages due to the well-known age-metallicity degeneracy, red-dominated passband combinations should be avoided.
NGC 3310 underwent a (possibly extended) global burst of cluster formation ~ 3 x 107 yr ago. This coincides closely with the last tidal interaction or merger with a low-metallicity galaxy that likely induced the formation of the large fraction of clusters with (significantly) subsolar metallicities. The logarithmic slope of the V-band cluster luminosity function, for clusters in the range 17.7 < F606W < 20.2 mag, is alphaF606W ~ -1.8 ± 0.4. The observed cluster system has a median mass of < log(m/Mo) > ~ 5.25 ± 0.1, obtained from scaling the appropriate model SEDs for known masses to the observed cluster SEDs.