Ages and Masses of Star Clusters in M33: a Multi-wavelength Study
  We combine archival images for the nearby galaxy M33 (Triangulum Galaxy) from
the ultraviolet (UV) to the infrared (IR) to derive ages, masses, and
extinctions for the young star cluster population, and compare our physical
parameters with published ones. Our goal is to test the robustness of clusters'
ages and masses, and possibly improve on existing ones both by expanding the
wavelength range of the spectral energy distribution (SED) fits and by using
more recent population synthesis models. The rationale for this experiment is
to verify the sensitivity of the clusters' physical parameters to observational
setups and model choices that span those commonly found in the literature. We
derive the physical parameters of 137 clusters, using SEDs measured in eight
UV-to-I bands, including H-alpha, from GALEX and ground-based images. We also
add the 24 micron image from the Spitzer Space Telescope to help break some age
degeneracies. We find that our derived cluster ages show significant
differences with earlier determinations, while the masses remain relatively
insensitive to the fitting approach adopted. We also highlight an already known
difficulty in recovering old, low-extinction clusters, as SED fitting codes
tend to prefer younger, higher extinction solutions when the extinction is a
free parameter. We publish updated ages, masses, and extinctions, with
uncertainties, for all sample star clusters, together with their photometry;
given the proximity of M33, this represents an important population to secure
for the study of star formation and cluster evolution in spirals.
