HII Region Luminosity Function of the Interacting Galaxy M51
  We present a study of HII regions in M51 using the Hubble Space Telescope ACS
images taken as part of the Hubble Heritage Program. We have catalogued about
19,600 HII regions in M51 with Ha luminosity in the range of L = 10^{35.5}
erg/s to 10^{39.0} erg/s. The Ha luminosity function of HII regions (HII LF) in
M51 is well represented by a double power law with its index alpha=-2.25\pm0.02
for the bright part and alpha=-1.42\pm0.01 for the faint part, separated at a
break point L= 10^{37.1} erg/s. This break was not found in previous studies of
M51 HII regions. Comparison with simulated HII LFs suggests that this break is
caused by the transition of HII region ionizing sources, from low mass clusters
(with ~ 10^3 M_sun, including several OB stars) to more massive clusters
(including several tens of OB stars). The HII LFs with L < 10^{37.1} erg/s are
found to have different slopes for different parts in M51: the HII LF for the
interarm region is steeper than those for the arm and the nuclear regions. This
observed difference in HII LFs can be explained by evolutionary effects that
HII regions in the interarm region are relatively older than those in the other
parts of M51.
