HII Region Luminosity Function of the Interacting Galaxy M51

TL;DR

This study analyzes the luminosity distribution of over 19,600 HII regions in M51, revealing a double power law with a break point linked to the transition of ionizing sources from low to high mass clusters, and regional differences suggest evolutionary effects.

Contribution

First detailed HII luminosity function of M51 revealing a double power law with a novel break point linked to cluster mass transition.

Findings

HII LF is a double power law with a break at 10^{37.1} erg/s.

Break point indicates transition from low to high mass ionizing clusters.

Interarm HII regions have steeper LFs, suggesting older ages.

Abstract

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.