The Pa{\alpha} Luminosity Function of HII Regions in Nearby Galaxies from HST/NICMOS

TL;DR

This study uses high-resolution space-based Paα imaging to analyze the luminosity function of HII regions in nearby galaxies, revealing a single power-law distribution that aligns with star cluster mass functions, overcoming ground-based limitations.

Contribution

First space-based analysis of HII region luminosity functions in multiple galaxies using Paα, providing more accurate, extinction-free measurements and challenging previous broken power-law findings.

Findings

HII region luminosity functions follow a single power law L^-1

Size distribution roughly D^-3, but affected by blending

Results align with star cluster mass functions and previous HST studies

Abstract

The HII region luminosity function (LF) is an important tool for deriving the birthrates and mass distribution of OB associations, and is an excellent tracer of the newly formed massive stars and associations. To date, extensive work (predominantly in H{\alpha}) has been done from the ground, which is hindered by dust extinction and the severe blending of adjacent (spatially or in projection) HII regions. Reliably measuring the properties of HII regions requires a linear resolution <40 pc, but analyses satisfying this requirement have been done only in a handful of galaxies, so far. As the first space-based work using a galaxy sample, we have selected 12 galaxies from our HST NICMOS Pa{\alpha} survey and studied the luminosity function and size distribution of HII regions both in individual galaxies and cumulatively, using a virtually extinction-free tracer of the ionizing photon rate. The high angular resolution and low sensitivity to diffuse emission of NICMOS also offer an advantage over ground-based imaging by enabling a higher degree of de-blending of the HII regions. We do not confirm the broken power-law LFs found in ground-based studies. Instead, we find that the LFs, both individual and co-added, follow a single power law dN(L)/dlnL ~ L^-1, consistent with the mass function of star clusters in nearby galaxies, and in agreement with the results of the existing analyses with HST data. The individual and co-added size distribution of HII regions are both roughly consistent with dN(D)/dlnD ~ D^-3, but the power-law scaling is probably contaminated by blended regions or complexes.