Brooke P. Skelton

The Hii Regions of M33. II. A Photometric Catalog of 1272 Newly Identified Emission Regions

We have identified a total of 1272 newly recognized emission regions in M33. Combined with the previously cataloged total of 1066 H ii regions and supernova remnants, this brings M33s total to 2338 emission regions. This paper provides photometry of the new objects in Hα, which is combined with data from previous catalogs to produce a global H ii region luminosity function (corrected for incompleteness) that reaches a faint luminosity limit of 2 × 1034 ergs s–1 and shows a broad maximum with a peak frequency at luminosities of 6 × 1035^{35} ergs s–1. We also plot the H ii region size distribution and comment on unusual morphologies.

THE LUMINOSITY FUNCTION AND SIZE DISTRIBUTION OF THE H II REGIONS IN M33

We present Hα fluxes and sizes for most of the H 2 regions in M33 listed in the catalog of Courtes et al. (1987). The observed bright end of the differential luminosity function is approximately a power law with exponent a = -2.40 ± 0.15, while the number counts turn over at an Hα luminosity of approximately 1036.4 erg s-1. After accounting for the effects of incompleteness in our sample, we find that the faint end of the corrected luminosity function remains almost constant instead of turning over. The cumulative size distribution approximately follows an exponential law with scale size D0 = 32 ± 1 pc. We briefly discuss the implications of our results for our understanding of recent high-mass star formation in M3.

Emission-Line Properties of the Large Magellanic Cloud Bubble N70

We present a spectrophotometric imaging study of the emission bubble N70 (DEM 301) in the Large Magellanic Cloud. N70 is approximately 100 pc in size with a nearly circular shell-like morphology. The nebular emission is powered by an uncertain combination of EUV photons, intense winds, and supernova shock waves from the central population of high-mass stars (the OB association LH 114). We have obtained narrowband images (FWHM ~ 6 A) of N70 in the light of Hα λ6563, [N ii] λ6584, [S ii] λλ6717, 6731, and [O iii] λ5007, along with the corresponding red and green continua. The resulting line fluxes and flux ratios are used to derive ionization rates, nebular densities, volume filling fractions, and excitation indices. The photoionizing luminosity inferred from the embedded stellar population is more than adequate to account for the observed hydrogen ionization rate.We compare the emission-line photometry with that derived from similar imaging of the Orion Nebula and with data collected from the literature on other emission-line regions in the LMC. Compared with the Orion Nebula, N70 shows much higher [S ii]/Hα intensity ratios that increase smoothly with radius—from less than 0.3 near the center to greater than 1.0 toward the outer filamentary shell. The measured intensity ratios in N70 more closely match the range of excitation spanned by giant and supergiant H ii shells and by some of the supernova remnants observed in the LMC. The contending ionization and excitation processes in the interior and outer shell of N70 are evaluated in terms of the available data. EUV photons probably contribute most of the inner nebulas ionization, whereas a combination of photoionization plus collisional ionization and excitation of sulfur atoms by low-velocity shocks seems to best fit the emission-line luminosities and intensity ratios observed in the outer shell. Considerations of the radiative and mechanical energetics that are involved may indicate the need for one or two supernova explosions having occurred during the last ~Myr.