Radio Continuum and Recombination Line Study of Ultracompact H II Regions with Extended Envelopes
By Kee-Tae Kim, B. Koo. 2000
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We have carried out 21 cm radio continuum observations of 16 ultracompact H II regions using the VLA (DnC array) in a search for associated extended emission. We have also observed the H76α recombination line toward all the sources and the He76α line at the positions with strong H76α line emission. The UC H II regions have simple morphologies and large (≳10) ratios of single-dish to VLA fluxes. We detected extended emission toward all the sources. The extended emission consists of one to several compact (~1' or 0.5-5 pc) components and a diffuse extended (2'-12' or 4-19 pc) envelope. All the UC H II regions but two are located in the compact components, where the UC H II regions always correspond to their peaks. The compact components with UC H II regions are usually smaller and denser than those without UC H II regions. For individual sources, we derive the spectral types (O7-O4) of the ionizing stars and the fractions of UV photons absorbed by dust within the nebulae, which are significantly different from previous estimates based on the UC H II regions alone. Our recombination line observations show that the ultracompact, compact, and extended components have approximately the same velocity in the individual sources with one exception (G25.72+0.05), implying that they are physically associated. The compact components in each object appear to be ionized by separate sources, while the UC H II regions and their associated compact components are likely to be ionized by the same sources on the basis of the morphological relations mentioned above. This suggests that almost all of the observed UC H II regions are not "real" UC H II regions but ultracompact cores of more extended H II regions, and that their actual ages are much greater than their dynamical age (≲104 yr). We find that most of simple UC H II regions previously known have large ratios of single-dish to VLA fluxes, similar to our sources. Therefore, the "age problem" of UC H II regions does not seem to be as serious as earlier studies argued. We present a simple model in which the coexistence of the ultracompact, compact, and extended components for a long (>105 yr) time is easily explained by combining the champagne flow model with the hierarchical structure of massive star-forming regions. The well-known relation between the density and diameter of H II regions, ne ∝ D-1, is a natural consequence of the hierarchical structure according to our model. We discuss some individual sources.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/e93ce22686556e874053c45918be3a656af69ea5
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Citations in the corpus
- Ultra-Compact HII Regions and Massive Star Formation (2002, methodology): “The Kim & Koo (2001) relation is shown in Figure 11.”
- SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements (2016, background): “Our reconstructed PSF is about 2.5” FWHM (2” covers 1 kpc at z=0.025) while the size of a typical H ii region is a few to hundreds of pc (Kennicutt 1984; Garay & Lizano 1999; Kim & Koo 2001; Hunt & Hirashita 2009).”
- H II REGIONS: WITNESSES TO MASSIVE STAR FORMATION (2010, background): “When the gas reservoir around the two most massive stars is exhausted, their H ii regions merge into a compact H ii region similar to the extended envelopes often observed around ultracompact H ii regions (Kim & Koo 2001; Kurtz et al. 1999).”
- THEORETICAL EVOLUTION OF OPTICAL STRONG LINES ACROSS COSMIC TIME (2013, background): “Ultracompact H II regions in the Milky Way contain a porous interstellar medium (Kurtz et al. 1999; Kim & Koo 2001).”