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Far Outer Galaxy H II Regions

1996; IOP Publishing; Volume: 458; Linguagem: Inglês

10.1086/176847

1538-4357

Alexander Rudolph, J. Brand, E. J. De Geus, J. G. A. Wouterloot,

Astronomy and Astrophysical Research

view Abstract Citations (45) References (46) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Far Outer Galaxy H II Regions Rudolph, Alexander L. ; Brand, Jan ; de Geus, Eugene J. ; Wouterloot, Jan G. A. Abstract We have made a multiwavelength (6, 3.6, and 2 cm), high-resolution (3"-6") radio continuum survey of IRA S-selected sources to search for and study H II regions in the far-outer Galaxy. We identified 31 sources with R ≳ 15 kpc and LFlR ≳ 104 Lsun, indicating the presence of high-mass star formation. We have observed 11 of these sources with the Very Large Array (VLA). The 6 and 2 cm observations were made using "scaled arrays," making possible a direct and reliable determination of spectral indices. Of the 39 sources we detected at 6 cm, 10 have spectral indices consistent with optically thin free-free emission from H II regions and are within 45" of the associated IRAS source. Combining our data with previous VLA observations by other investigators we analyzed a sample of 15 of the most remote H II regions found in our Galaxy, located at R = 15-18.2 kpc. The sizes of the H II regions range from ≲ 0.10 to 2.3 pc. Using the measured flux densities and sizes, we determined their electron densities, emission measures, and excitation parameters, as well as their Lyman continuum fluxes needed to keep the nebulae ionized. The sizes and electron densities indicate that most of the sources are (ultra)compact H II regions. Seven of the 15 H II regions have sizes ≲ 0.20 pc. The large number of compact H II regions suggests that the time these regions spend in a compact phase must be much longer than their dynamical expansion times. Five of the 15 H II regions have cometary shapes; the remainder are spherical or unresolved. Comparison of our data with molecular line maps suggests that the cometary shape of the two H II regions in S127 may be due to pressure confinement of the expanding ionized gas, as in the "blister" or "champagne flow" models of H II regions. Comparison of our data with the IRAS data indicates that the five most luminous H II regions are consistent with a single zero-age main sequence 0 or B star exciting a dust-free H II region. Publication: The Astrophysical Journal Pub Date: February 1996 DOI: 10.1086/176847 Bibcode: 1996ApJ...458..653R Keywords: ISM: H II REGIONS; ISM: INDIVIDUAL ALPHANUMERIC: S127; RADIO CONTINUUM: ISM; SURVEYS full text sources ADS | data products SIMBAD (22)