The physical structure of Magellanic Cloud HII regions
نویسندگان
چکیده
منابع مشابه
Letter to the Editor Compact HII regions in the Large Magellanic Cloud observed by ISO
We present ISOCAM observations of five fields in the Large Magellanic Cloud centered on IRAS point sources with colors of ultracompact HII regions. Three bright sources of parsec or subparsec size, with luminosities consistent with being embedded O stars, are detected at 15 μm in two fields belonging to the HII region N 159. Using published high resolution radio observations, it is found that t...
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We study the formation and evolution of Hii regions around the first stars formed at redshifts z = 10 − 30. We use a one-dimensional Lagrangian hydrodynamics code which self-consistently incorporates radiative transfer and non-equilibrium primordial gas chemistry. The star-forming region is defined as a spherical dense molecular gas cloud with a Population III star embedded at the center. We ex...
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We derive structural parameters and evidence for extended tidal debris from star count and preliminary standard candle analyses of the Large Magellanic Cloud based on Two Micron All Sky Survey (2MASS) data. The full-sky coverage and low extinction in Ks presents an ideal sample for structural analysis of the LMC. The star count surface densities and deprojected inclination for both young and ol...
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The projected distribution of stars in the Small Magellanic Cloud (SMC) from the Magellanic Clouds Photometric Survey is analysed. Stars of different ages are selected via criteria based on V magnitude and V − I colour, and the degree of ‘grouping’ as a function of age is studied. We quantify the degree of structure using the two-point correlation function and a method based on the Minimum Span...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2002
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361:20020864