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EXTRAGALACTIC MOLECULAR CLOUDS [PDF]
, 2007 We report the results of our study of 436 giant molecular clouds (GMCs) in NGC5128 using dust extinction. The proposed technique allows us toprobe the extinction up to 10 magnitudes in this galaxy. The clump massspectrum, derived by a clumpfind algorithm, is consistent with a powerlaw, dN/dM ∞ M -α, with α = 2.3.
Yuri Beletsky, João Alves
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Science, 1986
The interstellar medium in our galaxy contains matter in a variety of states ranging from hot plasma to cold and dusty molecular gas. The molecular phase consists of giant clouds, which are the largest gravitationally bound objects in the galaxy, the primary reservoir of material for the ongoing birth of new stars, and the medium regulating the ...
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The interstellar medium in our galaxy contains matter in a variety of states ranging from hot plasma to cold and dusty molecular gas. The molecular phase consists of giant clouds, which are the largest gravitationally bound objects in the galaxy, the primary reservoir of material for the ongoing birth of new stars, and the medium regulating the ...
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Magnetic Fields in Molecular Clouds
Annual Review of Astronomy and Astrophysics, 2007This review examines observations of magnetic fields in molecular clouds and what those observations tell us about the theory of molecular cloud evolution and star formation. First, the review briefly summarizes classes of theoretical models of molecular clouds and specific predictions of the models that can be tested by observation.
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The Composition of Interstellar Molecular Clouds
1999We consider four-aspects of interstellar chemistry for comparison with comets: molecular abundances in general, relative abundances of isomers (specifically, HCN and HNC), ortho/para ratios for molecules, and isotopic fractionation, particularly for the ratio hydrogen/deuterium.
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Astrophysics and Space Science, 2004
Theoretical models of star formation from the collapse of molecular cloud cores have been evolving in complexity for many years. This work describes the evolution of models from the nonrotating, nonmagnetized singular isothermal sphere to rotating, magnetized singular isothermal toroids. Four members of the same family are studied–the four combinations
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Theoretical models of star formation from the collapse of molecular cloud cores have been evolving in complexity for many years. This work describes the evolution of models from the nonrotating, nonmagnetized singular isothermal sphere to rotating, magnetized singular isothermal toroids. Four members of the same family are studied–the four combinations
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2017
This chapter discusses the Taurus molecular cloud. Sources are extracted from the SCUBA-2 850-\(\upmu \)m data, Herschel 250-\(\upmu \)m data, and Herschel 250-\(\upmu \)m data filtered to match the spatial scales detectable with SCUBA-2.
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This chapter discusses the Taurus molecular cloud. Sources are extracted from the SCUBA-2 850-\(\upmu \)m data, Herschel 250-\(\upmu \)m data, and Herschel 250-\(\upmu \)m data filtered to match the spatial scales detectable with SCUBA-2.
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2012
Of specific interest for stellar formation are regions where matter in the ISM appears most dense and in the form of clouds. Although there is no particular definition of the term cloud, it describes regions with a density larger than about 10 to 30 atoms per cm3. There are diffuse clouds, which do not reach these densities, and self-gravitating clouds
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Of specific interest for stellar formation are regions where matter in the ISM appears most dense and in the form of clouds. Although there is no particular definition of the term cloud, it describes regions with a density larger than about 10 to 30 atoms per cm3. There are diffuse clouds, which do not reach these densities, and self-gravitating clouds
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Properties of molecular clouds in the magellanic clouds
2008Guido Garay, Monica Rubio
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