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Authordc.contributor.authorLeroy, Adam 
Authordc.contributor.authorHughes, Annie 
Authordc.contributor.authorSchruba, Andreas 
Authordc.contributor.authorRosolowsky, Erik 
Authordc.contributor.authorBlanc Mendiberri, Guillermo 
Authordc.contributor.authorBolatto, Alberto 
Authordc.contributor.authorColombo, Dario 
Authordc.contributor.authorEscala Astorquiza, Andrés 
Authordc.contributor.authorKramer, Carsten 
Authordc.contributor.authorDiederik Kruijssen, J. M. 
Cita de ítemdc.identifier.citationThe Astrophysical Journal, 831:16 (33pp), 2016 November 1es_ES
Abstractdc.description.abstractThe cloud-scale density, velocity dispersion, and gravitational boundedness of the interstellar medium (ISM) vary within and among galaxies. In turbulent models, these properties play key roles in the ability of gas to form stars. New high-fidelity, high-resolution surveys offer the prospect to measure these quantities across galaxies. We present a simple approach to make such measurements and to test hypotheses that link small-scale gas structure to star formation and galactic environment. Our calculations capture the key physics of the Larson scaling relations, and we show good correspondence between our approach and a traditional "cloud properties" treatment. However, we argue that our method is preferable in many cases because of its simple, reproducible characterization of all emission. Using, low-J 12CO data from recent surveys, we characterize the molecular ISM at 60 pc resolution in the Antennae, the Large Magellanic Cloud (LMC), M31, M33, M51, and M74. We report the distributions of surface density, velocity dispersion, and gravitational boundedness at 60 pc scales and show galaxy-to-galaxy and intragalaxy variations in each. The distribution of flux as a function of surface density appears roughly lognormal with a 1σ width of ~0.3 dex, though the center of this distribution varies from galaxy to galaxy. The 60 pc resolution line width and molecular gas surface density correlate well, which is a fundamental behavior expected for virialized or free-falling gas. Varying the measurement scale for the LMC and M31, we show that the molecular ISM has higher surface densities, lower line widths, and more self-gravity at smaller scales.es_ES
Publisherdc.publisherThe American Astronomical Societyes_ES
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 Chile*
Link to Licensedc.rights.uri*
Sourcedc.sourceThe Astrophysical Journales_ES
Keywordsdc.subjectgalaxies: ISMes_ES
Keywordsdc.subjectgalaxies: star formationes_ES
Keywordsdc.subjectISM: cloudses_ES
Keywordsdc.subjectISM: moleculeses_ES
Keywordsdc.subjectISM: structurees_ES
Area Temáticadc.subject.otherAstronomíaes_ES
Títulodc.titleA portrait of cold gas in galaxies at 60 pc resolution and a simple method to test hypotheses that link small-scale ism structure to galaxy-scale processeses_ES
Document typedc.typeArtículo de revistaes_ES
Indexationuchile.indexArtículo de publicación ISIes_ES

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Attribution-NonCommercial-NoDerivs 3.0 Chile
Except where otherwise noted, this item's license is described as Attribution-NonCommercial-NoDerivs 3.0 Chile