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Authordc.contributor.authorMeidt, Sharon 
Authordc.contributor.authorGlover, Simon C.O. 
Authordc.contributor.authorDiederik Kruijssen, J. M. 
Authordc.contributor.authorLeroy, Adam K. 
Authordc.contributor.authorRosolowsky, Erik 
Authordc.contributor.authorSchruba, Andreas 
Authordc.contributor.authorHughes, Annie 
Authordc.contributor.authorSchinnerer, Eva 
Authordc.contributor.authorUsero, Antonio 
Authordc.contributor.authorBigiel, Frank 
Authordc.contributor.authorBlanc, Guillermo 
Authordc.contributor.authorChevance, Mélanie 
Authordc.contributor.authorPety, Jerome 
Authordc.contributor.authorQuerejeta, Miguel 
Authordc.contributor.authorUtomo, Dyas 
Cita de ítemdc.identifier.citationAstrophysical Journal (APR 2020) 89(2) 73es_ES
Abstractdc.description.abstractIn Meidt et al., we showed that gas kinematics on the scale of individual molecular clouds are not entirely dominated by self-gravity but also track a component that originates with orbital motion in the potential of the host galaxy. This agrees with observed cloud line widths, which show systematic variations from virial motions with environment, pointing at the influence of the galaxy potential. In this paper, we hypothesize that these motions act to slow down the collapse of gas and so help regulate star formation. Extending the results of Meidt et al., we derive a dynamical collapse timescale that approaches the free-fall time only once the gas has fully decoupled from the galactic potential. Using this timescale, we make predictions for how the fraction of free-falling, strongly self-gravitating gas varies throughout the disks of star-forming galaxies. We also use this collapse timescale to predict variations in the molecular gas star formation efficiency, which is lowered from a maximum, feedback-regulated level in the presence of strong coupling to the galactic potential. Our model implies that gas can only decouple from the galaxy to collapse and efficiently form stars deep within clouds. We show that this naturally explains the observed drop in star formation rate per unit gas mass in the Milky Way's Central Molecular Zone and other galaxy centers. The model for a galactic bottleneck to star formation also agrees well with resolved observations of dense gas and star formation in galaxy disks and the properties of local clouds.es_ES
Patrocinadordc.description.sponsorshipGerman Research Foundation (DFG): SCHI 536/7-2, SPP 1573. German Research Foundation (DFG): 138713538-SFB 881. Heidelberg cluster of excellence - German Excellence Strategy: EXC 2181-390900948. German Research Foundation (DFG): KR4801/1-1. German Research Foundation (DFG): KR4801/2-1. European Research Council (ERC): 714907. National Science Foundation (NSF): 1615105, 1615109, 1653300. Natural Sciences and Engineering Research Council of Canada: RGPIN-2017-03987. European Research Council (ERC): 694343. Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU. INC/INP - CEA. Centre National D'etudes Spatiales. Programme National Cosmology and Galaxies (PNCG) of CNRS/INSU. INP. IN2P3. French Atomic Energy Commission. Programme National Cosmology et Galaxies (PNCG) of CNRS/INSU. European Union's Horizon 2020 research and innovation programme: 726384-EMPIRE. Spanish funding grants: AYA2016-79006-P, PGC2018-094671-B-I00.es_ES
Publisherdc.publisherIOP Publishinges_ES
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 Chile*
Link to Licensedc.rights.uri*
Sourcedc.sourceAstrophysical Journales_ES
Keywordsdc.subjectStar formationes_ES
Keywordsdc.subjectInterstellar mediumes_ES
Títulodc.titleA model for the onset of self-gravitation and star formation in molecular gas governed by galactic forces. II. The bottleneck to collapse set by cloud-environment decouplinges_ES
Document typedc.typeArtículo de revistaes_ES
dcterms.accessRightsdcterms.accessRightsAcceso Abierto
Indexationuchile.indexArtículo de publicación ISIes_ES

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