Show simple item record

Authordc.contributor.authorSanhueza, Patricio 
Authordc.contributor.authorJackson, James 
Authordc.contributor.authorZhang, Qizhou 
Authordc.contributor.authorGuzmán Fernández, Andrés 
Authordc.contributor.authorLu, Xing 
Authordc.contributor.authorStephens, Ian W. 
Authordc.contributor.authorWang, Ke 
Authordc.contributor.authorTatematsu, Ken'ichi 
Admission datedc.date.accessioned2018-03-21T14:24:02Z
Available datedc.date.available2018-03-21T14:24:02Z
Publication datedc.date.issued2017-06-01
Cita de ítemdc.identifier.citationThe Astrophysical Journal, 841:97 (14pp), 2017 June 1es_ES
Identifierdc.identifier.other10.3847/1538-4357/aa6ff8
Identifierdc.identifier.urihttps://repositorio.uchile.cl/handle/2250/146932
Abstractdc.description.abstractThe infrared dark cloud (IRDC) G028.23-00.19 hosts a massive (1500M(circle dot)), cold (12 K), and 3.6-70 mu m IR dark clump (MM1) that has the potential to form high-mass stars. We observed this prestellar clump candidate with the Submillimeter Array (similar to 3 ''.5 resolution) and Jansky Very Large Array (similar to 2 ''.1 resolution) in order to characterize the early stages of high-mass star formation and to constrain theoretical models. Dust emission at 1.3 mm wavelength reveals five cores with masses <= 15Me(circle dot). None of the cores currently have the mass reservoir to form a high-mass star in the prestellar phase. If the MM1 clump will ultimately form high-mass stars, its embedded cores must gather a significant amount of additional mass over time. No molecular outflows are detected in the CO (2-1) and SiO (5-4) transitions, suggesting that the SMA cores are starless. By using the NH3 (1, 1) line, the velocity dispersion of the gas is determined to be transonic or mildly supersonic (Delta V-nt/Delta V-th similar to 1.1-1.8). The cores are not highly supersonic as some theories of high-mass star formation predict. The embedded cores are four to seven times more massive than the clump thermal Jeans mass and the most massive core (SMA1) is nine times less massive than the clump turbulent Jeans mass. These values indicate that neither thermal pressure nor turbulent pressure dominates the fragmentation of MM1. The low virial parameters of the cores (0.1-0.5) suggest that they are not in virial equilibrium, unless strong magnetic fields of similar to 1-2 mG are present. We discuss high-mass star formation scenarios in a context based on IRDC G028.23-00.19, a study case believed to represent the initial fragmentation of molecular clouds that will form high-mass stars.es_ES
Patrocinadordc.description.sponsorshipGerman Research Foundation (DFG) WA3628-1/1es_ES
Lenguagedc.language.isoenes_ES
Publisherdc.publisherIOP Publishinges_ES
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 Chile*
Link to Licensedc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/cl/*
Sourcedc.sourceThe Astrophysical Journales_ES
Keywordsdc.subjectISM: cloudses_ES
Keywordsdc.subjectISM: individual objects (IRDC G028.23-00.19)es_ES
Keywordsdc.subjectISM: kinematics and dynamicses_ES
Keywordsdc.subjectISM:moleculeses_ES
Keywordsdc.subjectStars: formationes_ES
Títulodc.titleA massive prestellar clump hosting no high-mass coreses_ES
Document typedc.typeArtículo de revistaes_ES
Catalogueruchile.catalogadorpgves_ES
Indexationuchile.indexArtículo de publicación ISIes_ES


Files in this item

Icon

This item appears in the following Collection(s)

Show simple item record

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