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Infall signatures in a prestellar core embedded in the high-mass 70 mu m Dark IRDC G331.372-00.116

Authordc.contributor.authorContreras, Yanett 
Authordc.contributor.authorSanhueza, Patricio 
Authordc.contributor.authorJackson, James M. 
Authordc.contributor.authorGuzmán, Andrés E. 
Authordc.contributor.authorLongmore, Steven 
Authordc.contributor.authorGaray Brignardello, Guido 
Authordc.contributor.authorZhang, Qizhou 
Authordc.contributor.authorQuang, Nguyen-Lu'o'Ng 
Authordc.contributor.authorTatematsu, Ken'ichi 
Authordc.contributor.authorNakamura, Fumitaka 
Authordc.contributor.authorSakai, Takeshi 
Authordc.contributor.authorOhashi, Satoshi 
Authordc.contributor.authorLiu, Tie 
Authordc.contributor.authorSaito, Masao 
Authordc.contributor.authorGómez, Laura 
Authordc.contributor.authorRathborne, Jill 
Authordc.contributor.authorWhitaker, Scott 
Cita de ítemdc.identifier.citationAstrophysical Journal Volumen: 861 Número: 1 Número de artículo: 14es_ES
Abstractdc.description.abstractUsing Galactic Plane surveys, we have selected a massive (1200M circle dot), cold (14 K) 3.6-70 mu m dark IRDC, G331.372-00.116. This infrared dark cloud (IRDC) has the potential to form high-mass stars, and given the absence of current star formation signatures, it seems to represent the earliest stages of high-mass star formation. We have mapped the whole IRDC with the Atacama Large Millimeter/submillimeter Array (ALMA) at 1.1 and 1.3 mm in dust continuum and line emission. The dust continuum reveals 22 cores distributed across the IRDC. In this work, we analyze the physical properties of the most massive core, ALMA1, which has no molecular outflows detected in the CO (2-1), SiO (5-4), and H2CO (3-2) lines. This core is relatively massive (M = 17.6M circle dot), subvirialized (virial parameter alpha(vir) = M-vir/M = 0.14), and is barely affected by turbulence (transonic Mach number of 1.2). Using the HCO+ (3-2) line, we find the first detection of infall signatures in a relatively massive, prestellar core (ALMA1) with the potential to form a high-mass star. We estimate an infall speed of 1.54 km s(-1) and a high accretion rate of 1.96. x. 10(-3) M circle dot yr(-1). ALMA1 is rapidly collapsing, out of virial equilibrium, which is more consistent with competitive accretion scenarios rather than the turbulent core accretion model. On the other hand, ALMA1 has a mass similar to 6 times larger than the clumps Jeans mass, as it is in an intermediate mass regime (M-J = 2.7 < M less than or similar to 30 M circle dot), contrary to what both the competitive accretion and turbulent core accretion theories predict.es_ES
Patrocinadordc.description.sponsorshipNational Astronomical Observatory of Japan FONDECYT 3150570 Japan Society for the Promotion of Science (JSPS) 18H01259 Conicyt project PFB-06es_ES
Publisherdc.publisherIOP Publishinges_ES
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 Chile*
Link to Licensedc.rights.uri*
Sourcedc.sourceAstrophysical Journales_ES
Keywordsdc.subjectISM: cloudses_ES
Keywordsdc.subjectISM: individual objects (IRDC G331.372-00.116)es_ES
Keywordsdc.subjectISM: kinematics and dynamicses_ES
Keywordsdc.subjectISM: moleculeses_ES
Keywordsdc.subjectStars: formationes_ES
Títulodc.titleInfall signatures in a prestellar core embedded in the high-mass 70 mu m Dark IRDC G331.372-00.116es_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