Show simple item record

Authordc.contributor.authorLiu, Tie 
Authordc.contributor.authorKim, Kee-Tae 
Authordc.contributor.authorYoo, Hyunju 
Authordc.contributor.authorLiu, Sheng-yuan 
Authordc.contributor.authorTatematsu, Ken'ichi 
Authordc.contributor.authorQin, Sheng-Li 
Authordc.contributor.authorZhang, Qizhou 
Authordc.contributor.authorWu, Yuefang 
Authordc.contributor.authorWang, Ke 
Authordc.contributor.authorGoldsmith, Paul 
Authordc.contributor.authorJuvela, Mika 
Authordc.contributor.authorLee, Jeong-Eun 
Authordc.contributor.authorTóth, L. Viktor 
Authordc.contributor.authorMardones Pérez, Diego 
Authordc.contributor.authorGaray Brignardello, Guido 
Authordc.contributor.authorBronfman Aguiló, Leonardo 
Authordc.contributor.authorCunningham, Maria 
Authordc.contributor.authorLi, Di 
Authordc.contributor.authorLo, Nadia 
Authordc.contributor.authorRistorcelli, Isabelle 
Authordc.contributor.authorSchnee, Scott 
Cita de ítemdc.identifier.citationThe Astrophysical Journal, 829:59 (21pp), 2016 October 1es_ES
Abstractdc.description.abstractWe observed 146 Galactic clumps in HCN (4-3) and CS (7-6) with the Atacama Submillimeter Telescope Experiment 10 m telescope. A tight linear relationship between star formation rate and gas mass traced by dust continuum emission was found for both Galactic clumps and the high redshift (z > 1) star forming galaxies (SFGs), indicating a constant gas depletion time of ~100 Myr for molecular gas in both Galactic clumps and high z SFGs. However, low z galaxies do not follow this relation and seem to have a longer global gas depletion time. The correlations between total infrared luminosities (L TIR) and molecular line luminosities $({L}_{\mathrm{mol}}^{\prime })$ of HCN (4-3) and CS (7-6) are tight and sublinear extending down to clumps with L TIR ~ 103 L ☉. These correlations become linear when extended to external galaxies. A bimodal behavior in the L TIR–${L}_{\mathrm{mol}}^{\prime }$ correlations was found for clumps with different dust temperature, luminosity-to-mass ratio, and σ line/σ vir. Such bimodal behavior may be due to evolutionary effects. The slopes of L TIR–L'mol correlations become more shallow as clumps evolve. We compared our results with lower J transition lines in Wu et al. (2010). The correlations between clump masses and line luminosities are close to linear for low effective excitation density tracers but become sublinear for high effective excitation density tracers for clumps with L TIR larger than L TIR ~ 104.5 L ☉. High effective excitation density tracers cannot linearly trace the total clump masses, leading to a sublinear correlations for both M clump–L'mol and L TIR–L'mol relations.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: evolutiones_ES
Keywordsdc.subjectgalaxies: ISMes_ES
Keywordsdc.subjectISM: kinematics and dynamicses_ES
Keywordsdc.subjectstars: formationes_ES
Area Temáticadc.subject.otherAstronomíaes_ES
Títulodc.titleStar formation laws in both galactic massive clumps and external galaxies: extensive study with dust coninuum, HCN (4-3), AND CS (7-6)es_ES
Document typedc.typeArtículo de revista
Indexationuchile.indexArtículo de publicación ISIes_ES

Files in this item


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