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Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z similar to 2-4 as probed by multi-J CO lines
Yang, C.; Omont, A.; Beelen, A.; Gao, Y.; van der Werf, P.; Gavazzi, R.; Zhang, Z. -Y.; Ivison, R.; Lehnert, M.; Liu, D.; Oteo, I.; Gonzalez-Alfonso, E.; Dannerbauer, H.; Cox, P.; Krips, M.; Neri, R.; Riechers, D.; Baker, A. J.; Michalowski, M. J.; Cooray, A.; Smail, I.
2017
发表期刊ASTRONOMY & ASTROPHYSICS
卷号608页码:A144
摘要We present the IRAM-30m observations of multiple-J CO (J(up) mostly from 3 up to 8) and [CI](P-3(2) -> P-3(1)) ([CI](2-1) hereafter) line emission in a sample of redshift similar to 2-4 submillimeter galaxies (SMGs). These SMGs are selected among the brightest-lensed galaxies discovered in the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). Forty-seven CO lines and 7 [CI](2-1) lines have been detected in 15 lensed SMGs. A non-negligible effect of differential lensing is found for the CO emission lines, which could have caused significant underestimations of the linewidths, and hence of the dynamical masses. The CO spectral line energy distributions (SLEDs), peaking around J(up) similar to 5-7, are found to be similar to those of the local starburst-dominated ultra-luminous infrared galaxies and of the previously studied SMGs. After correcting for lensing amplification, we derived the global properties of the bulk of molecular gas in the SMGs using non-LTE radiative transfer modelling, such as the molecular gas density n(H2) similar to 10(2.5)-10(4.1) cm(-3) and the kinetic temperature T-k similar to 20-750 K. The gas thermal pressure P-th ranging from similar to 10(5) Kcm(-3) to 10(6) Kcm(-3) is found to be correlated with star formation efficiency. Further decomposing the CO SLEDs into two excitation components, we find a low-excitation component with n(H2) similar to 10(2.8)-10(4.6) cm(-3) and T-k similar to 20-30 K, which is less correlated with star formation, and a high-excitation one (n(H2) similar to 10(2.7)-10(4.2) cm(-3), T-k similar to 60-400 K) which is tightly related to the on-going star-forming activity. Additionally, tight linear correlations between the far-infrared and CO line luminosities have been confirmed for the J(up) >= 5 CO lines of these SMGs, implying that these CO lines are good tracers of star formation. The [C I](2-1) lines follow the tight linear correlation between the luminosities of the [C I](2-1) and the CO(1-0) line found in local starbursts, indicating that [C I] lines could serve as good total molecular gas mass tracers for high-redshift SMGs as well. The total mass of the molecular gas reservoir, (1-30) x 10(10) M circle dot, derived based on the CO(3-2) fluxes and alpha(CO(1-0)) = 0.8 M circle dot (K km s(-1) pc(2))(-1), suggests a typical molecular gas depletion time t(dep) similar to 20-100 Myr and a gas to dust mass ratio delta(GDR) similar to 30-100 with similar to 20%-60% uncertainty for the SMGs. The ratio between CO line luminosity and the dust mass L'(CO)/M-dust appears to be slowly increasing with redshift for high-redshift SMGs, which need to be further confirmed by a more complete SMG sample at various redshifts. Finally, through comparing the linewidth of CO and H2O lines, we find that they agree well in almost all our SMGs, confirming that the emitting regions of the CO and H2O lines are co-spatially located.
DOI10.1051/0004-6361/201731391
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文献类型期刊论文
条目标识符http://libir.pmo.ac.cn/handle/332002/17883
专题期刊(老文献)
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Yang, C.,Omont, A.,Beelen, A.,et al. Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z similar to 2-4 as probed by multi-J CO lines[J]. ASTRONOMY & ASTROPHYSICS,2017,608:A144.
APA Yang, C..,Omont, A..,Beelen, A..,Gao, Y..,van der Werf, P..,...&Smail, I..(2017).Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z similar to 2-4 as probed by multi-J CO lines.ASTRONOMY & ASTROPHYSICS,608,A144.
MLA Yang, C.,et al."Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z similar to 2-4 as probed by multi-J CO lines".ASTRONOMY & ASTROPHYSICS 608(2017):A144.
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