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# VALES V: a kinematic analysis of the molecular gas content in H-ATLAS galaxies at z ∼ 0.03–0.35 using ALMA

J Molina, Maarten Baes (UGent) , et al.
(2019) 482(2). p.1499-1524
Author
Organization
Abstract
We present Atacama Large Millimeter/submillimeter Array (ALMA) resolved observations of molecular gas in galaxies up to z = 0.35 to characterize the role of global galactic dynamics on the global interstellar medium properties. These observations consist of a sub-sample of 39 galaxies taken from the Valpara ́ıso ALMA Line Emission Survey (VALES). From the CO(J = 1–0) emission line, we quantify the kinematic parameters by modelling the velocity fields. We find that the infrared (IR) luminosity increases with the rotational to dispersion velocity ratio (Vrot/σv, corrected for inclination). We find a dependence between Vrot/σv and the [C II]/IR ratio, suggesting that the so-called [C II] deficit is related to the dynamical state of the galaxies. We find that global pressure support is needed to reconcile the dynamical mass estimates with the stellar masses in our systems with low Vrot/σv values. The star formation rate (SFR) is weakly correlated with the molecular gas fraction (fH2 ) in our sample, suggesting that the release of gravitational energy from cold gas may not be the main energy source of the turbulent motions seen in the VALES galaxies. By defining a proxy of the ‘star formation efficiency’ (SFE) parameter as the SFR divided by the CO luminosity (SFE′ ≡SFR/L′CO), we find a constant SFE per crossing time (tcross). We suggest that tcross may be the controlling time-scale in which the star formation occurs in dusty z ∼ 0.03–0.35 galaxies.

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## Citation

Chicago
Molina, J, Edo Ibar, V Villanueva, A Escala, C Cheng, Maarten Baes, H Messias, et al. 2019. “VALES V: a Kinematic Analysis of the Molecular Gas Content in H-ATLAS Galaxies at z ∼ 0.03–0.35 Using ALMA.” Monthly Notices of the Royal Astronomical Society 482 (2): 1499–1524.
APA
Molina, J., Ibar, E., Villanueva, V., Escala, A., Cheng, C., Baes, M., Messias, H., et al. (2019). VALES V: a kinematic analysis of the molecular gas content in H-ATLAS galaxies at z ∼ 0.03–0.35 using ALMA. Monthly Notices of the Royal Astronomical Society, 482(2), 1499–1524.
Vancouver
1.
Molina J, Ibar E, Villanueva V, Escala A, Cheng C, Baes M, et al. VALES V: a kinematic analysis of the molecular gas content in H-ATLAS galaxies at z ∼ 0.03–0.35 using ALMA. Monthly Notices of the Royal Astronomical Society. Oxford University Press (OUP); 2019;482(2):1499–524.
MLA
Molina, J et al. “VALES V: a Kinematic Analysis of the Molecular Gas Content in H-ATLAS Galaxies at z ∼ 0.03–0.35 Using ALMA.” Monthly Notices of the Royal Astronomical Society 482.2 (2019): 1499–1524. Print.
@article{8607439,
abstract     = {We present Atacama Large Millimeter/submillimeter Array (ALMA) resolved observations of molecular gas in galaxies up to z = 0.35 to characterize the role of global galactic dynamics on the global interstellar medium properties. These observations consist of a sub-sample of 39 galaxies taken from the Valpara \unmatched{0301}{\i}so ALMA Line Emission Survey (VALES). From the CO(J = 1--0) emission line, we quantify the kinematic parameters by modelling the velocity fields. We find that the infrared (IR) luminosity increases with the rotational to dispersion velocity ratio (Vrot/\ensuremath{\sigma}v, corrected for inclination). We find a dependence between Vrot/\ensuremath{\sigma}v and the [C II]/IR ratio, suggesting that the so-called [C II] deficit is related to the dynamical state of the galaxies. We find that global pressure support is needed to reconcile the dynamical mass estimates with the stellar masses in our systems with low Vrot/\ensuremath{\sigma}v values. The star formation rate (SFR) is weakly correlated with the molecular gas fraction (fH2 ) in our sample, suggesting that the release of gravitational energy from cold gas may not be the main energy source of the turbulent motions seen in the VALES galaxies. By defining a proxy of the {\textquoteleft}star formation efficiency{\textquoteright} (SFE) parameter as the SFR divided by the CO luminosity (SFE{\textquotesingle} \ensuremath{\equiv}SFR/L{\textquotesingle}CO), we find a constant SFE per crossing time (tcross). We suggest that tcross may be the controlling time-scale in which the star formation occurs in dusty z \ensuremath{\sim} 0.03--0.35 galaxies.},
author       = {Molina, J and Ibar, Edo and Villanueva, V and Escala, A and Cheng, C and Baes, Maarten and Messias, H and Yang, C and Bauer, F E and Werf, van der and Leiton, R and Aravena, M and Swinbank, A M and Micha\unmatched{0142}owski, M J and Mu{\~n}oz-Arancibia, A M and Orellana, G and Hughes, T M and Farrah, D and De~Zotti, G and Lara-L{\'o}pez, M A and Eales, S and Dunne, L},
issn         = {0035-8711},
journal      = {Monthly Notices of the Royal Astronomical Society},
language     = {eng},
number       = {2},
pages        = {1499--1524},
publisher    = {Oxford University Press (OUP)},
title        = {VALES V: a kinematic analysis of the molecular gas content in H-ATLAS galaxies at z~\ensuremath{\sim}~0.03--0.35 using ALMA},
url          = {http://dx.doi.org/10.1093/mnras/sty2577},
volume       = {482},
year         = {2019},
}


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