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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

Molina, J; Ibar, Edo; Villanueva, V; Escala, A; Cheng, C; Baes, M; Messias, H; Yang, C; Bauer, FE; Werf, van der; Leiton, R; Aravena, M; Swinbank, AM; Michałowski, MJ; Muñoz-Arancibia, AM; Orellana, G; Hughes, TM; Farrah, D; De Zotti, G; Lara-López, MA; Eales, S; Dunne, L

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


J Molina

Edo Ibar

V Villanueva

A Escala

C Cheng

M Baes

H Messias

C Yang

FE Bauer

van der Werf

R Leiton

M Aravena

MJ Michałowski

AM Muñoz-Arancibia

G Orellana

TM Hughes

D Farrah

G De Zotti

MA Lara-López

S Eales

L Dunne


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 Valparaíso 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.

Journal Article Type Article
Acceptance Date Sep 14, 2018
Online Publication Date Sep 20, 2018
Publication Date Sep 20, 2018
Deposit Date Dec 6, 2018
Publicly Available Date Dec 6, 2018
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Royal Astronomical Society
Peer Reviewed Peer Reviewed
Volume 482
Issue 2
Pages 1499-1524
Public URL


Published Journal Article (5.7 Mb)

Copyright Statement
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2018 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

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