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The kiloparsec-scale gas kinematics in two star-forming galaxies at z ∼ 1.47 seen with ALMA and VLT-SINFONI.

Molina, J. and Ibar, E. and Smail, I. and Swinbank, A. M. and Villard, E. and Escala, A. and Sobral, D. and Hughes, T. M. (2019) 'The kiloparsec-scale gas kinematics in two star-forming galaxies at z ∼ 1.47 seen with ALMA and VLT-SINFONI.', Monthly notices of the Royal Astronomical Society., 487 (4). pp. 4856-4869.


We present Atacama Large Millimeter/submillimeter Array (ALMA) CO(J = 2 − 1) observations of two main-sequence star-forming galaxies at z ∼ 1.47 taken from the High-Z Emission Line Survey (HiZELS). These two systems have been previously reported to be molecular gas rich fH2≡MH2/(MH2+M⋆)∼0.8⁠. We carried out a follow-up study to resolve, at ∼kpc-scales, the CO emission. These new observations are combined with our earlier ALMA observations (sensitive to diffuse CO emission) and compared with our previous Hα-based study at matched spatial resolution. One target is marginally resolved in CO(2-1), showing complex dynamics with respect to the ionised gas traced by Hα. While the other source is spatially resolved, enabling a detailed exploration of its internal dynamical properties. In this system, both gaseous phases show similar spatial extension, rotation velocities and velocity dispersions (Vrot ∼ σv ∼ 100 km s−1) suggesting a rotational velocity to velocity dispersion ratio consistent with unity. By comparing the ionized and molecular gas tracers through the use of a two-dimensional kinematic model, we estimate a median depletion time τdep = 2.3 ± 1.2 Gyr for the galaxy as a whole. This value is in agreement with the average τdep value observed in local star-forming galaxies at similar spatial scales. Using a thick-disk dynamical modelling, we derive a dynamical mass Mdyn = (1.59 ± 0.19) × 1011 M⊙ within ≈6 kpc. This suggests a dark matter fraction (fDM ≡ MDM/Mdyn of 0.59 ± 0.10, in agreement with the average fDM value derived from stacked rotation curve analysis of galaxies at similar redshift range.

Item Type:Article
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Publisher statement:© 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
Date accepted:08 June 2019
Date deposited:14 June 2019
Date of first online publication:13 June 2019
Date first made open access:No date available

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