The kinematics of massive high-redshift dusty star-forming galaxies

ABSTRACT We present a new method for modelling the kinematics of galaxies from interferometric observations by performing the optimization of the kinematic model parameters directly in visibility space instead of the conventional approach of fitting velocity fields produced with the clean algorithm in real-space. We demonstrate our method on Atacama Large Millimeter/submillimeter Array (ALMA) observations of $^{12}$CO (2–1), (3–2), or (4–3) emission lines from an initial sample of 30 massive 850 $\mu$m-selected dusty star-forming galaxies with far-infrared luminosities $\gtrsim$$\, 10^{12}$ L$_{\odot }$ in the redshift range $z \sim$ 1.2–4.7. Using the results from our modelling analysis for the 12 of the 20 sources with the highest signal-to-noise emission lines that show disc-like kinematics, we conclude the following: (i) our sample prefers a CO-to-$H_2$ conversion factor, of $\alpha _{\rm CO} = 0.74 \pm 0.37$; (ii) these far-infrared luminous galaxies follow a similar Tully–Fisher relation between the circular velocity, $V_{\rm circ}$, and baryonic mass, $M_{\rm b}$, as less strongly star-forming samples at high redshift, but extend this relation to much higher masses – showing that these are some of the most massive disc-like galaxies in the Universe; (iii) finally, we demonstrate support for an evolutionary link between massive high-redshift dusty star-forming galaxies and the formation of local early-type galaxies using the both the distributions of the baryonic and kinematic masses of these two populations on the $M_{\rm b}$ – $\sigma$ plane and their relative space densities.

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Publication Details

Journal
Monthly Notices of the Royal Astronomical Society
Published
2024-12-13
DOI
https://doi.org/10.1093/mnras/stae2760
Citations
14
Primary Topic
Astronomy and Astrophysical Research
Type
article
Field-Weighted Citation Impact
7.09

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article

The kinematics of massive high-redshift dusty star-forming galaxies

Fabian Walter, W. N. Brandt, F. Bertoldi, Jacqueline Hodge et al.
14 citations
Monthly Notices of the Royal Astronomical Society
Astronomy and Astrophysical Research
7.09
article

The kinematics of massive high-redshift dusty star-forming galaxies

Fabian Walter, W. N. Brandt, F. Bertoldi, Jacqueline Hodge, U Dudzevičiūtė, Chian-Chou Chen, J.W Nightingale, K. K. Knudsen, Ian Smail, J. L. Wardlow, A. M. Swinbank, Caitlin M. Casey, Jack E. Birkin, S. C. Chapman, P. van der Werf, B. Gullberg, H. Dannerbauer, Aristeidis Amvrosiadis, K. M. Menten, P. Cox
article en
14 citations

Abstract

ABSTRACT We present a new method for modelling the kinematics of galaxies from interferometric observations by performing the optimization of the kinematic model parameters directly in visibility space instead of the conventional approach of fitting velocity fields produced with the clean algorithm in real-space. We demonstrate our method on Atacama Large Millimeter/submillimeter Array (ALMA) observations of $^{12}$CO (2–1), (3–2), or (4–3) emission lines from an initial sample of 30 massive 850 $\mu$m-selected dusty star-forming galaxies with far-infrared luminosities $\gtrsim$$\, 10^{12}$ L$_{\odot }$ in the redshift range $z \sim$ 1.2–4.7. Using the results from our modelling analysis for the 12 of the 20 sources with the highest signal-to-noise emission lines that show disc-like kinematics, we conclude the following: (i) our sample prefers a CO-to-$H_2$ conversion factor, of $\alpha _{\rm CO} = 0.74 \pm 0.37$; (ii) these far-infrared luminous galaxies follow a similar Tully–Fisher relation between the circular velocity, $V_{\rm circ}$, and baryonic mass, $M_{\rm b}$, as less strongly star-forming samples at high redshift, but extend this relation to much higher masses – showing that these are some of the most massive disc-like galaxies in the Universe; (iii) finally, we demonstrate support for an evolutionary link between massive high-redshift dusty star-forming galaxies and the formation of local early-type galaxies using the both the distributions of the baryonic and kinematic masses of these two populations on the $M_{\rm b}$ – $\sigma$ plane and their relative space densities.

Monthly Notices of the Royal Astronomical SocietyVol. 536(4)
Australian National University (AU), Leiden University (NL), Centre National de la Recherche Scientifique (FR), Dalhousie University (CA), Pennsylvania State University (US), Institute of Astronomy and Astrophysics, Academia Sinica (TW), University of Bonn (DE), Universidad de La Laguna (ES), The University of Western Australia (AU), Durham University (GB), Theodore Roosevelt High School (US), Mitchell Institute (US), Institut d'Astrophysique de Paris (FR), Sorbonne Université (FR), ASTRO-3D (AU), Max Planck Institute for Astronomy (DE), Instituto de Astrofísica de Canarias (ES), ARC Centre of Excellence for All-sky Astrophysics (AU), Max Planck Institute for Radio Astronomy (DE), International Centre for Radio Astronomy Research (AU), Chalmers University of Technology (SE), Lancaster University (GB), The University of Texas at Austin (US), Texas A&M University (US)
National Science Foundation, U.S. Nuclear Regulatory Commission, British Interplanetary Society, Department for Business, Energy and Industrial Strategy, UK Government, University of Cambridge, Durham University, Alberta Livestock and Meat Agency, Science and Technology Facilities Council, H2020 European Research Council
Openalex Percentile: Top 3%
Astronomy and Astrophysical Research
7.09
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