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WALLABY pilot survey: The diversity of HI structural parameters in nearby galaxies

Published online by Cambridge University Press:  08 June 2023

T. N. Reynolds*
Affiliation:
International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia
B. Catinella
Affiliation:
International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia
L. Cortese
Affiliation:
International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia
N. Deg
Affiliation:
Department of Physics, Engineering Physics, and Astronomy, Queen’s University, Kingston, ON K7L 3N6, Canada
H. Dénes
Affiliation:
ASTRON - The Netherlands Institute for Radio Astronomy, 7991 PD Dwingeloo, The Netherlands
A. Elagali
Affiliation:
School of Biological Sciences, The University of Western Australia, Perth, WA, Australia Minderoo Foundation, Perth, WA, Australia
B.-Q. For
Affiliation:
International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia
P. Kamphuis
Affiliation:
Faculty of Physics and Astronomy, Ruhr University Bochum, Astronomical Institute (AIRUB), Bochum D-44780, Germany
D. Kleiner
Affiliation:
INAF - Osservatorio Astronomico di Cagliari, Via della Scienza 5, Selargius, CA 09047, Italy
B. S. Koribalski
Affiliation:
CSIRO Space and Astronomy, PO Box 76, Epping, NSW 1710, Australia School of Science, Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia
K. Lee-Waddell
Affiliation:
International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia CSIRO Space and Astronomy, PO Box 1130, Bentley, WA 6102, Australia
C. Murugeshan
Affiliation:
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia CSIRO Space and Astronomy, PO Box 1130, Bentley, WA 6102, Australia
W. Raja
Affiliation:
CSIRO Space and Astronomy, PO Box 76, Epping, NSW 1710, Australia
J. Rhee
Affiliation:
International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia
K. Spekkens
Affiliation:
Department of Physics and Space Science, Royal Military College of Canada, PO Box 17000, Station Forces, Kingston, ON K7L 2E1, Canada
L. Staveley-Smith
Affiliation:
International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia
J. M. van der Hulst
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, Landleven 12, 9747AD Groningen, The Netherlands
J. Wang
Affiliation:
Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China
T. Westmeier
Affiliation:
International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia
O. I. Wong
Affiliation:
International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia CSIRO Space and Astronomy, PO Box 1130, Bentley, WA 6102, Australia
F. Bigiel
Affiliation:
Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
A. Bosma
Affiliation:
Aix Marseille Université, CNRS, CNES, LAM, Marseille, France
B. W. Holwerda
Affiliation:
Department of Physics and Astronomy, University of Louisville, Natural Science Building 102, Louisville, KY 40292, USA
D. A. Leahy
Affiliation:
Department of Physics and Astronomy, University of Calgary, Calgary, AB T2N 1N4, Canada
M. J. Meyer
Affiliation:
International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia
*
Corresponding author: T. N. Reynolds; Email: tristan.reynolds@uwa.edu.au.

Abstract

We investigate the diversity in the sizes and average surface densities of the neutral atomic hydrogen (H i) gas discs in $\sim$280 nearby galaxies detected by the Widefield ASKAP L-band Legacy All-sky Blind Survey (WALLABY). We combine the uniformly observed, interferometric H i data from pilot observations of the Hydra cluster and NGC 4636 group fields with photometry measured from ultraviolet, optical, and near-infrared imaging surveys to investigate the interplay between stellar structure, star formation, and H i structural parameters. We quantify the H i structure by the size of the H i relative to the optical disc and the average H i surface density measured using effective and isodensity radii. For galaxies resolved by $>$$1.3$ beams, we find that galaxies with higher stellar masses and stellar surface densities tend to have less extended H i discs and lower H i surface densities: the isodensity H i structural parameters show a weak negative dependence on stellar mass and stellar mass surface density. These trends strengthen when we limit our sample to galaxies resolved by $>$2 beams. We find that galaxies with higher H i surface densities and more extended H i discs tend to be more star forming: the isodensity H i structural parameters have stronger correlations with star formation. Normalising the H i disc size by the optical effective radius (instead of the isophotal radius) produces positive correlations with stellar masses and stellar surface densities and removes the correlations with star formation. This is due to the effective and isodensity H i radii increasing with mass at similar rates while, in the optical, the effective radius increases slower than the isophotal radius. Our results are in qualitative agreement with previous studies and demonstrate that with WALLABY we can begin to bridge the gap between small galaxy samples with high spatial resolution H i data and large, statistical studies using spatially unresolved, single-dish data.

Type
Research Article
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of the Astronomical Society of Australia

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