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The MAGPI survey: Drivers of kinematic asymmetries in the ionised gas of z ∼ 0.3 star-forming galaxies

Published online by Cambridge University Press:  28 November 2023

R.S. Bagge Open the ORCID record for R.S. Bagge [Opens in a new window] ,
C. Foster ,
A. Battisti ,
S. Bellstedt ,
M. Mun ,
K. Harborne ,
S. Barsanti ,
T. Mendel ,
S. Brough  and
S.M. Croom
...Show all authors
R.S. Bagge*
Affiliation:
School of Physics, University of New South Wales, Kensington, NSW, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia
C. Foster
Affiliation:
School of Physics, University of New South Wales, Kensington, NSW, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia
A. Battisti
Affiliation:
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia Research School of Astronomy and Astrophysics, Australian National University, Weston Creek, ACT, Australia
S. Bellstedt
Affiliation:
ICRAR, The University of Western Australia, Crawley, WA, Australia
M. Mun
Affiliation:
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia Research School of Astronomy and Astrophysics, Australian National University, Weston Creek, ACT, Australia
K. Harborne
Affiliation:
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia ICRAR, The University of Western Australia, Crawley, WA, Australia
S. Barsanti
Affiliation:
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia Research School of Astronomy and Astrophysics, Australian National University, Weston Creek, ACT, Australia Sydney Institue for Astronomy, School of Physics, University of Sydney, Camperdown, NSW, Australia
T. Mendel
Affiliation:
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia Research School of Astronomy and Astrophysics, Australian National University, Weston Creek, ACT, Australia
S. Brough
Affiliation:
School of Physics, University of New South Wales, Kensington, NSW, Australia ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia
S.M. Croom
Affiliation:
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia Sydney Institue for Astronomy, School of Physics, University of Sydney, Camperdown, NSW, Australia
C.D.P. Lagos
Affiliation:
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia ICRAR, The University of Western Australia, Crawley, WA, Australia
T. Mukherjee
Affiliation:
Australian Astronomical Optics, Macquarie University, North Ryde, NSW, Australia
Y. Peng
Affiliation:
Department of Astronomy, School of Physics, Peking University, Beijing, China Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, China
R.-S. Remus
Affiliation:
Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians-Universität München, München, Germany
G. Santucci
Affiliation:
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia ICRAR, The University of Western Australia, Crawley, WA, Australia
P. Sharda
Affiliation:
Leiden Observatory, Leiden University, RA, Leiden, The Netherlands
S. Thater
Affiliation:
Department of Astrophysics, University of Vienna, Vienna, Austria
J. van de Sande
Affiliation:
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia Sydney Institue for Astronomy, School of Physics, University of Sydney, Camperdown, NSW, Australia
L.M. Valenzuela
Affiliation:
Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians-Universität München, München, Germany
E. Wisnioski
Affiliation:
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australia Research School of Astronomy and Astrophysics, Australian National University, Weston Creek, ACT, Australia
T. Zafar
Affiliation:
Australian Astronomical Optics, Macquarie University, North Ryde, NSW, Australia Astronomy, Astrophysics and Astrophotonics Research Centre, Macquarie University, Sydney, NSW, Australia
B. Ziegler
Affiliation:
Department of Astrophysics, University of Vienna, Vienna, Austria
*
Corresponding author: R. S. Bagge, Email: r.bagge@unsw.edu.au
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Abstract

Galaxy gas kinematics are sensitive to the physical processes that contribute to a galaxy’s evolution. It is expected that external processes will cause more significant kinematic disturbances in the outer regions, while internal processes will cause more disturbances for the inner regions. Using a subsample of 47 galaxies ($0.27<z<0.36$) from the Middle Ages Galaxy Properties with Integral Field Spectroscopy (MAGPI) survey, we conduct a study into the source of kinematic disturbances by measuring the asymmetry present in the ionised gas line-of-sight velocity maps at the $0.5R_e$ (inner regions) and $1.5R_e$ (outer regions) elliptical annuli. By comparing the inner and outer kinematic asymmetries, we aim to better understand what physical processes are driving the asymmetries in galaxies. We find the local environment plays a role in kinematic disturbance, in agreement with other integral field spectroscopy studies of the local universe, with most asymmetric systems being in close proximity to a more massive neighbour. We do not find evidence suggesting that hosting an Active Galactic Nucleus contributes to asymmetry within the inner regions, with some caveats due to emission line modelling. In contrast to previous studies, we do not find evidence that processes leading to asymmetry also enhance star formation in MAGPI galaxies. Finally, we find a weak anti-correlation between stellar mass and asymmetry (i.e., high stellar mass galaxies are less asymmetric). We conclude by discussing possible sources driving the asymmetry in the ionised gas, such as disturbances being present in the colder gas phase (either molecular or atomic) prior to the gas being ionised, and non-axisymmetric features (e.g., a bar) being present in the galactic disk. Our results highlight the complex interplay between ionised gas kinematic disturbances and physical processes involved in galaxy evolution.

Keywords

galaxies: evolutiongalaxies: formationgalaxies: interactionsgalaxies: ISMgalaxies: kinematics and dynamicsgalaxies: star formation
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 40 , 2023 , e060
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of the Astronomical Society of Australia

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