The MAGPI Survey

Autor(en)
Yifan Mai, Scott M. Croom, Emily Wisnioski, Sam P. Vaughan, Mathew R. Varidel, Andrew J. Battisti, J. Trevor Mendel, Marcie Mun, Takafumi Tsukui, Caroline Foster, Katherine E. Harborne, Claudia D.P. Lagos, Di Wang, Sabine Bellstedt, Joss Bland-Hawthorn, Matthew Colless, Francesco D'Eugenio, Kathryn Grasha, Yingjie Peng, Giulia Santucci, Sarah M. Sweet, Sabine Thater, Lucas M. Valenzuela, Bodo Ziegler
Abstrakt

We measure the ionized gas velocity dispersions of star-forming galaxies in the MAGPI survey (z∼.03) and compare them with galaxies in the SAMI (z∼0.05) and KROSS (z∼1) surveys to investigate how the ionized gas velocity dispersion evolves. For the first time, we use a consistent method that forward models galaxy kinematics from z=0 to z=1. This method accounts for spatial substructure in emission line flux and beam smearing. We investigate the correlation between gas velocity dispersion and galaxy properties to understand the mechanisms that drive gas turbulence. We find that in both MAGPI and SAMI galaxies, the gas velocity dispersion more strongly correlates with the star-formation rate surface density (ΣSFR) than with a variety of other physical properties, and the average gas velocity dispersion is similar, at the same, for SAMI, MAGPI, and KROSS galaxies. The results indicate that mechanisms related to ΣSFR could be the dominant driver of gas turbulence from z∼1 to z∼0, for example, stellar feedback and/or gravitational instability. The gas velocity dispersion of MAGPI galaxies is also correlated with the non-rotational motion of the gas, illustrating that in addition to star-formation feedback, gas transportation and accretion may also contribute to the gas velocity dispersion for galaxies at z∼0.3. KROSS galaxies only have a moderate correlation between gas velocity dispersion and ΣSFR and a higher scatter of gas velocity dispersion with respect to, in agreement with the suggestion that other mechanisms, such as gas transportation and accretion, are relatively more important at higher redshift galaxies.

Organisation(en)
Institut für Astrophysik
Externe Organisation(en)
The University of Sydney, ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australian National University, Macquarie University, Swinburne University of Technology, University of New South Wales, University of Western Australia, University of Oxford, University of Cambridge, Peking University, University of Queensland, Ludwig-Maximilians-Universität München
Journal
Monthly Notices of the Royal Astronomical Society
Band
533
Seiten
3878-3892
Anzahl der Seiten
15
ISSN
0035-8711
DOI
https://doi.org/10.1093/mnras/stae2033
Publikationsdatum
10-2024
Peer-reviewed
Ja
ÖFOS 2012
103003 Astronomie, 103004 Astrophysik
Schlagwörter
ASJC Scopus Sachgebiete
Astronomy and Astrophysics, Space and Planetary Science
Link zum Portal
https://ucrisportal.univie.ac.at/de/publications/5cefe318-0cf3-449d-be7b-101d91f7996e