Kavli Affiliate: Yingjie Peng
| First 5 Authors: Yifan Mai, Scott M. Croom, Emily Wisnioski, Sam P. Vaughan, Mathew R. Varidel
| Summary:
We measure the ionised gas velocity dispersions of star-forming galaxies in
the MAGPI survey ($zsim0.3$) and compare them with galaxies in the SAMI
($zsim0.05$) and KROSS ($zsim1$) surveys to investigate how the ionised 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 ($Sigma_{rm SFR}$)
than with a variety of other physical properties, and the average gas velocity
dispersion is similar, at the same $Sigma_{rm SFR}$, for SAMI, MAGPI and
KROSS galaxies. The results indicate that mechanisms related to $Sigma_{rm
SFR}$ could be the dominant driver of gas turbulence from $zsim1$ to $zsim0$,
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 $zsim 0.3$. KROSS galaxies only
have a moderate correlation between gas velocity dispersion and $Sigma_{rm
SFR}$ and a higher scatter of gas velocity dispersion with respect to
$Sigma_{rm SFR}$, in agreement with the suggestion that other mechanisms,
such as gas transportation and accretion, are relatively more important at
higher redshift galaxies.
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