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SUMMARY:Kinematics of galaxy bulges\, disks\, and ionised gas from 3D spec
 troscopy - Sree Oh (ANU)
DTSTART:20230623T103000Z
DTEND:20230623T113000Z
UID:TALK201061@talks.cam.ac.uk
CONTACT:Sandro Tacchella
DESCRIPTION:The spatially-resolved kinematics of bulge and disk components
  from 3D spectroscopy describe how galaxies have a wide range of stellar k
 inematics according to galaxy types. Kinematic scaling relations demonstra
 te that the galaxy stellar mass scales with kinematics for both bulge and 
 disk components of all galaxy types\, which suggests kinematics of two com
 ponents are less dependent on galaxy populations and largely determined by
  the mass. Our findings also suggest that the relative contributions of bu
 lge and disk components explain\, at least to first order\, the complex ki
 nematic behaviour of galaxies according to galaxy type. 3D spectroscopy al
 so allows studying the impact of feedback processes on the gas and stellar
  velocity dispersions (σgas and σstar). σstar (derived from absorption 
 lines) tends to be higher than σgas (measured using emission lines)\, sug
 gesting that stars are generally dynamically hotter than ionised gas. We f
 ind that the ratio of σgas and σ∗ (Δσ = log σgas/σ∗) strongly co
 rrelates with the contribution of AGN\, implying that AGN inflates gas vel
 ocity dispersions. One possibility is AGN-driven outflow. We confirm the i
 mpact of AGN on gas kinematics by fitting emission lines with broad and na
 rrow components. Galaxies with broad component show inflated gas velocity 
 dispersions than the prediction. Also\, we find a tight correlation betwee
 n the velocity dispersion of the broad component (σbroad) and the power s
 ources: AGN shows a much higher σbroad. Therefore\, we conclude that gas 
 kinematics is sensitive to the power sources\, and AGN contributes to infl
 ated gas velocity dispersions.
LOCATION:Ryle seminar room + online
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