Strings

Juneau, Josh; Manelli, Luciano

doi:10.1007/978-1-4842-7963-2_3

Cited by 1 publication

(2 citation statements)

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“…AGNs are proven essential for reproducing the high mass end of the observed stellar mass function by preventing hot halo gas from cooling, effectively stopping further star formation in massive galaxies (Silk & Rees 1998; Bower et al 2006; Hopkins et al 2006; Schaye et al 2015; Bower et al 2017). AGN are also often found in galaxies with disturbed kinematics (Greene et al 2011; Zakamska et al 2016; Ellison et al 2019; Juneau et al 2022). Being centrally located within the galaxy, we might expect that the asymmetry would be larger inside a galaxy than it is in the outskirts for a galaxy with an AGN.…”

Section: Resultsmentioning

confidence: 99%

“…These gaseous flows onto the central regions of galaxies can trigger a galaxy’s Active Galactic Nucleus (AGN), which can contribute to ‘quenching’ the SFR in high stellar mass galaxies (e.g., Schawinski et al 2007). AGNs are also a known source of outflows, and can disturb the kinematics of the entire galactic disk (e.g., Greene et al 2011; Zakamska et al 2016) and are a suspected cause of complex kinematic features in a velocity maps (Juneau et al 2022).…”

Section: Introductionmentioning

confidence: 99%

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

Bagge,

Foster,

Battisti

et al. 2023

Publ. Astron. Soc. Aust.

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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.

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%