Ionised gas outflow signatures in SDSS-IV MaNGA active galactic nuclei. (arXiv:1911.10212v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wylezalek_D/0/1/0/all/0/1">Dominika Wylezalek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flores_A/0/1/0/all/0/1">Anthony M. Flores</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zakamska_N/0/1/0/all/0/1">Nadia L. Zakamska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greene_J/0/1/0/all/0/1">Jenny E. Greene</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riffel_R/0/1/0/all/0/1">Rogemar A. Riffel</a>

The prevalence of outflow and feedback signatures in active galactic nuclei
(AGN) is a major unresolved question which large integral field unit (IFU)
surveys now allow to address. In this paper, we present a kinematic analysis of
the ionised gas in 2778 galaxies at z $sim$ 0.05 observed by SDSS-IV MaNGA.
Specifically, we measure the kinematics of the [OIII] {lambda}5007{AA}
emission line in each spatial element and fit multiple Gaussian components to
account for possible non-gravitational motions of gas. Comparing the kinematics
of the ionised gas between 308 MaNGA-selected AGN that have been previously
identified through emission line diagnostics and sources not classified as AGN,
we find that while 25% of MaNGA-selected AGN show [OIII] components with
emission line widths of $>$ 500 km/s in more than 10% of their spaxels, only 7%
of MaNGA non-AGN show a similar signature. Even the AGN that do not show
nuclear AGN photoionisation signatures and that were only identified as AGN
based on their larger scale photoionisation signatures show similar kinematic
characteristics. In addition to obscuration, another possibility is that
outflow and mechanical feedback signatures are longer lived than the AGN
itself. Our measurements demonstrate that high velocity gas is more prevalent
in AGN compared to non-AGN and that outflow and feedback signatures in
low-luminosity, low-redshift AGN may so far have been underestimated. We show
that higher luminosity MaNGA-selected AGN are able to drive larger scale
outflows than lower luminosity AGN. But estimates of the kinetic coupling
efficiencies are $<$ 1% and suggest that the feedback signatures probed in this paper are unlikely to have a significant impact on the AGN host galaxies. However, continuous energy injection may still heat a fraction of the cool gas and delay or suppress star formation in individual galaxies even when the AGN is weak.

The prevalence of outflow and feedback signatures in active galactic nuclei
(AGN) is a major unresolved question which large integral field unit (IFU)
surveys now allow to address. In this paper, we present a kinematic analysis of
the ionised gas in 2778 galaxies at z $sim$ 0.05 observed by SDSS-IV MaNGA.
Specifically, we measure the kinematics of the [OIII] {lambda}5007{AA}
emission line in each spatial element and fit multiple Gaussian components to
account for possible non-gravitational motions of gas. Comparing the kinematics
of the ionised gas between 308 MaNGA-selected AGN that have been previously
identified through emission line diagnostics and sources not classified as AGN,
we find that while 25% of MaNGA-selected AGN show [OIII] components with
emission line widths of $>$ 500 km/s in more than 10% of their spaxels, only 7%
of MaNGA non-AGN show a similar signature. Even the AGN that do not show
nuclear AGN photoionisation signatures and that were only identified as AGN
based on their larger scale photoionisation signatures show similar kinematic
characteristics. In addition to obscuration, another possibility is that
outflow and mechanical feedback signatures are longer lived than the AGN
itself. Our measurements demonstrate that high velocity gas is more prevalent
in AGN compared to non-AGN and that outflow and feedback signatures in
low-luminosity, low-redshift AGN may so far have been underestimated. We show
that higher luminosity MaNGA-selected AGN are able to drive larger scale
outflows than lower luminosity AGN. But estimates of the kinetic coupling
efficiencies are $<$ 1% and suggest that the feedback signatures probed in this
paper are unlikely to have a significant impact on the AGN host galaxies.
However, continuous energy injection may still heat a fraction of the cool gas
and delay or suppress star formation in individual galaxies even when the AGN
is weak.

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