Ionized gas outflow signatures in SDSS-IV MaNGA active galactic nuclei

Abstract

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 ∼ 0.05 observed by SDSS-IV MaNGA. Specifically, we measure the kinematics of the [OIII] λ5007Å 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 −1 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.

Chemical abundances in Seyfert galaxies – V. The discovery of shocked emission outside the AGN ionization axis

“…C1 and C2) indicate that the presence of outflows not only along the ionization axis, but also in locations away from it. Values of 80 500 km s −1 are commonly interpreted as tracers of AGN outflows (Zakamska & Greene 2014;Kakkad et al 2020;Wylezalek et al 2020). For Mrk 79, the highest 80 values are observed perpendicular to the AGN ionization axis, which is indicated as a continuous line in the 80 map of Fig.…”

Super

“…Harrison et al 2016) and is a conservative estimate when compared to the cuts used in other works (e.g. 500 km s −1 in Wylezalek et al 2020).…”

“…The KASHz sample is matched in redshift (z ∼ 2.0-2.5) to the SUPER sample. For comparison, we also plotted the w 80 distribution of low-redshift massmatched sample of MANGA galaxies from Wylezalek et al (2020), which is shown in blue in Fig. 3.…”

“…The Type 1 sample used in this paper has a median hard X-ray luminosity of 10 44.8 erg s −1 and the redshift-matched KASHz targets have a median X-ray luminosity of 10 43.9 erg s −1 . The blue histogram shows the w 80 distribution of massmatched low redshift star forming sample fromWylezalek et al (2020), while the ocean-blue vertical bar shows the w 80 value from the redshift and mass-matched star forming sample from the KLEVER survey (334 ± 35 km s −1 ,Curti et al 2020). The dashed black-line at 600 km s −1 corresponds to the w 80 value used in this work to define if a target hosts an AGN-driven outflow.…”

The physical properties and impact of AGN outflows from high to low redshift

“…Studies of z < 1 AGN from SDSS (e.g. Mullaney et al 2013;Woo et al 2016) and MaNGA (Wylezalek et al 2020) have shown that ionised outflows are ubiquitous, that their fraction is higher in AGN than in inactive galaxies and that it increases with AGN luminosity and/or Eddington ratio. Despite their widespread presence, their global effect on SFR in the host does not seem to be significant (e.g.…”