Powerful ionized gas outflows in the interacting radio galaxy 4C+29.30

Abstract

We investigate the ionized gas excitation and kinematics in the inner 4.3 × 6.2 kpc2 of the merger radio galaxy 4C +29.30. Using optical integral field spectroscopy with the Gemini North Telescope, we present flux distributions, line-ratio maps, peak velocities and velocity dispersion maps as well as channel maps with a spatial resolution of ≈955 pc. We observe high blueshifts of up to ∼−650 $\rm km\, s^{-1}$ in a region ∼1″ south of the nucleus (the southern knot – SK), which also presents high velocity dispersions (∼250 $\rm km\, s^{-1}$), which we attribute to an outflow. A possible redshifted counterpart is observed north from the nucleus (the northern knot – NK). We propose that these regions correspond to a bipolar outflow possibly due to the interaction of the radio jet with the ambient gas. We estimate a total ionized gas mass outflow rate of $\dot{M}_{out} = 25.4 \substack{+11.5 \\-7.5}\,$M⊙ yr−1with a kinetic power of $\dot{E} = 8.1 \substack{+10.7 \\-4.0} \times 10^{42}\,$erg s−1, which represents $5.8 \substack{+7.6 \\-2.9} \%$ of the AGN bolometric luminosity. These values are higher than usually observed in nearby active galaxies with the same bolometric luminosities and could imply a significant impact of the outflows in the evolution of the host galaxy. The excitation is higher in the NK – that correlates with extended X-ray emission, indicating the presence of hotter gas – than in the SK, supporting a scenario in which an obscuring dust lane is blocking part of the AGN radiation to reach the southern region of the galaxy.

The MURALES survey

“…The final effect of the jet-ISM interaction depends on the jet power, the distribution of the surrounding medium, and its orientation with respect to the jet. In the merger radio galaxy 4C+29.30, Couto et al (2020) found a prominent outflow, with a total ionized gas mass outflow rate of 25 M yr −1 and an energy corresponding to ∼6 × 10 −2 of the AGN bolometric luminosity. A number of large-scale outflows of neutral hydrogen have been found mainly in young or restarted radio galaxies (identified by the blueshifted wings seen in HI absorption; see, e.g., Morganti et al 2003Morganti et al , 2005Morganti & Oosterloo 2018;Aditya & Kanekar 2018).…”

The Complex X-Ray Obscuration Environment in the Radio-loud Type 2 Quasar 3C 223

“…From the intrinsic (absorption-corrected) X-ray luminosity and [O III] luminosity, we estimate a radiative bolometric luminosity of ∼1-6 ×10 45 erg s −1 and an Eddington ratio of 5%, consistent with radiatively efficient accretion (Section 4.3). The bolometric luminosity, and associated Eddington ratio, calculated from the [O III] line is greater than that calculated from the X-ray luminosity, but it is unclear whether this result is due to the radio jet boosting the [O III] line luminosity (van Breugel et al 1986;Siemiginowska et al 2012;Couto et al 2020) or whether an inner, heavily Compton-thick ring of obscuration is causing the intrinsic X-ray luminosity deduced by the MYTORUS model to be underpredicted. The amount of kinetic energy carried by the jet (2.1 × 10 45 erg s −1 ) is comparable to that of the radiatively bolometric luminosity (Section 4.4).…”

BASS XXVI: DR2 Host Galaxy Stellar Velocity Dispersions

“…The two outlier Sy 2 systems are likewise unique, with the presence of strong outflows or double-peaked narrow emission lines. Recent, optical integral field spectroscopy with the Gemini North Telescope (Couto et al 2020) for 4C+29.30 (BAT ID=426) indicated a large southern knot 1 south of the nucleus (and hence in the 3 SDSS fiber), which also presents high velocity dispersions (∼250 km s −1 ) attributed to an outflow. The other Sy 2 outlier, SDSS J000911.58-003654.7 (BAT ID=7), shows double-peaked narrow emission lines, and five nearby galaxies within 30 at similar redshift (< 500 km s −1 ), indicative of a galaxy group.…”