CHEERS Results from NGC 3393. II. Investigating the Extended Narrow-line Region Using Deep Chandra Observations and Hubble Space Telescope Narrow-line Imaging

Abstract

The CHandra Extended Emission Line Region Survey (CHEERS) is an X-ray study of nearby active galactic nuclei (AGN) designed to take full advantage of Chandra's unique angular resolution by spatially resolving feedback signatures and effects. In the second paper of a series on CHEERS target NGC 3393, we examine deep high-resolution Chandra images and compare them with Hubble narrow line images of [O III], [S II] and Hα, as well as previously-unpublished midultraviolet (MUV) images. We find evidence for a complex multi-phase structure in the circumnuclear ISM, with no single simple correlation between X-rays and high-ionization ([O III]/Hα-dominated) and low-ionization ([S II]-dominated) features. We also find X-ray structures ∼ 50-pc in extent, Hα evidence for gas compression, and extended MUV emission associated with the Sshaped arms that envelope the radio jets. In conjunction with existing STIS kinematics, these findings support a role for shock contributions to the feedback, driven by the radio outflows associated with the radio jets.

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. I. Spatially Resolved Mass Outflow Rates for the Seyfert 2 Galaxy Markarian 573∗ †

“…As noted by others (Schlesinger et al 2009), we do not see any evidence for shock ionization in the outflow regions (see, e.g. Schlesinger et al 2009;Maksym et al 2016Maksym et al , 2017Terao et al 2016, and references therein for dis- cussions on shocks). Our composite models qualitatively agree with the IUE UV line ratios, indicating that we are likely encompassing a significant portion of the UV emitting gas in our models and resulting outflow rates.…”

The complex jet- and bar-perturbed kinematics in NGC 3393 as revealed with ALMA and GEMINI–GMOS/IFU

“…4) correspond to the 8.4 GHz VLA map, and indicate that the gas in the S-shaped arms seems to surround both NE and SW radio lobes. This morphology, and the interaction between radio jet and ionised gas, was previously observed and analysed by Cooke et al (2000), and Maksym et al (2017).…”

Feedback from low-luminosity radio galaxies: B2 0258+35

“…In NGC 6764, the interaction between the parsec- scale radio jets and the ISM is thought to be one of the causes of subkiloparsec-scale radio bubbles (Kharb et al 2010). Maksym et al (2017) and Wang et al (2010) also find evidence, via X-ray studies, of the jet-ISM interaction shaping the inner kpc region of the host galaxies of NGC 3396 and NGC 4151, respectively. Predictions from the numerical simulations of jets expanding at an inclination to a clumpy gas disc (e.g.…”

“…Rodríguez-Ardila et al (2017) report the presence of two expanding ionised gas shells that are spatially coincident with the radio jets. Fabbiano et al (2017Fabbiano et al ( , 2018 suggest, via deep Chandra imaging and spectroscopy, that the radio jets of ESO 428-G014 give rise to ∼ 2-3 kpc extended X-ray emission along the major axis of the radio source. In NGC 6764, the interaction between the parsec- scale radio jets and the ISM is thought to be one of the causes of subkiloparsec-scale radio bubbles (Kharb et al 2010).…”