Radio jets in NGC 4151: where eMERLIN meets HST

Williams, D.; McHardy, I. M.; Baldi, Ranieri D.; Beswick, R. J.; Argo, M. K.; Dullo, Bililign T.; Knapen, Johan H.; Brinks, E.; Fenech, Danielle; Mundell, C. G.; Muxlow, T. W. B.; Panessa, F.; Rampadarath, H.; Westcott, Jonathan

doi:10.1093/mnras/stx2205

Cited by 37 publications

(43 citation statements)

References 76 publications

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“…The positive feedback of the jet and the central AGN on the ISM are also supported by the alignment of the radio axis with the morphology of the ELR. While what expected from a radio-mode feedback matches the emission-line properties of the LEGs, the quasar-mode feedback plays a crucial role to interpret the ELR properties of HEGs, similar to what observed in local radioquiet Seyferts/QSO (Williams et al 2017;Fischer et al 2018;Revalski et al 2018). In both the feedback modes, the gas is photoionized along the axis of the jet, where most of the ionizing photons are able to escape and most of the cold gas is shocked.…”

Section: Discussionsupporting

confidence: 62%

Hubble Space Telescope Emission-line Images of Nearby 3CR Radio Galaxies: Two Photoionization, Accretion, and Feedback Modes

Baldi

Zaurín

Chiaberge

et al. 2019

ApJ

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We present HST/ACS narrow-band images of a low-z sample of 19 3C radio galaxies to study the Hα and [O III] emissions from the narrow-line region (NLR). Based on nuclear emission line ratios, we divide the sample into High and Low Excitation Galaxies (HEGs and LEGs). We observe different line morphologies, extended line emission on kpc scale, large [O III]/Hα scatter across the galaxies, and a radio-line alignment. In general, HEGs show more prominent emission line properties than LEGs: larger, more disturbed, more luminous, and more massive regions of ionized gas with slightly larger covering factors. We find evidence of correlations between line luminosities and (radio and X-ray) nuclear luminosities. All these results point to a main common origin, the active nucleus, which ionize the surrounding gas. However, the contribution of additional photoionization mechanism (jet shocks and star formation) are needed to account for the different line properties of the two classes.A relationship between the accretion, photoionization and feedback modes emerges from this study. For LEGs (hot-gas accretors), the synchrotron emission from the jet represents the main source of ionizing photons. The lack of cold gas and star formation in their hosts accounts for the moderate ionized-gas masses and sizes. For HEGs (cold-gas accretors), an ionizing continuum from a standard disk and shocks from the powerful jets are the main sources of photoionization, with the contribution from star formation. These components, combined with the large reservoir of cold/dust gas brought from a recent merger, account for the properties of their extended emission-line regions.

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Section: Discussionsupporting

confidence: 62%

Hubble Space Telescope Emission-line Images of Nearby 3CR Radio Galaxies: Two Photoionization, Accretion, and Feedback Modes

Baldi

Zaurín

Chiaberge

et al. 2019

ApJ

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“…Prototype radio maps of RQ AGN with extended radio morphologies. Upper panel maps with arcsec resolution (from VLA) and lower panel maps with mas resolution: 8-GHz jetted structure of NGC 4151 (panel a, Pedlar et al 1993), resolved in several components (panel b) with eMERLIN (Williams et al 2017) and VLBA (Mundell et al 2003) at 1.4 GHz; Mrk 6 at 1.5 GHz (panel c, Kharb et al 2006) for an outflowing bubble-like structure resolved in smaller components with VLBA at 1. structures of RQQ are found to be larger than those of Seyfert galaxies, but with similar morphologies (Leipski et al 2006). Similarly, LINERs typically show corebrightened radio jets reminiscent of those observed in small FR Is (Capetti et al 2017).…”

Section: Jetsmentioning

confidence: 99%

The origin of radio emission from radio-quiet active galactic nuclei

et al. 2019

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The central nuclei of galaxies, where super-massive black holes (SMBHs) are thought to reside, can experience phases of activity when they become Active Galactic Nuclei (AGN). An AGN can eject winds, jets, and produce radiation across the entire electromagnetic spectrum. The fraction of the bolometric emission in the radio spans a factor of ∼10 5 across the different AGN classes. The weakest radio sources, radio-quiet (RQ) AGN, are typically 1,000 times fainter than the radio-loud (RL) AGN, and represent the majority of the AGN population. In RL AGN, radio emission is essentially all produced by synchrotron emission from a relativistic jet. In contrast, in RQ AGN the absence of luminous jets allows us to probe radio emission from a wide range of possible mechanisms, from the host galaxy kpc scale down to the innermost region near the SMBHs: star formation, AGN driven wind, free-free emission from photo-ionized gas, low power jet, and the innermost accretion disc coronal activity. All these mechanisms can now be probed with unprecedented precision and spatial resolution, thanks to the current and forthcoming generation of highly sensitive radio arrays.

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“…This result strengthens the interpretation that N2 is indeed a type 2 nucleus. In these sources, the AGN radiation field is highly asymmetric due to nuclear obscuration and, as a result, their narrow line region (NLR) often show a biconical morphology (see, e.g., Tadhunter & Tsvetanov 1989;Wilson et al 1993;Williams et al 2017). In the case of 3C 459 the bicone partly overlaps with the NLR of the radio loud AGN.…”

Section: Linementioning

confidence: 99%

The MURALES survey

Balmaverde¹,

Capetti²,

Marconi³

et al. 2018

A&A

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We observed the FR II radio galaxy 3C 459 (z = 0.22) with the MUSE spectrograph at the Very Large Telescope (VLT) as part of the MURALES project (a MUse RAdio Loud Emission line Snapshot survey). We detected diffuse nuclear emission and a filamentary ionized gas structure forming a one-sided, triangular-shaped region extending out to ∼80 kpc. The central emission line region is dominated by two compact knots of similar flux: the first (N1) cospatial with the radio core and the (N2) second located 1″.2 (5.3 kpc) to the SE. The two regions differ dramatically from the point of view of velocity (with an offset of ∼400 km s−1), line widths, and line ratios. This suggests that we are observing a dual AGN system formed by a radio loud AGN and type 2 QSO companion, which is the result of the recent merger that also produced its disturbed host morphology. The alternative possibility that N2 is just a bright emission line knot resulting from, for example, a jet-cloud interaction, is disfavored because of (1) the presence of a high ionization bicone whose apex is located at N2; (2) the observed narrow line widths; (3) its line luminosity (∼1042 erg s−1) typical of luminous QSOs; and (4) its location, which is offset from the jet path. The putative secondary AGN must be highly obscured, since we do not detect any emission in the Chandra and infrared Hubble Space Telescope images.

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Radio jets in NGC 4151: where eMERLIN meets HST

Cited by 37 publications

References 76 publications

Hubble Space Telescope Emission-line Images of Nearby 3CR Radio Galaxies: Two Photoionization, Accretion, and Feedback Modes

Hubble Space Telescope Emission-line Images of Nearby 3CR Radio Galaxies: Two Photoionization, Accretion, and Feedback Modes

The origin of radio emission from radio-quiet active galactic nuclei

The MURALES survey

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