Fueling the central engine of radio galaxies

Labiano, Á.; García‐Burillo, S.; Combes, F.; Usero, A.; Soria-Ruiz, R.; López, Javier Piqueras; Fuente, A.; Hunt, L. K.; Neri, R.

doi:10.1051/0004-6361/201323123

Cited by 22 publications

(28 citation statements)

References 136 publications

(200 reference statements)

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“…This should not be of any surprise, however, since the analysed system is rich in warm and cold molecular gas, with the total masses of 3.7 × 10 9 M and 2.2 × 10 10 M , respectively (Ogle et al 2010;Labiano et al 2014). Importantly, this gas is distributed along the extended warped disk, which rotates around the galactic centre.…”

Section: The Accretion Powermentioning

confidence: 79%

Dynamical analysis of the complex radio structure in 3C 293: clues on a rapid jet realignment in X-shaped radio galaxies

Machalski

Jamrozy

Stawarz

et al. 2016

A&A

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Context. Radio galaxies classified as X-shaped/winged, are characterised by two pairs of extended and misaligned lobes, which suggest a rapid realignment of the jet axis, for which a potential cause (including binary supermassive black holes, a black hole merger, or a Lense-Thirring precession) is still under debate. Aims. Here we analyse the complex radio structure of 3C 293 winged source hosted by the post-merger galaxy UGC 8782, which uniquely displays a significant asymmetry between the sizes (and therefore the ages) of the two pairs of lobes, indicating that an episode of jet realignment took place only very recently. This allows us to tightly constrain the corresponding timescales, and therefore to discriminate between different models proposed for the formation of X-shaped radio galaxies in general.Methods. Based on all the available and carefully re-analysed radio data for 3C 293, we have performed a detailed spectral modelling for the older and younger lobes in the system, using the existing evolutionary DYNAGE algorithm. In this way we derived the lobes' ages and jet energetics, which we then compared to the accretion power in the source. Results. We found that the 200 kpc-scale outer lobes of 3C 293 are ∼ 60 Myr old and, until very recently, have been supplied with fresh electrons and magnetic field by the jets, i.e., jet activity related to the formation of the outer lobes ceased within the last Myr. Meanwhile, the inner 4 kpc-scale lobes, tilted by ∼ 40• with respect to the outer ones, are only about ∼ 0.3 Myr old. Interestingly, the best model fits also return identical values of the jet power supplying the outer and the inner structures. This power, moreover, is of the order of the maximum kinetic luminosity of a Blandford-Znajek jet for a given black hole mass and accretion rate, but only in the case of relatively low values of a black hole spin, a ∼ 0.2. Conclusions. The derived jet energetics and timescales, along with the presence of two optical nuclei in UGC 8782, all provide a strong support to the Lense-Thirring precession model in which the supermassive black hole spin, and therefore the jet axis, flips rapidly owing to the interactions with the tilted accretion disk in a new tidal interaction episode of the merging process. We further speculate that, in general, X-shape radio morphology forms in post-merger systems that are rich in cold molecular gas, and only host slowly spinning supermassive black holes.

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Section: The Accretion Powermentioning

confidence: 79%

Dynamical analysis of the complex radio structure in 3C 293: clues on a rapid jet realignment in X-shaped radio galaxies

Machalski

Jamrozy

Stawarz

et al. 2016

A&A

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“…Such large line-widths in the off-nuclear regions are inconsistent with the normal gravitation motions of gas in the disk of a galaxy (i.e. Labiano et al 2014 show that the kinematics of the inner 7 kpc CO disk are consistent with rotation around the core). Thus, the 2 The line-widths have been corrected for the instrumental width long-slit results confirm what was seen in the IFU observations in the sense that they show that the disturbed emission line kinematics have a significant extent perpendicular to the radio axis.…”

Section: Comparison With Long-slit Datamentioning

confidence: 91%

“…To confirm this, follow-up Xray observations revealed 10 7 K shock-heated gas in both the nucleus and the inner radio jets, again driven by jet-induced shocks (Lanz et al 2015). Studies of the cold molecular gas in this galaxy indicate a cold H 2 mass of 2.2×10 10 M and a starformation rate of 4 M yr −1 (Evans et al 1999;Labiano et al 2014). The outflows detected in HI and ionised gas have not yet been detected in CO, however, Labiano et al (2014) derive a 3σ upper limit of the molecular gas outflow of 3.2% of the total H2 mass.…”

Section: Introductionmentioning

confidence: 93%

“…Studies of the cold molecular gas in this galaxy indicate a cold H 2 mass of 2.2×10 10 M and a starformation rate of 4 M yr −1 (Evans et al 1999;Labiano et al 2014). The outflows detected in HI and ionised gas have not yet been detected in CO, however, Labiano et al (2014) derive a 3σ upper limit of the molecular gas outflow of 3.2% of the total H2 mass. This limit can rule out an extreme molecular outflow like that observed in Mrk 231 (Feruglio et al 2010), but it is within the range observed in other objects with molecular outflows (e.g.…”

Section: Introductionmentioning

confidence: 93%

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Jet-driven outflows of ionized gas in the nearby radio galaxy 3C 293

Mahony

Oonk

Morganti

et al. 2015

Mon. Not. R. Astron. Soc.

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Fast outflows of gas, driven by the interaction between the radio-jets and ISM of the host galaxy, are being observed in an increasing number of galaxies. One such example is the nearby radio galaxy 3C293. In this paper we present Integral Field Unit (IFU) observations taken with OASIS on the William Herschel Telescope (WHT), enabling us to map the spatial extent of the ionised gas outflows across the central regions of the galaxy. The jet-driven outflow in 3C293 is detected along the inner radio lobes with a mass outflow rate ranging from ∼ 0.05−0.17 M yr −1 (in ionised gas) and corresponding kinetic power of ∼ 0.5−3.5× 10 40 erg s −1 . Investigating the kinematics of the gas surrounding the radio jets (i.e. not directly associated with the outflow), we find line-widths broader than 300 km s −1 up to 5 kpc in the radial direction from the nucleus (corresponding to 3.5 kpc in the direction perpendicular to the radio axis at maximum extent). Along the axis of the radio jet line-widths > 400 km s −1 are detected out to 7 kpc from the nucleus and line-widths of > 500 km s −1 at a distance of 12 kpc from the nucleus, indicating that the disturbed kinematics clearly extend well beyond the high surface brightness radio structures of the jets. This is suggestive of the cocoon structure seen in simulations of jet-ISM interaction and implies that the radio jets are capable of disturbing the gas throughout the central regions of the host galaxy in all directions.

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“…To obtain a complete picture of the kinematics and physics behind this jet-ISM iteraction, the next step would be to search for outflows of molecular gas. Unfortunately no significant outflows of molecular gas have been detected in this object to date (Labiano et al 2014). …”

Section: New Observationsmentioning

confidence: 93%

Evidence for jet driven outflows: the case of 3C293

et al. 2014

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The tight correlations observed between galaxies and their SMBH provides compelling evidence that the evolution of the galaxy and its central black hole are strongly linked. This is generally attributed to feedback mechanisms which, according to simulations, often take the form of outflows of gas, quenching star formation in the host galaxy and halting accretion onto the central black hole. While there are a number of plausible ways that outflows could be produced, recent results have shown that in some cases radio jets could be responsible for driving fast outflows of gas. One such example is seen in the nearby radio galaxy 3C293. In this talk I will present results from JVLA radio observations where we detect fast outflows (∼1200 km/s) of neutral gas which are being driven by the radio-jet approximately 0.5 kpc from the central core, providing direct evidence for jet-ISM interaction. This is accompanied with recent IFU observations showing that ionised gas outflows are also being driven by the radio jet. Pinpointing the location of these outflows enables us to derive crucial parameters, such as the mass outflow rates and kinetic energy involved, which we can compare to predictions from galaxy evolution simulations.

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Fueling the central engine of radio galaxies

Cited by 22 publications

References 136 publications

Dynamical analysis of the complex radio structure in 3C 293: clues on a rapid jet realignment in X-shaped radio galaxies

Dynamical analysis of the complex radio structure in 3C 293: clues on a rapid jet realignment in X-shaped radio galaxies

Jet-driven outflows of ionized gas in the nearby radio galaxy 3C 293

Evidence for jet driven outflows: the case of 3C293

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