Gas Outflows in Radio Galaxies

Morganti, Raffaella; Oosterloo, Thomas; Emonts, B.; Tadhunter, C. N.; Holt, J.

doi:10.1017/s0074180900197876

Cited by 8 publications

(8 citation statements)

References 18 publications

(18 reference statements)

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“…Recent observations done with the new broad-band system at the WSRT have given further insight the characteristics of the absorption. These observations show that the broad absorption is much wider than measured before by Mirabel (1989), covering now a range in velocities of about 2000 km s −1 ; most of this H I absorption is blueshifted (see Morganti et al 2003a and the profile shown in Fig. 2).…”

Section: Introductionsupporting

confidence: 53%

The unfriendly ISM in the radio galaxy 4C 12.50 (PKS 1345+12)

Morganti

Oosterloo

Tadhunter

et al. 2004

A&A

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Abstract. The radio source 4C 12.50 has often been suggested to be a prime candidate for the link between ultraluminous infrared galaxies and young radio galaxies. A VLBI study of the neutral hydrogen in the nuclear regions of this object shows that most of the gas detected close to the systemic velocity is associated with an off-nuclear cloud (∼50 to 100 pc from the radio core) with a column density of ∼10 22 T spin /(100 K) cm −2 and an H I mass of a few times 10 5 to 10 6 M . We consider a number of possibilities to explain the results. In particular, we discuss the possibility that this cloud indicates the presence of a rich and clumpy interstellar medium in the centre, likely left over from the merger that triggered the activity and that this medium influences the growth of the radio source. The location of the cloud -at the edge of the northern radio jet/lobe -suggests that the radio jet might be interacting with a gas cloud. This interaction could be responsible for bending the young radio jet. The velocity profile of the gas is relatively broad (∼150 km s −1 ) and we interpret this as kinematical evidence for interaction of the radio plasma with the cloud. We also consider the model where the cloud is part of a broader circumnuclear structure. Only a limited region of this structure would have sufficient background radio brightness and large enough column depth in neutral gas to obtain detectable H I absorption against the counterjet. The VLBI study of the neutral hydrogen in 4C 12.50 suggests that H I detected near the systemic velocity (as it is often the case in radio galaxies) may not necessarily be connected with a circumnuclear disk or torus (as is very often assumed) but instead could be a tracer of the large-scale medium that surrounds the active nucleus and that may influence the growth of the young radio source.

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Section: Introductionsupporting

confidence: 53%

The unfriendly ISM in the radio galaxy 4C 12.50 (PKS 1345+12)

Morganti

Oosterloo

Tadhunter

et al. 2004

A&A

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“…The bulk H i kinetic luminosities represent about a few percent of the Eddington luminosities. This is two orders of magnitude larger than the ionized outflow kinetic power (Holt et al 2006;Morganti et al 2007Morganti et al , 2010. We will further discuss these results in Section 6.2 when examining the transfer of kinetic energy from the jet to the H i and H 2 gas.…”

Section: H I Gasmentioning

confidence: 93%

Strong Molecular Hydrogen Emission and Kinematics of the Multiphase Gas in Radio Galaxies With Fast Jet-Driven Outflows

Guillard

Ogle

Emonts

et al. 2012

ApJ

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Observations of ionized and neutral gas outflows in radio galaxies (RGs) suggest that active galactic nucleus (AGN) radio jet feedback has a galaxy-scale impact on the host interstellar medium, but it is still unclear how the molecular gas is affected. Thus, it is crucial to determine the physical conditions of the molecular gas in powerful RGs to understand how radio sources may regulate the star formation in their host galaxies. We present deep Spitzer Infrared Spectrograph (IRS) high-resolution spectroscopy of eight nearby RGs that show fast H i outflows. Strikingly, all of these H i-outflow RGs have bright H 2 mid-IR lines that cannot be accounted for by UV or X-ray heating. This strongly suggests that the radio jet, which drives the H i outflow, is also responsible for the shock excitation of the warm H 2 gas. In addition, the warm H 2 gas does not share the kinematics of the ionized/neutral gas. 4C 12.50, 3C 459, and PKS 1549-79. This shows that, contrary to the H i gas, the H 2 gas is inefficiently coupled to the AGN jet-driven outflow of ionized gas. While the dissipation of a small fraction (<10%) of the jet kinetic power can explain the turbulent heating of the molecular gas, our data show that the bulk of the warm molecular gas is not expelled from these galaxies.

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“…Tadhunter 1991;Tadhunter et al 2001;Holt et al 2003;van Bemmel et al 2003;and Morganti et al 2004, for a summary of recent results). However, it is intriguing that in several radio sources fast outflows of neutral hydrogen (up to 2000 km s −1 ) have been discovered.…”

Section: Introductionmentioning

confidence: 99%

The location of the broad H i absorption in 3C 305: clear evidence for a jet-accelerated neutral outflow

Morganti¹,

Oosterloo²,

Tadhunter

et al. 2005

A&A

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104

138

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Abstract. We present high-spatial resolution 21-cm H I VLA observations of the radio galaxy 3C 305 (z = 0.041). These new high-resolution data show that the ∼1000 km s −1 broad H  absorption, earlier detected in low-resolution WSRT observations, is occurring against the bright, eastern radio lobe, about 1.6 kpc from the nucleus. We use new optical spectra taken with the WHT to make a detailed comparison of the kinematics of the neutral hydrogen with that of the ionised gas. The striking similarity between the complex kinematics of the two gas phases suggests that both the ionised gas and the neutral gas are part of the same outflow. Earlier studies of the ionised gas had already found evidence for a strong interaction between the radio jet and the interstellar medium at the location of the eastern radio lobe. Our results show that the fast outflow produced by this interaction also contains a component of neutral atomic hydrogen. The most likely interpretation is that the radio jet ionises the ISM and accelerates it to the high outflow velocities observed. Our observations demonstrate that, following this strong jet-cloud interaction, not all gas clouds are destroyed and that part of the gas can cool and become neutral. The mass outflow rate measured in 3C 305 is comparable, although at the lower end of the distribution, to that found in Ultra-Luminous IR galaxies. This suggests that AGN-driven outflows, and in particular jet-driven outflows, can have a similar impact on the evolution of a galaxy as starburst-driven superwinds.

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Gas Outflows in Radio Galaxies

Cited by 8 publications

References 18 publications

The unfriendly ISM in the radio galaxy 4C 12.50 (PKS 1345+12)

The unfriendly ISM in the radio galaxy 4C 12.50 (PKS 1345+12)

Strong Molecular Hydrogen Emission and Kinematics of the Multiphase Gas in Radio Galaxies With Fast Jet-Driven Outflows

The location of the broad H i absorption in 3C 305: clear evidence for a jet-accelerated neutral outflow

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