A jet-induced outflow of warm gas in 3C 293

Emonts, B.; Morganti, Raffaella; Tadhunter, C. N.; Oosterloo, Thomas; Holt, J.; Hulst, van der Thijs

doi:10.1111/j.1365-2966.2005.09354.x

Cited by 89 publications

(133 citation statements)

References 67 publications

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“…7), and within the stellar mass range of powerful HzRGs of a few 10 11 M (Seymour et al 2007;De Breuck et al 2010). Moreover, the existence of kpc-scale rotating disks in a few lowredshift radio galaxies (e.g., Emonts et al 2005;Nesvadba et al 2011a) suggests that disk rotation is very possible in galaxies with radio sources not much weaker than we find here.…”

Section: Outflows or Disk Rotation?contrasting

confidence: 46%

Kinematic signatures of AGN feedback in moderately powerful radio galaxies atz~ 2 observed with SINFONI

Collet

Nesvadba

Breuck

et al. 2016

A&A

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Most successful galaxy formation scenarios now postulate that the intense star formation in massive, high-redshift galaxies during their major growth period was truncated when powerful AGNs launched galaxy-wide outflows of gas that removed large parts of the interstellar medium. SINFONI imaging spectroscopy of the most powerful radio galaxies at z ∼ 2 show clear signatures of such winds, but are too rare to be good representatives of a generic phase in the evolution of all massive galaxies at high redshift. Here we present SINFONI imaging spectroscopy of the rest-frame optical emission-line gas in 12 radio galaxies at redshifts ∼2. Our sample spans a range in radio power that is intermediate between the most powerful radio galaxies with known wind signatures at these redshifts and vigorous starburst galaxies, and are about two orders of magnitude more common than the most powerful radio galaxies. Thus, if AGN feedback is a generic phase of massive galaxy evolution for reasonable values of the AGN duty cycle, these are just the sources where AGN feedback should be most important. Our sources show a diverse set of gas kinematics ranging from regular velocity gradients with amplitudes of Δv = 200−400 km s −1 consistent with rotating disks to very irregular kinematics with multiple velocity jumps of a few 100 km s −1 . Line widths are generally high, typically around FWHM = 800 km s −1 , more similar to the more powerful high-z radio galaxies than mass-selected samples of massive high-z galaxies without bright AGNs, and consistent with the velocity range expected from recent hydrodynamic models. A broad Hα line in one target implies a black hole mass of a few 10 9 M . Velocity offsets of putative satellite galaxies near a few targets suggest dynamical masses of a few 10 11 M for our sources, akin to the most powerful high-z radio galaxies. Ionized gas masses are 1−2 orders of magnitude lower than in the most powerful radio galaxies, and the extinction in the gas is relatively low, up to A V ∼ 2 mag. The ratio of line widths, σ, to bulk velocity, v, is so large that even the gas in galaxies with regular velocity fields is unlikely to be gravitationally bound. It is unclear, however, whether the large line widths are due to turbulence or unresolved, local outflows as are sometimes observed at low redshifts. We compare our sources with sets of radio galaxies at low and high redshift, finding that they may have more in common with gas-rich nearby radio galaxies with similar jet power than with the most powerful high-z radio galaxies. Comparison of the kinetic energy with the energy supply from the AGNs through jet and radiation pressure suggests that the radio source still plays a dominant role for feedback, consistent with low-redshift radio-loud quasars.

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Section: Outflows or Disk Rotation?contrasting

confidence: 46%

Kinematic signatures of AGN feedback in moderately powerful radio galaxies atz~ 2 observed with SINFONI

Collet

Nesvadba

Breuck

et al. 2016

A&A

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“…We have chosen 3C293 because it has particularly luminous CO line emission (Evans et al 1999, and unlike 3C 326) and with CO line ratios suggesting the molecular gas is highly excited (Papadopoulos et al 2008). It also has a significant outflow of neutral gas Emonts et al 2005). Its H 2 emission-line luminosity, warm molecular gas mass and optical line ratios are very similar to those of 3C 326 N (Ogle et al 2010), which suggests that 3C 293 may be a "gas-rich analog" and thus a foil of 3C 326 N.…”

Section: Implications Of This Scenario For Galaxy Evolutionmentioning

confidence: 99%

“…Observationally, a picture is emerging where radio jets may play a large role in transforming the energy ejected by the AGN into kinetic and thermal energy of the interstellar medium of the host galaxy. Observations of radio-loud AGN (e.g., Heckman et al 1991b,a;Morganti et al 2005;Emonts et al 2005;Best et al 2005Best et al , 2006Nesvadba et al 2006Nesvadba et al , 2007McNamara & Nulsen 2007;Nesvadba et al 2008;Holt et al 2008;Baldi & Capetti 2008;Fu & Stockton 2009;Humphrey et al 2009) and a large number of hydrodynamical simulations (e.g., Krause 2005;Saxton et al 2005;Heinz et al 2006;Sutherland & Bicknell 2007;Merloni & Heinz 2007;Antonuccio-Delogu & Silk 2008) suggest that radio-loud AGN inject a few percent of their mechanical energy into the ambient gas, parts of which produce significant outflows of warm gas Emonts et al 2005;Nesvadba et al 2006Nesvadba et al , 2007Holt et al 2008;Nesvadba et al 2008;Fu & Stockton 2009). However, most previous studies focused on the warm and hot gas at temperatures ≥10 4 K, and did not address the impact on the molecular phase, which is a A&A 521, A65 (2010) serious limitation if we want to understand how the radio-loud AGN may regulate star formation in the host galaxy.…”

Section: Introductionmentioning

confidence: 99%

Energetics of the molecular gas in the H₂luminous radio galaxy 3C 326: Evidence for negative AGN feedback

Nesvadba¹,

Boulanger²,

Salomé

et al. 2010

A&A

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232

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We present a detailed analysis of the gas conditions in the H 2 luminous radio galaxy 3C 326 N at z ∼ 0.1, which has a low starformation rate (SFR ∼ 0.07 M yr −1 ) in spite of a gas surface density similar to those in starburst galaxies. Its star-formation efficiency is likely a factor ∼10−50 lower than those of ordinary star-forming galaxies. Combining new IRAM CO emission-line interferometry with existing Spitzer mid-infrared spectroscopy, we find that the luminosity ratio of CO and pure rotational H 2 line emission is factors 10−100 lower than what is usually found. This suggests that most of the molecular gas is warm. The Na D absorption-line profile of 3C 326 N in the optical suggests an outflow with a terminal velocity of ∼−1800 km s −1 and a mass outflow rate of 30−40 M yr −1 , which cannot be explained by star formation. The mechanical power implied by the wind, of order 10 43 erg s −1 , is comparable to the bolometric luminosity of the emission lines of ionized and molecular gas. To explain these observations, we propose a scenario where a small fraction of the mechanical energy of the radio jet is deposited in the interstellar medium of 3C 326 N, which powers the outflow, and the line emission through a mass, momentum and energy exchange between the different gas phases of the ISM. Dissipation times are of order 10 7−8 yrs, similar or greater than the typical jet lifetime. Small ratios of CO and PAH surface brightnesses in another 7 H 2 luminous radio galaxies suggest that a similar form of AGN feedback could be lowering star-formation efficiencies in these galaxies in a similar way. The local demographics of radio-loud AGN suggests that secular gas cooling in massive early-type galaxies of ≥10 11 M could generally be regulated through a fundamentally similar form of "maintenance-phase" AGN feedback.

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“…Signs of massive gas outflows have been detected for ionized atomic gas (e.g., Veilleux et al 1995;Emonts et al 2005;Holt et al 2006;Müller-Sánchez et al 2006), neutral atomic gas (e.g., Morganti et al 2005;Rupke et al 2005), and molecular CO and OH gas (e.g., Curran et al 1999;Das et al 2005;García-Burillo et al 2009;Sakamoto et al 2009;Feruglio et al 2010;Fischer et al 2010;Sturm et al 2011). In this letter we present evidence for the first detection of highly turbulent motions of H 2 gas at a temperature of a few hundred Kelvin as seen with Spitzer for several local AGN.…”

Section: Introductionmentioning

confidence: 99%

Turbulent and fast motions of H₂gas in active galactic nuclei

Dasyra

Combes

2011

A&A

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Querying the Spitzer archive for optically-selected active galactic nuclei (AGN) observed in high-resolution-mode spectroscopy, we identified radio and/or interacting galaxies with highly turbulent motions of H 2 gas at a temperature of a few hundred Kelvin. Unlike all other AGN that have unresolved H 2 line profiles at a spectral resolution of ∼600, 3C 236, 3C 293, IRAS 09039+0503, MCG-2-58-22 and Mrk 463E have intrinsic velocity dispersions exceeding 200 km s −1 for at least two of the rotational S0, S1, S2, and S3 lines. In a sixth source, 4C 12.50, a blue wing was detected in the S1 and S2 line profiles, indicating the presence of a warm molecular gas component moving at −640 km s −1 with respect to the bulk of the gas at systemic velocity. Its mass is 5.2 × 10 7 M , accounting for more than one fourth of the H 2 gas at 374 K, but less than 1% of the cold H 2 gas computed from CO observations. Because no diffuse gas component of 4C 12.50 has been observed to date to be moving at more than 250 km s −1 from systemic velocity, the H 2 line wings are unlikely to be tracing gas in shock regions along the tidal tails of this merging system. They can instead be tracing gas driven by a jet or entrained by a nuclear outflow, which is known to emerge from the west nucleus of 4C 12.50. It is improbable that such an outflow, with an estimated mass loss rate of 130 M yr −1 , entirely quenches the star formation around this nucleus.

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A jet-induced outflow of warm gas in 3C 293

Cited by 89 publications

References 67 publications

Kinematic signatures of AGN feedback in moderately powerful radio galaxies atz~ 2 observed with SINFONI

Kinematic signatures of AGN feedback in moderately powerful radio galaxies atz~ 2 observed with SINFONI

Energetics of the molecular gas in the H₂luminous radio galaxy 3C 326: Evidence for negative AGN feedback

Turbulent and fast motions of H₂gas in active galactic nuclei

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A jet-induced outflow of warm gas in 3C 293

Cited by 89 publications

References 67 publications

Kinematic signatures of AGN feedback in moderately powerful radio galaxies atz~ 2 observed with SINFONI

Kinematic signatures of AGN feedback in moderately powerful radio galaxies atz~ 2 observed with SINFONI

Energetics of the molecular gas in the H2luminous radio galaxy 3C 326: Evidence for negative AGN feedback

Turbulent and fast motions of H2gas in active galactic nuclei

Contact Info

Product

Resources

About

Energetics of the molecular gas in the H₂luminous radio galaxy 3C 326: Evidence for negative AGN feedback

Turbulent and fast motions of H₂gas in active galactic nuclei