OUTFLOWS FROM ACTIVE GALACTIC NUCLEI: KINEMATICS OF THE NARROW-LINE AND CORONAL-LINE REGIONS IN SEYFERT GALAXIES<sup>,</sup>

Müller–Sánchez, F.; Prieto, M. A.; Hicks, E. K. S.; Vives-Arias, H.; Davies, R. I.; Malkan, M. A.; Tacconi, L. J.; Genzel, R.

doi:10.1088/0004-637x/739/2/69

Cited by 282 publications

(423 citation statements)

References 140 publications

(197 reference statements)

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“…Although our sources do have extended lower surfacebrightness line emission with more quiescent kinematics, their contribution to the integrated line profile is smaller, and this gas is outside the region where a connection with the radio source is obvious (Villar-Martín et al 2003). In quasars and Seyfert galaxies at low redshift, Husemann et al (2013) and Müller-Sánchez et al (2011) also find that the gas is only perturbed near the radio source, in broad agreement with our findings (but see Liu et al 2013). …”

Section: Comparison With Other Massive High-z Galaxiessupporting

confidence: 88%

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: Comparison With Other Massive High-z Galaxiessupporting

confidence: 88%

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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“…Müller Sánchez et al (2006) argue that coronal line emission stems from the inner NLR and that they are probably associated with outflows. Recently, Müller-Sánchez et al (2011) and Mazzalay et al (2013a) observed extended emission in the coronal lines of NGC 1068, as well as a great complexity in the morphology and kinematics. This indicates that the nature of coronal line emission is far from being understood.…”

Section: Emission-line Fitsmentioning

confidence: 99%

A low-luminosity type-1 QSO sample

Busch

Smajić

Scharwächter

et al. 2015

A&A

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Circumnuclear star formation and active galactic nucleus (AGN) feedback is believed to play a critical role in galaxy evolution. The low-luminosity quasi-stellar object (LLQSO) sample that contains 99 of the closest AGN with redshift z ≤ 0.06 fills the gap between the local AGN population and high-redshift QSOs that is essential to understand the AGN evolution with redshift. In this paper, we present the results of the near-infrared H-and K-integral field spectroscopy of the inner kiloparsecs of the LLQSO HE 1029-1831 with SINFONI. Line maps show that ionized hydrogen gas is located in spiral arms within the stellar bar and in a circumnuclear ring. Line fluxes and diagnostic line ratios indicate recent or ongoing star formation in the circumnuclear region and the presence of young and intermediate-age stellar populations in the bulge. In particular, we find traces of an intense starburst in the circumnuclear region that has begun around 100 Myr ago but has declined to a fraction of the maximum intensity now. We estimate the dynamical bulge mass and find that the galaxy follows published M BH −M bulge relations. However, bulge-disk decomposition of the K-band image with B reveals that HE 1029-1831 does not follow the M BH −L bulge relations of inactive galaxies. We conclude that the deviation from M BH −L bulge relations of inactive galaxies in this source is instead caused by young stellar populations and not by an undermassive black hole.

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“…However, a significant fraction of early-type massive galaxies have a substantial amount of warm neutral and cold molecular gas Crocker et al 2012;Serra et al 2012;Bayet et al 2013), so simple energy arguments may not be enough. To inhibit star formation and efficient AGN fueling, many observational studies of AGN feedback have focused on outflows (Fischer et al 2010;Feruglio et al 2010;Dasyra & Combes 2012;Müller-Sánchez et al 2011;Sturm et al 2011;Combes et al 2013;Labiano et al 2013;Alatalo et al 2014c;Morganti et al 2013a;Mahony et al 2013;McNamara et al 2014). Spectroscopic observations of ionized, neutral, and molecular gas suggest that winds are ubiquitous in galaxies hosting AGN (e.g., Morganti et al 2005b;Lehnert et al 2011;Dasyra & Combes 2011;Alatalo et al 2011;Guillard et al 2012;Cicone et al 2014;Förster Schreiber et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Exceptional AGN-driven turbulence inhibits star formation in the 3C 326N radio galaxy

Guillard

Boulanger

Lehnert

et al. 2015

A&A

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We detect bright [Cii]λ158 μm line emission from the radio galaxy 3C 326N at z = 0.09, which shows no sign of ongoing or recent star formation (SFR < 0.07 M yr −1 ) despite having strong H 2 line emission and a substantial amount of molecular gas (2 × 10 9 M , inferred from the modeling of the far-infrared (FIR) dust emission and the CO(1−0) line emission). The [Cii] line is twice as strong as the 0−0S(1) 17 μm H 2 line, and both lines are much in excess of what is expected from UV heating. We combine infrared Spitzer and Herschel photometry and line spectroscopy with gas and dust modeling to infer the physical conditions in the [Cii]-emitting gas. The [Cii] line, like rotational H 2 emission, traces a significant fraction (30 to 50%) of the total molecular gas mass. This gas is warm (70 < T < 100 K) and at moderate densities 700 < n H < 3000 cm [Cii] is similar to the profiles of the near-infrared H 2 lines and the Na D optical absorption lines, and is likely to be shaped by a combination of rotation, outflowing gas, and turbulence. If the line wing is interpreted as an outflow, the mass loss rate would be higher than 20 M yr −1 , and the depletion timescale close to the orbital timescale (≈3 × 10 7 yr). If true, we are observing this object at a very specific and brief time in its evolution, assuming that the disk is not replenished. Although there is evidence of an outflow in this source, we caution that the outflow rates may be overestimated because the stochastic injection of turbulent energy on galactic scales can create short-lived, large velocity increments that contribute to the skewness of the line profile and mimic outflowing gas. The gas physical conditions raise the issue of the heating mechanism of the warm gas, and we show that the dissipation of turbulent energy is the main heating process. Cosmic rays can also contribute to the heating, but cannot be the dominant heating source because it requires an average gas density that is higher than the observational constraints. After subtracting the contribution of the disk rotation, we estimate the turbulent velocity dispersion of the molecular gas to be 120 < σ turb < 330 km s −1 , which corresponds to a turbulent heating rate that is higher than the gas cooling rate computed from the line emission. The dissipation timescale of the turbulent energy (2 × 10 7 −10 8 yrs) is comparable to or larger than the jet lifetime or the dynamical timescale of the outflow, which means that turbulence can be sustained during the quiescent phases when the radio jet is shut off. The strong turbulent support maintains a very high gas scale height (0.3 to 4 kpc) in the disk. The cascade of turbulent energy can inhibit the formation of gravitationally bound structures on all scales, which offers a natural explanation for the lack of ongoing star formation in 3C 326N, despite its having sufficient molecular gas to form stars at a rate of a few solar mass per year. To conclude, the bright [Cii] line indicates that strong AGN jet-driven turbulence may play a key ...

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OUTFLOWS FROM ACTIVE GALACTIC NUCLEI: KINEMATICS OF THE NARROW-LINE AND CORONAL-LINE REGIONS IN SEYFERT GALAXIES^,

Cited by 282 publications

References 140 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

A low-luminosity type-1 QSO sample

Exceptional AGN-driven turbulence inhibits star formation in the 3C 326N radio galaxy

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OUTFLOWS FROM ACTIVE GALACTIC NUCLEI: KINEMATICS OF THE NARROW-LINE AND CORONAL-LINE REGIONS IN SEYFERT GALAXIES,

Cited by 282 publications

References 140 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

A low-luminosity type-1 QSO sample

Exceptional AGN-driven turbulence inhibits star formation in the 3C 326N radio galaxy

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Resources

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OUTFLOWS FROM ACTIVE GALACTIC NUCLEI: KINEMATICS OF THE NARROW-LINE AND CORONAL-LINE REGIONS IN SEYFERT GALAXIES^,