Dense gas without star formation: the kpc-sized turbulent molecular disk in 3C 326 N

Nesvadba, N. P. H.; Boulanger, F.; Lehnert, M. D.; Guillard, P.; Salomé, P.

doi:10.1051/0004-6361/201118018

Cited by 58 publications

(86 citation statements)

References 41 publications

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“…Disks with low v/σ values that are highly turbulent and not gravitationally bound have been studied in a few individual cases at low redshift (Alatalo et al 2011;Nesvadba et al 2011a), and are characterized by large line widths and complex line profiles as we find here. These disks are very different from classical thin disks, for example, in spiral galaxies.…”

Section: Random Motion and Kinetic Energysupporting

confidence: 70%

“…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?supporting

confidence: 51%

“…They are thus in principle able to offset the excess cooling out to the highest galaxy masses (Silk & Rees 1998). If sufficiently large parts of this energy are deposited in the interstellar medium (ISM) of the host galaxy, they may drive winds (Di Matteo et al 2005) or turbulence (Nesvadba et al 2011a). The mechanisms that cause this, however, are still not very well understood.…”

Section: Introductionmentioning

confidence: 99%

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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: Random Motion and Kinetic Energysupporting

confidence: 70%

Section: Outflows or Disk Rotation?supporting

confidence: 51%

Section: Introductionmentioning

confidence: 99%

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

Collet

Nesvadba

Breuck

et al. 2016

A&A

Self Cite

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“…It shows evidence of molecular reservoirs thought to be formed by positive feedback (Nesvadba et al 2011). …”

Section: C 192 (Pks 0802+24mentioning

confidence: 99%

The link between accretion mode and environment in radio-loud active galaxies

Ineson

Croston

Hardcastle

et al. 2015

Mon. Not. R. Astron. Soc.

130

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The interactions between radio-loud AGN and their environments play an important rôle in galaxy and cluster evolution. Recent work has demonstrated fundamental differences between High and Low Excitation Radio Galaxies (HERGs and LERGs), and shown that they may have different relationships with their environments. In the Chandra Large Project ERA (Environments of Radio-loud AGN), we made the first systematic X-ray environmental study of the cluster environments of radio galaxies at a single epoch (z ∼ 0.5), and found tentative evidence for a correlation between radio luminosity and cluster X-ray luminosity. We also found that this relationship appeared to be driven by the LERG sub-population (Ineson et al. 2013).We have now repeated the analysis with a low redshift sample (z ∼ 0.1), and found strong correlations between radio luminosity and environment richness and between radio luminosity and central density for the LERGs but not for the HERGs. These results are consistent with models in which the HERGs are fuelled from accretion discs maintained from local reservoirs of gas, while LERGs are fuelled more directly by gas ingested from the intra-cluster medium.Comparing the samples, we found that although the maximum environment richness of the HERG environments is similar in both samples, there are poorer HERG environments in the z ∼ 0.1 sample than in the z ∼ 0.5 sample. We have therefore tentative evidence of evolution of the HERG environments. We found no differences between the LERG subsamples for the two epochs, as would be expected if radio and cluster luminosity are related.

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“…However, starformation can also be quenched or suppressed through powerful galaxy-scale outflows driven by energy released during AGN accretion (e.g. Di Springel et al 2005;Bower et al 2006;Croton et al 2006;Schawinski et al 2007;Nesvadba et al 2010;DeBuhr et al 2012;Maiolino et al 2012;Karouzos et al 2014). A large number of AGN host galaxies lie in the 'Green Valley' of the galaxy colour-magnitude diagram (e.g.…”

Section: Introductionmentioning

confidence: 99%

Starburst–AGN mixing – II. Optically selected active galaxies

Davies

Kewley

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We use 4 galaxies from the Calar Alto Legacy Integral Field Area (CALIFA) survey with clear signs of accretion onto supermassive black holes to investigate the relative contribution of star-formation and active galactic nucleus (AGN) activity to the lineemission of each galaxy as a function of radius. The combination of star-formation and AGN activity produces curved "mixing sequences" on standard optical diagnostic diagrams, and the fraction of emission due to AGN activity decreases smoothly with distance from the centre of the galaxy. We use the AGN activity profiles to calculate the size of the AGN narrow line regions, which have radii of ∼ 6.3 kpc. We calculate the fractional contribution of the star-formation and the AGN activity to the global Hα, [O II] λλ 3727,3729 and [O III] λ 5007 luminosities of each galaxy, and show that both ionization sources contribute significantly to the emission in all three lines. We use weighted combinations of stellar and AGN photoionization models to produce mixing models, which are consistent with observations for 85 percent of spaxels across the galaxies in our sample. We also present a new diagnostic for starburst-AGN mixing which requires only the [O II], [O III] and Hβ emission lines, and can therefore be used to calculate AGN fractions up to z ∼ 0.85 in the optical and z ∼ 3.5 in the nearinfrared. We anticipate that this diagnostic will facilitate studies of the properties of AGN ionizing radiation fields and the relative optical contribution of star-formation and AGN activity over cosmic time.

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Dense gas without star formation: the kpc-sized turbulent molecular disk in 3C 326 N

Cited by 58 publications

References 41 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

The link between accretion mode and environment in radio-loud active galaxies

Starburst–AGN mixing – II. Optically selected active galaxies

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