Galaxy-scale outflows driven by active galactic nuclei

DeBuhr, Jackson; Quataert, Eliot; Pei, Chung

doi:10.1111/j.1365-2966.2011.20187.x

Cited by 192 publications

(283 citation statements)

References 41 publications

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“…Fig. 2 shows the mass of the black hole at the time the BHAR reaches its maximum value as function of the stellar velocity dispersion of the resulting elliptical galaxy, on how to calculate the latter we refer to Debuhr et al (2011). The results are consistent with the observed correlation from Gültekin et al (2009) indicated by the solid line.…”

Section: T H E G E N E R a L P I C T U R Esupporting

confidence: 74%

“…Here we use v w = 10 4 km s −1 following Debuhr et al (2012). As thus not all of the mass that is made available by the accretion disc enters the black hole, its accretion rate must be reduced accordinglẏ…”

Section: Agn Feedbackmentioning

confidence: 99%

“…Debuhr et al (2011Debuhr et al ( , 2012, Di Matteo et al (2005), we furthermore limit the black hole accretion rate to the Eddington limiṫ (Eddington 1921). Here M BH is the black hole mass and τ S = η × 4.5 × 10 8 yr the Salpeter time-scale (Salpeter 1964).…”

Section: Agn Feedbackmentioning

confidence: 99%

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Viscous time lags between starburst and AGN activity

Blank

Duschl

2016

Mon. Not. R. Astron. Soc.

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There is strong observational evidence indicating a time lag of order of some 100 Myr between the onset of starburst and AGN activity in galaxies. Dynamical time lags have been invoked to explain this. We extend this approach by introducing a viscous time lag the gas additionally needs to flow through the AGN's accretion disc before it reaches the central black hole. Our calculations reproduce the observed time lags and are in accordance with the observed correlation between black hole mass and stellar velocity dispersion.Key words: galaxies: active -galaxies: formation -galaxies: interactions -galaxies: nucleiquasars: general -galaxies: starburst. I N T RO D U C T I O NMotivated by, for instance, observed correlations between the mass of an AGN's central black hole and the host galaxy's velocity dispersion (e.g. Gebhardt et al. 2000) and between black hole mass and bulge mass (e.g. Kormendy & Richstone 1995), there is an ongoing debate whether, and if so, how starbursts and AGN are connected to each other.Di , for instance, explain such correlations as due to a thermal AGN feedback that heats the gas of the galaxy and thus prevents further star formation and AGN activity: more massive galaxies have a deeper gravitational potential well, thus the black hole has to gain more mass before its luminosity is capable of expelling the gas from the galaxy and quenching star formation and AGN activity. This then leads to the velocity dispersion and the bulge mass, respectively, to be related to the black hole mass. In these simulations starburst and AGN activity occur simultaneously, but recent observations show that AGN activity may be delayed with regard to star formation activity by time-scales of 50-250 Myr (e.g. Davies et al. 2007;Schawinski et al. 2009;Wild, Heckman & Charlot 2010).Hopkins (2012) argues that such a time lag can occur for purely dynamical reasons. His high spatial resolution simulations of galaxy mergers show first an inward motion of gas towards the dynamical centre giving rise to (a burst of) star formation. In these models, the gas flowing further inwards can do so only by losing angular momentum by gravitational instabilities. This, in turn, gives rise to a time lag between star formation and AGN activity.We extend this idea by modelling the loss of angular momentum and the ensuing inflow in the framework of an accretion disc scenario. Thus the time lag between starburst and AGN activity consists of a dynamical lag given by the time span the gas needs to E-mail: mblank@astrophysik.uni-kiel.de reach the accretion disc and a subsequent viscous lag given by the time span the gas needs to flow through the accretion disc until it reaches the black hole.In Section 2 we explain our numerical methods and the setup of the merger event that is, in this scenario, responsible for the inflow of gas to the newly forming galactic centre. In Section 3 we present and discuss the general picture that results from our calculations. As our model depends on a number of parameters, we perform a parameter stud...

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Section: T H E G E N E R a L P I C T U R Esupporting

confidence: 74%

Section: Agn Feedbackmentioning

confidence: 99%

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Viscous time lags between starburst and AGN activity

Blank

Duschl

2016

Mon. Not. R. Astron. Soc.

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“…The formation of active galaxy nucleus (AGN) and the associated feedback is intensively discussed, as well as the pairing of black holes in mergers (see e.g. Lagos et al, 2008;Narayanan et al, 2008;Blecha et al, 2011;Debuhr et al, 2011;Sijacki et al, 2011, among many others).…”

Section: Forty Years Of Numerical Simulationsmentioning

confidence: 99%

Tides in Colliding Galaxies

Duc

Renaud

2013

Tides in Astronomy and Astrophysics

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Long tails and streams of stars are the most noticeable upshots of galaxy collisions. Their origin as gravitational, tidal, disturbances has however been recognized only less than fifty years ago and more than ten years after their first observations. This Review describes how the idea of galactic tides emerged, in particular thanks to the advances in numerical simulations, from the first ones that included tens of particles to the most sophisticated ones with tens of millions of them and state-of-the-art hydrodynamical prescriptions. Theoretical aspects pertaining to the formation of tidal tails are then presented. The third part of the review turns to observations and underlines the need for collecting deep multi-wavelength data to tackle the variety of physical processes exhibited by collisional debris. Tidal tails are not just stellar structures, but turn out to contain all the components usually found in galactic disks, in particular atomic / molecular gas and dust. They host star-forming complexes and are able to form star-clusters or even second-generation dwarf galaxies. The final part of the review discusses what tidal tails can tell us (or not) about the structure and content of present-day galaxies, including their dark components, and explains how tidal tails may be used to probe the past evolution of galaxies and their mass assembly history. On-going deep wide-field surveys disclose many new lowsurface brightness structures in the nearby Universe, offering great opportunities for attempting galactic archeology with tidal tails.

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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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Galaxy-scale outflows driven by active galactic nuclei

Cited by 192 publications

References 41 publications

Viscous time lags between starburst and AGN activity

Viscous time lags between starburst and AGN activity

Tides in Colliding Galaxies

Starburst–AGN mixing – II. Optically selected active galaxies

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