A Close Look at Star Formation around Active Galactic Nuclei

Davies, R. I.; Sánchez, Francisco; Genzel, R.; Tacconi, L. J.; Hicks, E. K. S.; Friedrich, Susanne; Sternberg, A.

doi:10.1086/523032

Cited by 434 publications

(742 citation statements)

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“…This is equivalent to ∼1% of the rest-mass energy of the black hole, and is sufficient (in principle) to expel the entire ISM of such a galaxy. This feedback may play a major role in regulating the growth of the black hole (Davies et al 2007(Davies et al , 2009bWild et al 2010). …”

Section: T M Heckmanmentioning

confidence: 99%

“…On larger spatial scales, JWST, GSMT/E-ELT, and ALMA could be used to map out the distribution and kinematics of ionized and molecular gas for a large and complete sample of AGN and suitable control sample (e.g., Fathi et al 2006;Storchi-Bergmann et al 2007;Riffel et al 2008;Davies et al 2009a;Lindt-Krieg et al 2008;Schinnerer et al 2000). A complementary approach could be provided by mapping of the stellar population and star-formation history in these regions (e.g., Gonzalez Delgado et al 2004;Davies et al 2007). …”

Section: Fueling the Black Holementioning

confidence: 99%

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The Co-Evolution of Galaxies and Black Holes: Current Status and Future Prospects

Heckman

2009

Proc. IAU

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Abstract. I begin by summarizing the evidence that there is a close relationship between the evolution of galaxies and supermassive black holes. They evidently share a common fuel source, and feedback from the black hole may be needed to suppress over-cooling in massive galaxies.I then review what we know about the co-evolution of galaxies and black holes in the modern universe (z < 1). We now have a good documentation of which black holes are growing (the lower mass ones), where they are growing (in the less massive early-type galaxies), and how this growth is related in a statistical sense to star formation in the central region of the galaxy. The opportunity in the next decade will be to use the new observatories to undertake ambitious programs of 3-D imaging spectroscopy of the stars and gas in order to understand the actual astrophysical processes that produce the demographics we observe. At high redshift (z > 2), the most massive black holes and the progenitors of the most massive galaxies are forming. Here, we currently have a tantalizing but fragmented view of their co-evolution. In the next decade, the huge increase in sensitivity and discovery power of our observatories will enable us to analyze the large, complete samples we need to achieve robust and clear results.

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Section: T M Heckmanmentioning

confidence: 99%

Section: Fueling the Black Holementioning

confidence: 99%

The Co-Evolution of Galaxies and Black Holes: Current Status and Future Prospects

Heckman

2009

Proc. IAU

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“…Silk & Norman 2009), and/or the onset of star formation with subsequently fuelled AGN (e.g. Davies et al 2007;Hopkins 2012). The star formation in AGN host galaxies is not concentrated primarily in the nuclear regions, but is distributed over scales of at least several kiloparsecs (e.g.…”

Section: Introductionmentioning

confidence: 99%

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Hakobyan¹,

Nazaryan²,

Adibekyan³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the relative frequencies of different supernova (SN) types in spirals with various morphologies and in barred or unbarred galaxies. We use a well-defined and homogeneous sample of spiral host galaxies of 692 SNe from the Sloan Digital Sky Survey in different stages of galaxy-galaxy interaction and activity classes of nucleus. We propose that the underlying mechanisms shaping the number ratios of SNe types can be interpreted within the framework of interaction-induced star formation, in addition to the known relations between morphologies and stellar populations. We find a strong trend in behaviour of the N Ia /N CC ratio depending on host morphology, such that early spirals include more Type Ia SNe. The N Ibc /N II ratio is higher in a broad bin of early-type hosts. The N Ia /N CC ratio is nearly constant when changing from normal, perturbed to interacting galaxies, then declines in merging galaxies, whereas it jumps to the highest value in post-merging/remnant galaxies. In contrast, the N Ibc /N II ratio jumps to the highest value in merging galaxies and slightly declines in post-merging/remnant subsample. The interpretation is that the star formation rates and morphologies of galaxies, which are strongly affected in the final stages of interaction, have an impact on the number ratios of SNe types. The N Ia /N CC (N Ibc /N II ) ratio increases (decreases) from star-forming to active galactic nuclei (AGN) classes of galaxies. These variations are consistent with the scenario of an interaction-triggered starburst evolving into AGN during the later stages of interaction, accompanied with the change of star formation and transformation of the galaxy morphology into an earlier type.

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“…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.…”

mentioning

confidence: 99%

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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A Close Look at Star Formation around Active Galactic Nuclei

Cited by 434 publications

References 105 publications

The Co-Evolution of Galaxies and Black Holes: Current Status and Future Prospects

The Co-Evolution of Galaxies and Black Holes: Current Status and Future Prospects

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Viscous time lags between starburst and AGN activity

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