On the dynamics of supermassive black holes in gas-rich, star-forming galaxies: the case for nuclear star cluster co-evolution

Biernacki, P.; Teyssier, Romain; Bleuler, Andreas

doi:10.1093/mnras/stx845

Cited by 32 publications

(30 citation statements)

References 115 publications

(188 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Hayward et al, 2014;Gabor et al, 2016) and to the specific implementation of BH dynamics (e.g. Lupi et al, 2015a,b;Biernacki et al, 2017), accretion (e.g. Debuhr et al, 2010; Hopkins and Quataert, 2011), and feedback (e.g.…”

Section: Dual Agn Properties and Occurrencementioning

confidence: 99%

The quest for dual and binary supermassive black holes: A multi-messenger view

Rosa

Vignali

Bogdanović

et al. 2019

New Astronomy Reviews

201

123

View full text Add to dashboard Cite

The quest for binary and dual supermassive black holes (SMBHs) at the dawn of the multi-messenger era is compelling. Detecting dual active galactic nuclei (AGN)-active SMBHs at projected separations larger than several parsecs-and binary AGN-probing the scale where SMBHs are bound in a Keplerian binary-is an observational challenge. The study of AGN pairs (either dual or binary) also represents an overarching theoretical problem in cosmology and astrophysics. The AGN triggering calls for detailed knowledge of the hydrodynamical conditions of gas in the imminent surroundings of the SMBHs and, at the same time, their duality calls for detailed knowledge on how galaxies assemble through major and minor mergers and grow fed by matter along the filaments of the cosmic web. This review describes the techniques used across the electromagnetic spectrum to detect dual and binary AGN candidates and proposes new avenues for their search. The current observational status is compared with the state-of-the-art numerical simulations and models for formation of dual and binary AGN. Binary SMBHs are among the loudest sources of gravitational waves (GWs) in the Universe. The search for a background of GWs at nHz frequencies from inspiralling SMBHs at low redshifts, and the direct detection of signals from their coalescence by the Laser Interferometer Space Antenna in the next decade, make this a theme of major interest for multi-messenger astrophysics. This review discusses the future facilities and observational strategies that are likely to significantly advance this fascinating field.

show abstract

Section: Dual Agn Properties and Occurrencementioning

confidence: 99%

The quest for dual and binary supermassive black holes: A multi-messenger view

Rosa

Vignali

Bogdanović

et al. 2019

New Astronomy Reviews

201

123

View full text Add to dashboard Cite

show abstract

“…This is in agreement with our understanding of dynamical friction: it is a very long process if the mass of the BH is low. The presence of a nuclear star cluster could speed-up the process (Biernacki et al 2017), increasing the mass experiencing dynamical friction, but due to our limited resolution, Table 3, as noted in the inset. If the BH in the satellite galaxy merges with the BH of the central galaxy, we show its subsequent evolution with dashed lines.…”

Section: Formation Of a Black Hole Binary In A High-redshift Galaxy Mmentioning

confidence: 99%

The erratic dynamical life of black hole seeds in high-redshift galaxies

Pfister

Volonteri

Dubois

et al. 2019

Monthly Notices of the Royal Astronomical Society

144

111

View full text Add to dashboard Cite

The dynamics of black hole seeds in high redshift galaxies is key to understand their ability to grow via accretion and to pair in close binaries during galactic mergers. To properly follow the dynamics of black holes we develop a physically motivated model to capture unresolved dynamical friction from stars, dark matter and gas. We first validate the model and then we use it to investigate the dynamics of seed black holes born at z ∼ 9 in dwarf proto-galaxies. We perform a suite of zoom cosmological simulations with spatial resolution as high as 10 pc and with a stellar and dark matter mass resolution of 2×10 3 M and 2×10 5 M respectively. We first explore the dynamics of a seed black hole in the galaxy where it is born and show that it is highly erratic if the seed mass is less than 10 5 M . The dynamics is dominated by the stellar component, whose distribution is irregular and patchy, thus inducing stochasticity in the orbits: the black hole may be anywhere in the proto-galaxy. When this dwarf merges into a larger galaxy, it is paramount to simulate the process with very high spatial and mass resolution in order to correctly account for the stripping of the stellar envelope of the satellite black hole. The outcome of the encounter could be either a tight binary or, at least temporary, a wandering black hole, leading to multiple black holes in a galaxy, each inherited from a different merger.

show abstract

“…In order to overcome the overcooling problem of supernovae feedback due to our limited resolution, we use a non-thermal energy variable that dissipates over a 10 Myr timescale (see Teyssier et al 2013, for details). Supermasive black holes (SMBHs) are modelled with our new sink particle algorithm (Bate et al 1995;Krumholz et al 2004;Bleuler & Teyssier 2014;Biernacki et al 2017). We allow for only one sink to form in our simulations.…”

Section: Numerical Setupmentioning

confidence: 99%

The combined effect of AGN and supernovae feedback in launching massive molecular outflows in high-redshift galaxies

Biernacki

Teyssier

2018

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We have recently improved our model of active galactic nucleus (AGN) by attaching the supermassive black hole (SMBH) to a massive nuclear star cluster (NSC). Here we study the effects of this new model in massive, gas-rich galaxies with several simulations of different feedback recipes with the hydrodynamics code RAMSES. These simulations are compared to a reference simulation without any feedback, in which the cooling halo gas is quickly consumed in a burst of star formation. In the presence of strong supernovae (SN) feedback, we observe the formation of a galactic fountain that regulates star formation over a longer period, but without halting it. If only AGN feedback is considered, as soon as the SMBH reaches a critical mass, strong outflows of hot gas are launched and prevent the cooling halo gas from reaching the disk, thus efficiently halting star formation, leading to the so-called "quenching". If both feedback mechanisms act in tandem, we observe a non-linear coupling, in the sense that the dense gas in the supernovae-powered galactic fountain is propelled by the hot outflow powered by the AGN at much larger radii than without AGN. We argue that these particular outflows are able to unbind dense gas from the galactic halo, thanks to the combined effect of SN and AGN feedback. We speculate that this mechanism occurs at the end of the fast growing phase of SMBH, and is at the origin of the dense molecular outflows observed in many massive high-redshift galaxies.

show abstract

On the dynamics of supermassive black holes in gas-rich, star-forming galaxies: the case for nuclear star cluster co-evolution

Cited by 32 publications

References 115 publications

The quest for dual and binary supermassive black holes: A multi-messenger view

The quest for dual and binary supermassive black holes: A multi-messenger view

The erratic dynamical life of black hole seeds in high-redshift galaxies

The combined effect of AGN and supernovae feedback in launching massive molecular outflows in high-redshift galaxies

Contact Info

Product

Resources

About