Feedback by Massive Black Holes in Gas-rich Dwarf Galaxies

Silk, Joseph

doi:10.3847/2041-8213/aa67da

Cited by 120 publications

(101 citation statements)

References 85 publications

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“…These potential fluctuations dynamically heat the DM and lead to the formation of a core (e.g. Martizzi, Teyssier & Moore 2013;Peirani, et al 2017;Silk 2017). The gradually dispersion of the DM particles away from the center of the halo is ultimately responsible for core creation.…”

Section: The Cusp-core Problemmentioning

confidence: 99%

Subhalo sinking and off-centre massive black holes in dwarf galaxies

Boldrini

Mohayaee

Silk

2020

Monthly Notices of the Royal Astronomical Society: Letters

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Using fully GPU N-body simulations, we demonstrate for the first time that subhalos sink and transfer energy via dynamical friction into the centres of dwarf galaxies. This dynamical heating kicks any central massive black hole (MBH) out to tens of parsecs, especially at early epochs (z=1.5-3). This mechanism helps explain the observed off-center BHs in dwarf galaxies and also predicts that off-center BHs are more common in higher mass dwarf galaxies since dynamical friction becomes significantly weaker and BHs take more time to sink back towards the centres of their host galaxies. One consequence of off-center BHs during early epochs of dwarf galaxies is to quench any BH feedback.

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Section: The Cusp-core Problemmentioning

confidence: 99%

Subhalo sinking and off-centre massive black holes in dwarf galaxies

Boldrini

Mohayaee

Silk

2020

Monthly Notices of the Royal Astronomical Society: Letters

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“…But the occupation fraction, which is critical in setting the white dwarf TDE rate is unknown. Circumstantial arguments by Silk (2017) suggest that an occupation fraction near unity would resolve many of the open questions in dwarf galaxy evolution. Fig.…”

Section: Abstract White Dwarf · Intermediate-mass Black Hole 1 Introdmentioning

confidence: 99%

Tidal Disruptions of White Dwarfs: Theoretical Models and Observational Prospects

et al. 2020

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White dwarf stars that enter the tidal radius of black holes with masses < ∼ 10 5 M are doomed to be ripped apart by tidal forces. Black holes in this mass range between stellar black holes and supermassive black holes have not been conclusively identified so the detection of a tidal disruption of a white dwarf would provide clear evidence for the existence of intermediatemass black holes. In this review, we present a theoretical and observational overview of the transient events that result from the tidal disruptions of white dwarfs by intermediate-mass black holes. This includes discussion of the latest simulations and predicted properties, the results of observational searches, as well as a summary of the potential for gravitational wave emission to be detected with upcoming missions.

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“…Di Cintio et al (2017) used the NIHAO simulation to study the formation of UDG-type galaxies, and they also suggested that internal processes, particularly outflow-driven feedback, may be responsible for their formation. Feedback from active galactic nuclei in dwarf galaxies may also contribute to their diversity and range in morphologies (Silk 2017).…”

Section: Introductionmentioning

confidence: 99%

The abundance of ultra-diffuse galaxies from groups to clusters

Burg

Hoekstra

Muzzin

et al. 2017

A&A

116

106

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In recent years, many studies have reported substantial populations of large galaxies with low surface brightness in local galaxy clusters. Various theories that aim to explain the presence of such ultra-diffuse galaxies (UDGs) have since been proposed. A key question that will help to distinguish between models is whether UDGs have counterparts in host haloes with lower masses, and if so, what their abundance as a function of halo mass is. We here extend our previous study of UDGs in galaxy clusters to galaxy groups. We measure the abundance of UDGs in 325 spectroscopically selected groups from the Galaxy And Mass Assembly (GAMA) survey. We make use of the overlapping imaging from the ESO Kilo-Degree Survey (KiDS), from which we can identify galaxies with mean surface brightnesses within their effective radii down to ∼25.5 mag arcsec −2 in the r band. We are able to measure a significant overdensity of UDGs (with sizes r eff ≥ 1.5 kpc) in galaxy groups down to M 200 = 10 12 M , a regime where approximately only one in ten groups contains a UDG that we can detect. We combine measurements of the abundance of UDGs in haloes that cover three orders of magnitude in halo mass, finding that their numbers scale quite steeply with halo mass: N UDG (R < R 200 ) ∝ M . This shows that compared to bright galaxies, UDGs are relatively more abundant in massive clusters than in groups. We discuss the implications, but it is still unclear whether this difference is related to a higher destruction rate of UDGs in groups or if massive haloes have a positive effect on UDG formation.

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Feedback by Massive Black Holes in Gas-rich Dwarf Galaxies

Cited by 120 publications

References 85 publications

Subhalo sinking and off-centre massive black holes in dwarf galaxies

Subhalo sinking and off-centre massive black holes in dwarf galaxies

Tidal Disruptions of White Dwarfs: Theoretical Models and Observational Prospects

The abundance of ultra-diffuse galaxies from groups to clusters

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