Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

Dullo, Bililign T.; Graham, Alister W.

doi:10.1093/mnras/stu1590

Cited by 83 publications

(165 citation statements)

References 164 publications

(317 reference statements)

Supporting

Mentioning

154

Contrasting

Order By: Relevance

“…This value is in accordance with several observed core-type galaxies in Rusli et al (2013) and Dullo & Graham (2014) and it results in a 3D density profile, which declines faster than r −0.5 . This is an important constraint for isotropic models as it guarantees the dynamical stability within the influence radius of the black hole (Tremaine et al 1994).…”

Section: Initial Galaxy Profiles and Parameterssupporting

confidence: 92%

“…This is an important constraint for isotropic models as it guarantees the dynamical stability within the influence radius of the black hole (Tremaine et al 1994). The transition parameter, α = 4.25, is obtained from the arithmetic mean values from all galaxies in Rusli et al (2013) and Dullo & Graham (2014) except NGC 7768. This particular galaxy has a transition value that is too sharp, α → ∞, which would otherwise bias the arithmetic mean.…”

Section: Initial Galaxy Profiles and Parametersmentioning

confidence: 99%

“…Black hole scaling relations link different properties of galaxies, such as total luminosity and bulge mass (Kormendy & Richstone 1995;McLure & Dunlop 2002;Marconi & Hunt 2003;Häring & Rix 2004;McConnell & Ma 2013), the velocity dispersion, σ, (Ferrarese & Merritt 2000;Gebhardt et al 2000;Gültekin et al 2009;McConnell & Ma 2013), and the central surface brightness profile (Lauer et al 2007a;Kormendy & Bender 2009;Rusli et al 2013;Dullo & Graham 2014) to the mass of the nuclear SMBH. Currently, there is a debate about whether the empirical M • − σ relation is a consequence of black hole feedback regulated galaxy growth (e.g., Silk & Rees 1998;Fabian 2012) or results from stochastic averaging over numerous galaxy coalescences in a cosmological merger tree (Jahnke & Macciò 2011).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Unveiling Gargantua: A new search strategy for the most massive central cluster black holes

Brockamp

Baumgardt

Britzen

et al. 2016

A&A

View full text Add to dashboard Cite

Aims. We aim to unveil the most massive central cluster black holes in the Universe.Methods. We present a new search strategy, which is based on a black hole mass gain sensitive calorimeter and which links the innermost stellar density profile of a galaxy to the adiabatic growth of its central supermassive black hole (SMBH). As a first step we convert observationally inferred feedback powers into SMBH growth rates using reasonable energy conversion efficiency parameters, . In the main part of this paper we use these black hole growth rates, sorted in logarithmically increasing steps encompassing our whole parameter space, to conduct N-body computations of brightest cluster galaxies (BCGs) with the newly developed M software. For the initial setup of galaxies, we use core-Sérsic models to account for SMBH scouring. Results. We find that adiabatically driven core regrowth is significant at the highest accretion rates. As a result, the most massive black holes should be located in BCGs with less pronounced cores when compared to the predictions of empirical scaling relations, which are usually calibrated in less extreme environments. For efficiency parameters < 0.1, BCGs in the most massive, relaxed, and X-ray luminous galaxy clusters might even develop steeply rising density cusps. Finally, we discuss several promising candidates for follow-up investigations, among them the nuclear black hole in the Phoenix cluster. Based on our results, its central black hole might have a mass of the order of 10 11 M .

show abstract

Section: Initial Galaxy Profiles and Parameterssupporting

confidence: 92%

Section: Initial Galaxy Profiles and Parametersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Unveiling Gargantua: A new search strategy for the most massive central cluster black holes

Brockamp

Baumgardt

Britzen

et al. 2016

A&A

View full text Add to dashboard Cite

show abstract

“…Dullo & Graham 2014). It is certainly telling that the orientations of the kinematic features are linked to those of the photometric body, but they are not compatible with two thin discs.…”

Section: ′′mentioning

confidence: 99%

Unveiling the counter-rotating nature of the kinematically distinct core in NGC 5813 with MUSE

Krajnović

Weilbacher

Urrutia

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

MUSE observations of NGC 5813 reveal a complex structure in the velocity dispersion map, previously hinted by SAURON observations. The structure is reminiscent of velocity dispersion maps of galaxies comprising two counter-rotating discs, and may explain the existence of the kinematically distinct core (KDC). Further evidence for two counter-rotating components comes from the analysis of the higher moments of the stellar line-of-sight velocity distributions and fitting MUSE spectra with two separate Gaussian line-of-sight velocity distributions. The emission-line kinematics show evidence of being linked to the present cooling flows and the buoyant cavities seen in Xrays. We detect ionised gas in a nuclear disc-like structure, oriented like the KDC, which is, however, not directly related to the KDC. We build an axisymmetric Schwarzschild dynamical model, which shows that the MUSE kinematics can be reproduced well with two counter-rotating orbit families, characterised by relatively low angular momentum components, but clearly separated in integral phase space and with radially varying contributions. The model indicates that the counter-rotating components in NGC 5813 are not thin discs, but dynamically hot structures. Our findings give further evidence that KDCs in massive galaxies should not necessarily be considered as structurally or dynamically decoupled regions, but as the outcomes of the mixing of different orbital families, where the balance in the distribution of mass of the orbital families is crucial. We discuss the formation of the KDC in NGC 5813 within the framework of gas accretion, binary mergers and formation of turbulent thick discs from cold streams at high redshift.

show abstract

“…Graham 2004;Rusli et al 2013b;Dullo & Graham 2014). This relation simply exists over a restricted mass range.…”

Section: Pseudobulgesmentioning

confidence: 99%

Galaxy Bulges and Their Massive Black Holes: A Review

Graham

2016

Astrophysics and Space Science Library

Self Cite

122

View full text Add to dashboard Cite

With references to both key and oft-forgotten pioneering works, this article starts by presenting a review into how we came to believe in the existence of massive black holes at the centres of galaxies. It then presents the historical development of the near-linear (black hole)-(host spheroid) mass relation, before explaining why this has recently been dramatically revised. Past disagreement over the slope of the (black hole)-(velocity dispersion) relation is also explained, and the discovery of substructure within the (black hole)-(velocity dispersion) diagram is discussed. As the search for the fundamental connection between massive black holes and their host galaxies continues, the competing array of additional black hole mass scaling relations for samples of predominantly inactive galaxies are presented.

show abstract

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

Cited by 83 publications

References 164 publications

Unveiling Gargantua: A new search strategy for the most massive central cluster black holes

Unveiling Gargantua: A new search strategy for the most massive central cluster black holes

Unveiling the counter-rotating nature of the kinematically distinct core in NGC 5813 with MUSE

Galaxy Bulges and Their Massive Black Holes: A Review

Contact Info

Product

Resources

About