Depleted Galaxy Cores and Dynamical Black Hole Masses

Rusli, Stephanie; Erwin, Peter; Saglia, R.; Thomas, Jens; Fabricius, Maximilian; Bender, Ralf; Nowak, N.

doi:10.1088/0004-6256/146/6/160

Cited by 106 publications

(337 citation statements)

References 83 publications

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“…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%

“…Selected parameters for our models are listed in Table 1 and are discussed below. By first fixing the initial SMBH mass at M • [M 9 ] = 1.5, 5, 10, 15, 20, 40, R b is then extracted from the parameter relation in Rusli et al (2013). Although values as high as R b = 3.8 kpc seem far-fetched, there exist central cluster galaxies, e.g., Abell 2261 and Abell 85, which have similar or even larger break-radii (Postman et al 2012;López-Cruz et al 2014).…”

Section: Initial Galaxy Profiles and Parametersmentioning

confidence: 99%

“…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%

“…Using the M • − R break (Rusli et al 2013), M • − R cusp (Lauer et al 2007a) and M • − L def (Kormendy & Bender 2009) relations, where R cusp is the cusp radius of a Nuker profile and L def is the total luminosity difference between measured and extrapolated light profile, McNamara et al (2009) and López-Cruz et al (2014) found indications for extraordinary massive SMBHs. The central black hole masses in MS0735 and Abell 85 might be as high as 10 11 M as long as their shallow density profiles are carved out by black hole merging processes 1 .…”

Section: Introductionmentioning

confidence: 99%

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

Brockamp

Baumgardt

Britzen

et al. 2016

A&A

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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 .

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Section: Initial Galaxy Profiles and Parameterssupporting

confidence: 92%

Section: Initial Galaxy Profiles and Parametersmentioning

confidence: 99%

Section: Initial Galaxy Profiles and Parametersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Brockamp

Baumgardt

Britzen

et al. 2016

A&A

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Dark Matter in Elliptical Galaxies

Buote

Humphrey

2011

Astrophysics and Space Science Library

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We review X-ray constraints on dark matter in giant elliptical galaxies (10 12 M ⊙ < ∼ M vir < ∼ 10 13 M ⊙ ) obtained using the current generation of X-ray satellites, beginning with an overview of the physics of the hot interstellar medium and mass modeling methodology. Dark matter is now firmly established in many galaxies, with inferred NFW concentration parameters somewhat larger than the mean theoretical relation. X-ray observations confirm that the total mass profile (baryons+DM) is close to isothermal (M ∼ r), and new evidence suggests a more general power-law relation for the slope of the total mass profile that varies with the stellar half-light radius. We also discuss constraints on the baryon fraction, supermassive black holes, and axial ratio of the dark matter halo. Finally, we review constraints on non-thermal gas motions and discuss the accuracy of the hydrostatic equilibrium approximation in elliptical galaxies.

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Galactic Bulges

2016

Astrophysics and Space Science Library

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978-3-319-19377-9 ISBN 978-3-319-19378-6 (eBook) DOI 10.1007/978-3-319-19378-6 Library of Congress Control Number: 2015949217 Springer Cham Heidelberg New York Dordrecht London © Springer International Publishing Switzerland 2016 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. The use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specific statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. The publisher, the authors and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication. Neither the publisher nor the authors or the editors give a warranty, express or implied, with respect to the material contained herein or for any errors or omissions that may have been made.Cover Illustration: In the cover the 3.6 images of one nearby galaxy, NGC 4565, is shown. The images are from the Spitzer Survey of Stellar Structure in Galaxies (PI Kartik Sheth).Printed on acid-free paper Springer International Publishing AG Switzerland is part of Springer Science+Business Media (www.springer.com) PrefaceThe main motivation for this book was our impression that when observers talk about bulges in galaxies, they do not necessarily mean the same thing as people making theoretical models. Even among the observers, it is not always clear what they mean by classical and pseudobulges. According to most researchers, classical bulges are highly relaxed systems typically formed in galaxy mergers or by coalescence of massive gas clumps at high redshifts, whereas pseudobulges have more disc-like properties. Some people divide pseudobulges further into discy pseudobulges, defined as small central discs in the plane of the galactic disc, and boxy/peanut bulges which are actually dynamically heated, vertically thick inner parts of bars. Galaxies can also have central star clusters, usually called nuclear clusters, which structures are not called bulges in this book (see the review by Cole and Debattista). In recent years significant progress has been made both on the theoretical and observational sides, including galactic and extragalactic research. In this book we try to bring all these communities closer to each other.Most probably many of us share the Copernican approach trying to understand the universe with some simple beautiful theory. Such an attempt is the current paradigm of structure formation, i.e., the hierarchical growth of dark matter halos ( CDM), and the subsequent formatio...

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Depleted Galaxy Cores and Dynamical Black Hole Masses

Cited by 106 publications

References 83 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

Dark Matter in Elliptical Galaxies

Galactic Bulges

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