CENTRAL STELLAR MASS DEFICITS IN THE BULGES OF LOCAL LENTICULAR GALAXIES, AND THE CONNECTION WITH COMPACT<i>z</i>∼ 1.5 GALAXIES

Dullo, Bililign T.; Graham, Alister W.

doi:10.1088/0004-637x/768/1/36

Cited by 75 publications

(122 citation statements)

References 175 publications

(226 reference statements)

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“…7. As noted in Dullo & Graham (2013), mass deficits in core-Sérsic S0s suggest a two stage assembly: an earlier "dry" major merger event involving SMBHs creates the bulges with depleted cores, and the disc subsequently builds up via cold gas accretion events.…”

Section: Bhmentioning

confidence: 81%

“…As in Dullo & Graham (2013), we build new, composite light profiles for all the 26 core-Sérsic elliptical galaxies by combining the Lauer et al (2005) very inner (R < ∼ 1 ′′ ) deconvolved F555W (∼ V -band) light profiles with our new (calibrated V -band) major-axis light profiles (see below). We have chosen to use the inner deconvolved light profile from Lauer et al (2005) so that differences in the core parameters between our works are not attributed to the use of different treatments of the PSF, but rather the application of the Nuker versus the core-Sérsic model.…”

Section: Surface Brightness Profilesmentioning

confidence: 99%

“…1−6 which were derived here by applying a least-squares fit to each galaxy's (g − V ) and (g − z) data (see also Dullo & Graham 2013 and references therein for a similar practice). For NGC 1399, Lauer et al (2005) published this galaxy's F606W (roughly R-band) light profile, thus we calibrate our ACS g-and Iband data to the R-band light profile using Eq.…”

Section: Surface Brightness Profilesmentioning

confidence: 99%

“…We account for these nuclear light excesses using a Gaussian function. Dullo & Graham (2013) presented the coreSérsic(+exponential) model fits, along with the fit Richings et al (2011, I-and H-bands, triangles) and Dullo & Graham (2012, V -band, red circles for ellipticals and blue disc symbols for S0s). We also compare the inner most Sérsic model fitting radii (R min ) and our break radii for six common galaxies (squares).The geometric-mean break radii from Ferrarese et al (2006) were converted into semi-major axis break radii using their published galaxy ellipticities at R b .…”

Section: Applicationmentioning

confidence: 99%

“…The agreement between their break radii and our measurements are good except for three galaxies (NGC 4382,NGC 4552,and NGC 4472). The most discrepant (by more than 100%) is the S0 galaxy NGC 4382 but this is because it was modelled with a core-Sérsic+exponential model by Dullo & Graham (2013, their Fig. 3).…”

Section: Comparison With Core-sérsic Fits From the Literaturementioning

confidence: 99%

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

Dullo¹,

Graham²

2014

Monthly Notices of the Royal Astronomical Society

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New surface brightness profiles from 26 early-type galaxies with suspected partially depleted cores have been extracted from the full radial extent of Hubble Space Telescope images. We have carefully quantified the radial stellar distributions of the elliptical galaxies using the core-Sérsic model whereas for the lenticular galaxies a core-Sérsic bulge plus an exponential disc model gives the best representation. We additionally caution about the use of excessive multiple Sérsic functions for decomposing galaxies and compare with past fits in the literature. The structural parameters obtained from our fitted models are in general, in good agreement with our initial study using radially limited (R < ∼ 10 ′′ ) profiles, and are used here to update several "central" as well as "global" galaxy scaling relations. We find near-linear relations between the break radius R b and the spheroid luminosity L such that R b ∝ L 1.13±0.13 , and with the supermassive black hole mass. This is internally consistent with the notion that major, dry mergers add the stellar and black hole mass in equal proportion, i.e., M BH ∝ L. In addition, we observe a linear relation R b ∝ R 0.98±0.15 e for the core-Sérsic elliptical galaxies-where R e is the galaxies' effective half light radii-which is collectively consistent with the approximately-linear, bright-end of the curved L − R e relation. Finally, we measure accurate stellar mass deficits M def that are in general 0.5−4 M BH , and we identify two galaxies (NGC 1399, NGC 5061) that, due to their high M def /M BH ratio, may have experienced oscillatory core-passage by a (gravitational radiation)-kicked black hole. The galaxy scaling relations and stellar mass deficits favor core-Sérsic galaxy formation through a few "dry" major merger events involving supermassive black holes such that M def ∝ M 3.70±0.76 BH , for M BH > ∼ 2 × 10 8 M ⊙ .

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Section: Bhmentioning

confidence: 81%

Section: Surface Brightness Profilesmentioning

confidence: 99%

Section: Surface Brightness Profilesmentioning

confidence: 99%

Section: Applicationmentioning

confidence: 99%

Section: Comparison With Core-sérsic Fits From the Literaturementioning

confidence: 99%

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

Dullo¹,

Graham²

2014

Monthly Notices of the Royal Astronomical Society

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147

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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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Galaxy Bulges and Their Massive Black Holes: A Review

Graham

2016

Astrophysics and Space Science Library

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122

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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.

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CENTRAL STELLAR MASS DEFICITS IN THE BULGES OF LOCAL LENTICULAR GALAXIES, AND THE CONNECTION WITH COMPACTz∼ 1.5 GALAXIES

Cited by 75 publications

References 175 publications

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

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

Galactic Bulges

Galaxy Bulges and Their Massive Black Holes: A Review

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