The kinematic properties of faint elliptical galaxies

Davies, R. L.; Efstathiou, G.; Fall, S. Michael; Illingworth, G. D.; Schechter, Paul L.

doi:10.1086/160757

Cited by 518 publications

(475 citation statements)

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“…One of these is the M BH -s relation (Ferrarese & Merritt 2000;Gebhardt et al 2000), which can be described with a single power law (M BH 5 6 s µ -) over a wide range in velocity dispersion (70 350 km s 1 --, e.g., Graham et al 2011;McConnell et al 2011;. The other is the L sph -s relation, which has long been known to be a "double power law," with L sph 5 6 s µ -at the luminous end 5 (Schechter 1980;Malumuth & Kirshner 1981;Lauer et al 2007b;von der Linden et al 2007;Liu et al 2008)and L sph 2 s µ at intermediate and faint luminosities (Davies et al 1983;Held et al 1992;de Rijcke et al 2005;Matković & Guzmán 2005;Balcells et al 2007;Chilingarian et al 2008;Forbes et al 2008;Cody et al 2009;Tortora et al 2009 When Graham (2012) pointed out this overlooked inconsistency between these linear and bent relations, he identified two different populations of galaxies, namely the core-Sérsic spheroids Trujillo et al 2004) and the Sérsic spheroids 6 , and attributed the change in slope (from super-quadratic to linear) to their different formation mechanisms. In this scenario, core-Sérsic spheroids are built in dry merger events where the black hole and the bulge grow at the same pace, increasing their mass in lock steps (M L BH sph 1 µ ), whereas Sérsic spheroids originate from gas-rich processes in which the mass of the black hole increases more rapidly than the mass of its host spheroid (M L BH sph 2.5 µ ).…”

Section: Introductionmentioning

confidence: 99%

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

Savorgnan

Graham

Marconi

et al. 2016

ApJ

133

181

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In our first paper, we performed a detailed (i.e., bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, M BH , imaged at 3.6 m m with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between M BH and the host spheroid (and galaxy) luminosity, L sph (and L gal ), and also stellar mass, M .,sph * While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have M M 10 , argued by some to be pseudo-bulges, are not offset to lower M BH from the correlation defined by the current bulge sample with n 2; sph > and (3)L sph and L gal correlate equally well with M BH , in terms of intrinsic scatter, only for early-type galaxies-once reasonable numbers of spiral galaxies are included, the correlation with L sph is better than that with L gal .

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Section: Introductionmentioning

confidence: 99%

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

Savorgnan

Graham

Marconi

et al. 2016

ApJ

133

181

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“…Davies et al (1983) studied the now classical V max /σ o versus diagram for spheroids (Illingworth 1977;Binney 1978), where V max is the maximum of the lineof-sight (l.o.s.) rotation curve, σ o is the central l.o.s.…”

Section: Introductionmentioning

confidence: 99%

Shape and kinematics of elliptical galaxies: evolution due to merging at z ${<}$ 1.5

González-García¹,

Oñorbe²,

Domínguez-Tenreiro³

et al. 2009

A&A

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Aims. We investigate the evolution in the shape and kinematics of elliptical galaxies in a cosmological framework. Methods. We identified relaxed, elliptical-like objects (ELOs) at redshifts z = 0, z = 0.5, z = 1 and z = 1.5 within a set of hydrodynamic, self-consistent simulations completed for a concordance cosmological model. Results. The population of elliptical systems that we analysed evolve systematically with time becoming rounder in general by z = 0 and also more velocity dispersion supported. We found that this is due primarily to major dry mergers where only a modest amount of angular momentum is involved in the merger event. Despite the general trend, in a significant number of cases the merger event involves a relatively high amount of specific angular momentum, which causes the system in general to acquire higher rotational support and/or a more oblate shape. These evolutionary patterns persist when we study our systems in projection, in simulating true observations, and thus should be evident in future observations.

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“…Ever since the seminal study by Davies et al (1983), it has been known that elliptical galaxies can be divided in two distinct classes. The bright ellipticals gener-(M B [ [20.5) ally have a boxy appearance, are pressure supported, and often show some form of radio and/or X-ray activity.…”

Section: Introductionmentioning

confidence: 99%

WFPC2 Images of the Central Regions of Early-Type Galaxies. I. The Data

Rest

Bosch

Jaffe

et al. 2001

The Astronomical Journal

207

377

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We present high-resolution R-band images of the central regions of 67 early-type galaxies obtained with the Wide Field and Planetary Camera 2 (WFPC2) aboard the Hubble Space T elescope (HST ). This homogeneously selected sample roughly doubles the number of early-type galaxies that have now been imaged at HST resolution and complements similar data on the central regions of radio galaxies and the bulges of spiral galaxies. Our sample strikingly conÐrms the complex morphologies of the central regions of early-type galaxies which have become apparent from previous studies with HST . In particular, we detect dust, either in the form of nuclear disks or with a Ðlamentary distribution, in 43% of all galaxies, in good agreement with previous estimates. In addition, we Ðnd evidence for embedded stellar disks in a remarkably large fraction of 51%. In 14 of those galaxies the disklike structures are misaligned with the main galaxy, suggesting that they correspond to stellar bars in S0 galaxies. We analyze the luminosity proÐles of the galaxies in our sample and classify galaxies according to their central cusp slope. To a large extent we conÐrm the results from previous HST surveys in that early-type galaxies reveal a clear dichotomy : the bright ellipticals are generally boxy and have luminosity proÐles that (M B [ [20.5) break from steep outer power laws to shallow inner cusps (referred to as "" core ÏÏ galaxies). The fainter ellipticals, on the other hand, typically have disky isophotes and luminosity proÐles that lack a clear break and have a steep central cusp (referred to as "" power-law ÏÏ galaxies). The advantages and shortcomings of classiÐcation schemes utilizing the extrapolated central cusp slope c are discussed, and it is shown that c might be an inadequate representation for galaxies whose luminosity proÐle slope changes smoothly with radius rather than resembling a broken power law. Thus, we introduce a new, alternative parameter and show how this a †ects the classiÐcation. In fact, we Ðnd evidence for an "" intermediate ÏÏ class of galaxies that cannot unambiguously be classiÐed as either core or power-law galaxies and that have central cusp slopes and absolute magnitudes intermediate between those of core and power-law galaxies. It is unclear at present, however, whether these galaxies make up a physically distinct class or whether distance and/or resolution e †ects cause them to lose their distinct core or power-law characteristics.

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The kinematic properties of faint elliptical galaxies

Cited by 518 publications

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SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

Shape and kinematics of elliptical galaxies: evolution due to merging at z ${<}$ 1.5

WFPC2 Images of the Central Regions of Early-Type Galaxies. I. The Data

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The kinematic properties of faint elliptical galaxies

Cited by 518 publications

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SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE MBH–M*,SPH DIAGRAM

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE MBH–M*,SPH DIAGRAM

Shape and kinematics of elliptical galaxies: evolution due to merging at z ${<}$ 1.5

WFPC2 Images of the Central Regions of Early-Type Galaxies. I. The Data

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SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM