The Centers of Early‐Type Galaxies with<i>Hubble Space Telescope</i>. VI. Bimodal Central Surface Brightness Profiles

Lauer, Tod R.; Gebhardt, Karl; Faber, S. M.; Richstone, D. O.; Tremaine, Scott; Kormendy, John; Aller, M.; Bender, Ralf; Dressler, Alan; Filippenko, A. V.; Green, Richard; Ho, Luis C.

doi:10.1086/519229

Cited by 227 publications

(417 citation statements)

References 57 publications

(195 reference statements)

Supporting

Mentioning

388

Contrasting

Order By: Relevance

“…The superscript d shows elliptical galaxies which are classified as disc galaxies in the literature (Appendix C). Col. (3) Absolute V -band (galaxy or bulge) magnitude obtained from Lauer et al (2007b). These magnitudes are corrected for Galactic extinction and (1 + z) 4 surface brightness dimming, and adjusted using the distances from col. (4).…”

Section: Galaxy Imagingmentioning

confidence: 99%

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

Dullo¹,

Graham²

2014

Monthly Notices of the Royal Astronomical Society

147

View full text Add to dashboard Cite

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 ⊙ .

show abstract

Section: Galaxy Imagingmentioning

confidence: 99%

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

Dullo¹,

Graham²

2014

Monthly Notices of the Royal Astronomical Society

147

View full text Add to dashboard Cite

show abstract

“…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). The effective radii, R e , and dynamical masses, M dyn , of our model galaxies are based on real galaxies (NGC 1399, M 60, NGC 3842, NGC 4889, NGC 6166) with similar black holes (Magorrian et al 1998;Lauer et al 2007b;McConnell & Ma 2013). The SMBH masses (M • [M 9 ] = 15, 20) are within the one sigma confidence limits of NGC 4889.…”

Section: Initial Galaxy Profiles and Parametersmentioning

confidence: 83%

“…The action of binary or multiple black holes after merger events of their host galaxies is suspected to be responsible for the formation of shallow central brightness profiles of luminous galaxies (Ebisuzaki et al 1991;Milosavljević & Merritt 2001;Merritt 2006) with V-band magnitudes M V −21 (Lauer et al 2007b). This scenario is supported by Thomas et al (2014), who found a tangentially biased velocity distribution within the break radius, R break , which is located at the maximal curvature of the surface brightness profile.…”

Section: Introductionmentioning

confidence: 99%

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

“…Namely, the inner regions of radio-loud galaxies display star deficient cores. Such cores, in turn, reside preferentially in giant ellipticals (see, e.g., Lauer et al, 2007). On the other hand, radioquiet galaxies, including nearby low-luminosity Seyferts, display instead cuspy brightness profiles.…”

Section: Discussionmentioning

confidence: 99%

“…Namely, the 'core-galaxies' -i.e., the ones with shallow central stellar density distributions -are much radio-louder than the powerlaw/cuspy galaxies (Capetti & Balmaverde, 2006, 2007. It is then interesting to note that the coregalaxies are on average much more massive than the power-law galaxies, being usually identified as giant ellipticals, while the power-law stralight profiles are common in disk galaxies or disky-ellipticals (Lauer et al, 2007;Capetti & Balmaverde, 2007). …”

Section: Radio-loudnessmentioning

confidence: 99%

Radio-loudness of active galaxies and the black hole evolution

Sikora

Stawarz

Lasota

2008

New Astronomy Reviews

View full text Add to dashboard Cite

Active galactic nuclei (AGNs) form two distinct sequences on the radio-loudness -Eddington-ratio plane. The 'upper' sequence contains radio selected AGNs, the 'lower' sequence is composed mainly of optically selected AGNs. The sequences mark the upper bounds for the radio-loudness of two distinct populations of AGNs, hosted respectively by elliptical and disk galaxies. Both sequences show the same dependence of the radio-loudness on the Eddington ratio (an increase with decreasing Eddington ratio), which suggests that another parameter in addition to the accretion rate must play a role in determining the efficiency of jet production in AGNs. We speculate that this additional parameter is the spin of the black hole, assuming that black holes in giant elliptical galaxies have (on average) much larger spins than black holes in disc galaxies. Possible evolutionary scenarios leading to such a spin dichotomy are discussed. The galaxy-morphology related radio-dichotomy breaks down at high accretion rates where the dominant fraction of luminous quasars being hosted by giant ellipticals is radio quiet. This indicates that the production of powerful jets at high accretion rates is in most cases suppressed and, in analogy to X-ray binary systems (XRB) during high and very high states, may be intermittent. Such intermittency can be caused by switches between two different accretion modes, assuming that only during one of them an outflow from the central engine is sufficiently collimated to form a relativistic jet.

show abstract

The Centers of Early‐Type Galaxies withHubble Space Telescope. VI. Bimodal Central Surface Brightness Profiles

Cited by 227 publications

References 57 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

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

Radio-loudness of active galaxies and the black hole evolution

Contact Info

Product

Resources

About