THEMBH-LSPHEROIDRELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES

Graham, Alister W.; Scott, Nicholas

doi:10.1088/0004-637x/764/2/151

Cited by 257 publications

(269 citation statements)

References 297 publications

(309 reference statements)

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“…Given the well known MBH − σ (Ferrarese & Merritt 2000;Gebhardt et al 2000) and MBH −L (Marconi & Hunt 2003;Graham & Scott 2013) relations, the strong R b − σ and R b − L correlations in Section 4.1 hint at a tight R b − MBH relation. This trend is observed in Fig.…”

Section: Core Size Versus Black Hole Massmentioning

confidence: 89%

“…8, and quantified in Table 3 for our sample of 31 galaxies. Eight of these galaxies have direct SMBH mass measurements, while the remaining SMBH masses were predicted using either the Graham & Scott (2013) "non-barred MBH − σ" relation 8 log MBH M ⊙ = (5.53±0.34) log σ 200 kms −1 + (8.22 ±0.05), (13) or their B-band core-Sérsic MBH − L relation which is converted here to V -band using B − V = 1.0 (Fukugita et al 1995;Faber et al 1997), to give Figure 8. Correlation between core-Sérsic break radius R b (Table 2) and black hole mass.…”

Section: Core Size Versus Black Hole Massmentioning

confidence: 99%

“…Correlation between core-Sérsic break radius R b (Table 2) and black hole mass. The SMBH masses are acquired from direct SMBH mass measurements for 8 circled galaxies, while for the remaining 23 galaxies the SMBH masses are predicted using either (a) the Graham & Scott (2013) "non-barred M BH − σ" relation (Table 4) or (b) their B-band core-Sérsic M BH − L relation which is converted here to the V -band using B − V = 1.0 (Fukugita et al 1995). Symbolic representations are as in Fig.…”

Section: Core Size Versus Black Hole Massmentioning

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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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: Core Size Versus Black Hole Massmentioning

confidence: 89%

Section: Core Size Versus Black Hole Massmentioning

confidence: 99%

Section: Core Size Versus Black Hole Massmentioning

confidence: 99%

See 1 more Smart Citation

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

Dullo¹,

Graham²

2014

Monthly Notices of the Royal Astronomical Society

Self Cite

147

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“…Boyle & Terlevich 1998;Merloni et al 2004;Aird et al 2010;Madau & Dickinson 2014) and 4) a tight correlation is found between the BH and stellar mass of the host galaxy bulge (e.g. Magorrian et al 1998;McConnell & Ma 2013;Graham & Scott 2013;Kormendy & Ho 2013). There are several examples of composite objects showing both AGN and star formation activity, in the literature (e.g.…”

Section: Introductionmentioning

confidence: 99%

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Kalfountzou

Stevens

Jarvis

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Several studies support the existence of a link between the AGN and star formation activity. Radio jets have been argued to be an ideal mechanism for direct interaction between the AGN and the host galaxy. A drawback of previous surveys of AGN is that they are fundamentally limited by the degeneracy between redshift and luminosity in flux-density limited samples. To overcome this limitation, we present far-infrared Herschel observations of 74 radio-loud quasars (RLQs), 72 radio-quiet quasars (RQQs) and 27 radio galaxies (RGs), selected at 0.9 < z < 1.1 which span over two decades in optical luminosity. By decoupling luminosity from evolutionary effects, we investigate how the star formation rate (SFR) depends on AGN luminosity, radio-loudness and orientation. We find that: 1) the SFR shows a weak correlation with the bolometric luminosity for all AGN sub-samples, 2) the RLQs show a SFR excess of about a factor of 1.4 compared to the RQQs, matched in terms of black hole mass and bolometric luminosity, suggesting that either positive radio-jet feedback or radio AGN triggering are linked to star-formation triggering and 3) RGs have lower SFRs by a factor of 2.5 than the RLQ sub-sample with the same BH mass and bolometric luminosity. We suggest that there is some jet power threshold at which radio-jet feedback switches from enhancing star formation (by compressing gas) to suppressing it (by ejecting gas). This threshold depends on both galaxy mass and jet power.

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“…These empirical correlations suggest that the growth of the central SBH and the host galaxy are fundamentally interlinked. Active galactic nucleus (AGN) feedback may be responsible for the correlations observed (Silk & Rees 1998;King 2003;Fabian 2012), although it has also been argued that the origin of the observed relations is entirely non-causal and is a natural consequence of mergerdriven galaxy growth (Peng 2007;Jahnke & Macciò 2011;Graham & Scott 2013). The energy released from the central SBH is several orders more than the binding energy of massive galaxies (Fabian 2012).…”

Section: Introductionmentioning

confidence: 99%

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

Vaddi

O’Dea

Baum

et al. 2016

ApJ

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We address the relation between star formation and active galactic nucleus (AGN) activity in a sample of 231 nearby (0.0002 < z < 0.0358) early-type galaxies by carrying out a multi-wavelength study using archival observations in the UV, IR, and radio. Our results indicate that early-type galaxies in the current epoch are rarely powerful AGNs, with P 10 WHz 22 1 < -for a majority of the galaxies. Only massive galaxies are capable of hosting powerful radio sources while less massive galaxies are hosts to lower radio power sources. Evidence of ongoing star formation is seen in approximately 7% of the sample. The star formation rate (SFR) of these galaxies is less than 0.1 M e yr −1 . They also tend to be radio faint (P 10 WHzThere is a nearly equal fraction of star-forming galaxies in radio faint (P 10 WHz 22 1 < -) and radio bright galaxies (P 10 WHz 22 1  -) suggesting that both star formation and radio mode feedback are constrained to be very low in our sample. We notice that our galaxy sample and the Brightest Cluster Galaxies follow similar trends in radio power versus SFR. This may be produced if both radio power and SFR are related to stellar mass.

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THEM_BH-L_SPHEROIDRELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES

Cited by 257 publications

References 297 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

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

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