Cosmic Evolution of Black Holes and Spheroids. III. The MBH-σ* Relation in the Last Six Billion Years

By J. Woo, T. Treu, M. Malkan, R. Blandford. 2008

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We measure the evolution of the correlation between black hole mass and host spheroid velocity dispersion (MBH-σ*) over the last 6 billion years, by studying three carefully selected samples of active galaxies at z = 0.57, z = 0.36 and z < 0.1. For all three samples, virial black hole masses are consistently estimated using the line dispersion of Hβ and the continuum luminosity at 5100 Å or Hα line luminosity, based on our cross calibration of the broad-line region size-luminosity relation. For the z = 0.57 sample, new stellar velocity dispersions are measured from high signal-to-noise ratio spectra obtained at the Keck Telescope, while for the two lower redshift samples they are compiled from previous works. Extending our previous result at z = 0.36, we find an offset from the local relation, suggesting that for fixed MBH, distant spheroids have on average smaller velocity dispersions than local ones. The measured offset at z = 0.57 is Δ log σ* = 0.12 ± 0.05 ± 0.06 (or Δ log MBH = 0.50 ± 0.22 ± 0.25), i.e., Δ log MBH = (3.1 ± 1.5) log (1 + z) + 0.05 ± 0.21. This is inconsistent with a tight and nonevolving universal MBH-σ* relation at the 95% CL.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3440b8afa93e7635db2270e8da34c45b569c848e

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Citations in the corpus

PRECISE BLACK HOLE MASSES FROM MEGAMASER DISKS: BLACK HOLE–BULGE RELATIONS AT LOW MASS (2010, background): “If they were to adopt a lower value of f , then the evidence for redshift evolution, which they report to be a factor of 2− 5 at z = 0.4, could disappear (Woo et al. 2008).”
Journey to the MBH-σ relation: the fate of low-mass black holes in the Universe (2009, methodology): “To push this scenario further, we have implemented a model where the MBH–σ correlation evolves with redshift as proposed by Woo et al. (2008), based on observations of z ∼ 0.5 AGN.”
ONGOING AND CO-EVOLVING STAR FORMATION IN zCOSMOS GALAXIES HOSTING ACTIVE GALACTIC NUCLEI (2008, result): “The observational situation is so far unclear: limited AGN samples at higher redshifts (Woo et al. 2006, 2008) show preferentially higher black hole masses relative to that expected by the local M − σ relation, while other studies of low redshift AGNs, undergoing substantial rates of accretion…”
PRIMUS: THE DEPENDENCE OF AGN ACCRETION ON HOST STELLAR MASS AND COLOR (2011, background): “It is also unclear if the Mbh−σ relation evolves with redshift or exists at all outside the local universe (e.g., Shields et al. 2003; Merloni 2004; Croton 2006; Peng et al. 2006a; Woo et al. 2006; Salviander et al. 2007; Woo et al. 2008; Merloni et al. 2010; Shen & Kelly 2010).”
An expanded Mbh–σ diagram, and a new calibration of active galactic nuclei masses (2010, background): “…hole masses from AGN spectra, the effects of changing f can be far-ranging, from individual objects to large AGN surveys (Barth, Greene & Ho 2005; Woo et al. 2006, 2008; Dong et al. 2007; Treu et al. 2007; Zhang, Dultzin-Hacyan & Wang 2007; Shen et al. 2008a,b; Vestergaard et al. 2008; Trump et…”
ON THE COSMIC EVOLUTION OF THE SCALING RELATIONS BETWEEN BLACK HOLES AND THEIR HOST GALAXIES: BROAD-LINE ACTIVE GALACTIC NUCLEI IN THE zCOSMOS SURVEY (2009, background): “An alternative path has been followed by Woo et al. (2006), Treu et al. (2007) and Woo et al. (2008), who have studied carefully selected samples of moderately bright AGN in narrow redshift ranges (z ∼ 0.36 and 0.57), where the host’s stellar velocity dispersion can be measured directly from the…”
Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation (2016, background): “On the other hand, most analyses based on Soltantype arguments or direct detections suggest that theMbh-σ relation evolves weakly if at all (e.g., Gaskell & Kormendy 2009; Shankar et al. 2009a; Zhang et al. 2012; Shen et al. 2015, but see also Woo et al. 2008).”
The quasar relation through cosmic time – II. Evidence for evolution from z = 3 to the present age (2009, background): “…despite the large efforts perfused both from a theoretical (e.g., Silk & Rees 1998; King 2005; Wyithe & Loeb 2006; Robertson et al. 2006; Hopkins et al. 2007; Malbon et al. 2007) and an observational point of view (McLure et al. 2006; Peng et al. 2006a,b; Salviander et al. 2007; Woo et al. 2008).”
The Illustris simulation: the evolving population of black holes across cosmic time (2014, background): “…for a given host galaxy at higher redshifts, black holes are more massive than their z = 0 counterparts (e.g. Treu et al. 2004; Shields et al. 2006; Woo et al. 2008; Merloni et al. 2010, for a review see Kormendy & Ho 2013), systematic uncertainties, selection effects and insufficient data do not…”
THE LOW-LUMINOSITY END OF THE RADIUS–LUMINOSITY RELATIONSHIP FOR ACTIVE GALACTIC NUCLEI (2013, background): “…et al. 2008; Vestergaard & Osmer 2009; Kelly et al. 2009; Schulze & Wisotzki 2010), cos mic evolution of black holes and their host galaxies (e.g., Woo et al. 2008; Merloni et al. 2010; Bennert et al. 2010), the na ture of narrow-line Seyfert 1 galaxies (e.g., Mathur et al. 2012; Papadakis et al.…”
Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime (2012, background): “However, the origin of the M• −σ relation (Ciotti et al., 2010, King, 2003, Silk and Rees, 1998, Wyithe and Loeb, 2003), and its evolution at look-back times is still unclear (Peng, 2007, Robertson et al., 2006, Treu et al., 2007, Woo et al., 2008).”
What drives the growth of black holes (2011, methodology): “Studies of broad-line quasars consistently find that the BH is overmassive relative to its host galaxy compared to the local relation (e.g., Walter et al., 2004; Woo et al., 2008; Decarli et al., 2010b; Bennert et al., 2010; Merloni et al., 2010).”
THE LICK AGN MONITORING PROJECT: THE MBH–σ* RELATION FOR REVERBERATION-MAPPED ACTIVE GALAXIES (2010, methodology): “The local AGN samples with single-epoch black hole masses selected from the SDSS are much larger than the reverberation sample (e.g., Greene & Ho 2006; Woo et al. 2008), but these mass estimates have larger uncertainties (∼ 0.5 dex) and may suffer from unknown systematic errors (Collin et al. 2006).”
The Spitzer/IRAC view of black hole–bulge scaling relations (2010, background): “For instance, Woo et al. (2008) report a significant evolution of the BH-bulge relations at z = 0.3 − 0.6, with larger BH masses for given bulge σ/luminosity with respect to local values.”
EDDINGTON-LIMITED ACCRETION AND THE BLACK HOLE MASS FUNCTION AT REDSHIFT 6 (2010, background): “Studies involving AGN tend to show higher than local ratios of MBH/Mstellar at all redshifts; z < 1 (Mathur & Grupe 2005; Woo et al. 2008), 1 < z < 4 (Peng et al. 2006; McLure et al. 2006; Merloni et al. 2010); z > 4 (Walter et al. 2004; Riechers et al. 2008; Wang et al. 2010), whereas studies…”