Evolution in the Black Hole–galaxy Scaling Relations and the Duty Cycle of Nuclear Activity in Star-Forming Galaxies

Trump, Jonathan R.; Brandt, W. N.; Alexander, D. M.; Jahnke, K.; Rosario, D. J.; Wang, Sharon X.; Xue, Yongquan

doi:10.1088/0004-637x/802/1/14

Cited by 82 publications

(101 citation statements)

References 127 publications

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“…Our interpretation of the observed σ − M * BH,vir relation at high z is therefore fundamentally different from Woo et al, in that we believe the differences seen between high-z and low-z samples are mainly not due to real evolution, but largely caused by selection biases and BH mass uncertainties in luminositythreshold quasar samples, as emphasized in several recent studies (e.g., Lauer et al 2007;Salviander et al 2007;Jahnke et al 2009;Shen & Kelly 2010;Schulze & Wisotzki 2011, 2014Salviander & Shields 2013;Schramm & Silverman 2013;Shen 2013;Matsuoka et al 2014;Sun et al 2015). Indeed, Figure 7.…”

Section: Discussioncontrasting

confidence: 69%

THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: NO EVIDENCE FOR EVOLUTION IN THE ${{M}_{\bullet }}-{{\sigma }_{*}}$ RELATION TO $z\sim 1$

Shen

Greene

et al. 2015

ApJ

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108

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We present host stellar velocity dispersion measurements for a sample of 88 broad-line quasars at < < z 0.1 1 (46 at > z 0.6) from the Sloan Digital Sky Survey Reverberation Mapping (SDSS-RM) project. High signal-to-noise ratio coadded spectra (average ≈ S N 30 per 69 − km s 1 pixel) from SDSS-RM allowed for the decomposition of the host and quasar spectra and for measurements of the host stellar velocity dispersions and black hole (BH) masses using the single-epoch ( ) lead to the first clear detection of a correlation between SE virial BH mass and host stellar velocity dispersion far beyond the local universe. However, the observed correlation is significantly flatter than the local relation, suggesting that there are selection biases in high-z luminosity-threshold quasar samples for such studies. Our uniform sample and analysis enable an investigation of the redshift evolution of the σ − M *• relation relatively free of caveats by comparing different samples/analyses at disjoint redshifts. We do not observe evolution of the σ − M *• relation in our sample up to ∼ z 1, but there is an indication that the relation flattens toward higher redshifts. Coupled with the increasing threshold luminosity with redshift in our sample, this again suggests that certain selection biases are at work, and simple simulations demonstrate that a constant σ − M * • relation is favored to ∼ z 1. Our results highlight the scientific potential of deep coadded spectroscopy from quasar monitoring programs, and offer a new path to probe the co-evolution of BHs and galaxies at earlier times.

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Section: Discussioncontrasting

confidence: 69%

THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: NO EVIDENCE FOR EVOLUTION IN THE ${{M}_{\bullet }}-{{\sigma }_{*}}$ RELATION TO $z\sim 1$

Shen

Greene

et al. 2015

ApJ

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108

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“…Sun et al (2015) also find general co-evolution of galaxies and their black holes, which is consistent with no deviation in the MBH/M * ratio from z = 2 → 0. However, they specifically find that low-z disk black holes appear to grow faster than their galaxies, often with sṀBH > 10 −9 yr −1 .…”

Section: Smbh Growth Rates In Star-forming Galaxiessupporting

confidence: 78%

“…Recent work shows that disk-dominated galaxies host lowluminosity AGN, which is critical for our hypothesis since COS-Halos star-forming galaxies are disk galaxies. Sun et al (2015) compiled an X-ray-selected, Herschel cross-matched sample of disk-dominated galaxies with AGN calculating a duty cycle of ≈ 10% with an average λ Edd ∼ 0.1.…”

Section: Agn Luminosities and Duty Cycles In Star-forming Galaxiesmentioning

confidence: 99%

Flickering AGN can explain the strong circumgalactic O viobserved by COS-Halos

Oppenheimer¹,

Segers

Schaye

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Proximity zone fossils (PZFs) are ionization signatures around recently active galactic nuclei (AGN) where metal species in the circumgalactic medium remain overionized after the AGN has shut-off due to their long recombination timescales. We explore cosmological zoom hydrodynamic simulations using the EAGLE model paired with a non-equilibrium ionization and cooling module including time-variable AGN radiation to model PZFs around star-forming, disk galaxies in the z ∼ 0.2 Universe. Previous simulations typically under-estimated the O vi content of galactic haloes, but we show that plausible PZF models increase O vi column densities by 2 − 3× to achieve the levels observed around COS-Halos star-forming galaxies out to 150 kpc. Models with AGN bolometric luminosities 10 43.6 erg s −1 , duty cycle fractions 10%, and AGN lifetimes 10 6 yr are the most promising, because their supermassive black holes grow at the cosmologically expected rate and they mostly appear as inactive AGN, consistent with COS-Halos. The central requirement is that the typical star-forming galaxy hosted an active AGN within a timescale comparable to the recombination time of a high metal ion, which for circumgalactic O vi is ≈ 10 7 years. H i, by contrast, returns to equilibrium much more rapidly due to its low neutral fraction and does not show a significant PZF effect. O vi absorption features originating from PZFs appear narrow, indicating photo-ionization, and are often well-aligned with lower metal ion species. PZFs are highly likely to affect the physical interpretation of circumgalactic high ionization metal lines if, as expected, normal galaxies host flickering AGN.

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“…As discussed above, observations of SMGs support this scenario. Some studies of high-redshift quasars find higher M BH /M * ratios than the local values, not expected in our scheme (e.g., Ho 2007; Merloni et al 2010; but also see, e.g., Jahnke et al 2009;Sun et al 2015). However, the M BH /M * measured from quasars might be biased and not representative for the majority of galaxies (e.g., Lauer et al 2007).…”

Section: Discussioncontrasting

confidence: 48%

“…The SEDs of broad-line AGNs often have significant accretion disk emission besides their starlight. Their SFR and M * measurements from SED fitting have potential large uncertainties (e.g., Bongiorno et al 2012;Sun et al 2015). Thus, we exclude the 19 broadline AGNs reported in the literature (e.g., Mignoli et al 2005;Ravikumar et al 2007;Silverman et al 2010) and discuss the effects of their exclusion in Section 3.5.1.…”

Section: Sample Selectionmentioning

confidence: 99%

Black Hole Growth Is Mainly Linked to Host-galaxy Stellar Mass Rather Than Star Formation Rate

Yang

Chen

Vito

et al. 2017

ApJ

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134

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Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe investigate the dependence of black hole accretion rate (BHAR) on host-galaxy star formation rate (SFR) and stellar mass (M * ) in the CANDELS/GOODS-South field in the redshift range of  < z 0.5 2.0. Our sample consists of »18,000 galaxies, allowing us to probe galaxies with . We use sample-mean BHAR to approximate long-term average BHAR. Our samplemean BHARs are derived from the Chandra Deep Field-South 7Ms observations, while the SFRs and M * have been estimated by the CANDELS team through spectral energy distribution fitting. The average BHAR is correlated positively with both SFR and M * , and the BHAR-SFR and BHAR-M * relations can both be described acceptably by linear models with a slope of unity. However, BHAR appears to be correlated more strongly with M * than SFR. This result indicates that M * is the primary host-galaxy property related to supermassive black hole (SMBH) growth, and the apparent BHAR-SFR relation is largely a secondary effect due to the star-forming main sequence. Among our sources, massive galaxies ( *  ☉ M M 10 10) have significantly higher BHAR/SFR ratios than less massive galaxies, indicating that the former have higher SMBH fueling efficiency and/or higher SMBH occupation fraction than the latter. Our results can naturally explain the observed proportionality between M BH and M * for local giant ellipticals and suggest that their * M M BH is higher than that of local star-forming galaxies. Among local star-forming galaxies, massive systems might have higher * M M BH compared to dwarfs.

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Evolution in the Black Hole–galaxy Scaling Relations and the Duty Cycle of Nuclear Activity in Star-Forming Galaxies

Cited by 82 publications

References 127 publications

THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: NO EVIDENCE FOR EVOLUTION IN THE ${{M}_{\bullet }}-{{\sigma }_{*}}$ RELATION TO $z\sim 1$

THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: NO EVIDENCE FOR EVOLUTION IN THE ${{M}_{\bullet }}-{{\sigma }_{*}}$ RELATION TO $z\sim 1$

Flickering AGN can explain the strong circumgalactic O viobserved by COS-Halos

Black Hole Growth Is Mainly Linked to Host-galaxy Stellar Mass Rather Than Star Formation Rate

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