SECULAR EVOLUTION AND A NON-EVOLVING BLACK-HOLE-TO-GALAXY MASS RATIO IN THE LAST 7 Gyr

Cisternas, Mauricio; Jahnke, K.; Bongiorno, A.; Inskip, K. J.; Impey, C. D.; Koekemoer, Anton M.; Merloni, A.; Salvato, M.; Trump, Jonathan R.

doi:10.1088/2041-8205/741/1/l11

Cited by 222 publications

(276 citation statements)

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“…Lauer et al (2007) discussed how such a bias could affect studies of SMBH mass scaling relations using broad-line AGNs outside the local universe. In fact, recent studies have found tentative evidence for strong evolution in the scaling between M bh and host spheroid mass (e.g., Treu et al 2007;Jahnke et al 2009;Merloni et al 2010;Bennert et al 2011b; although see also Alexander et al 2008;Cisternas et al 2011). Our model, which assumes a constant scaling and scatter in the M bh -M * relation, may provide a simple explanation for such findings, although a full investigation is beyond the scope of this paper (see also Schulze & Wisotzki 2011;Volonteri & Stark 2011;Salviander & Shields 2013).…”

Section: The Nature Of the Agn Populationmentioning

confidence: 65%

PRIMUS: AN OBSERVATIONALLY MOTIVATED MODEL TO CONNECT THE EVOLUTION OF THE ACTIVE GALACTIC NUCLEUS AND GALAXY POPULATIONS OUT TOz∼ 1

Aird¹,

Coil²,

Moustakas³

et al. 2013

ApJ

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We present an observationally motivated model to connect the active galactic nucleus (AGN) and galaxy populations at 0.2 < z < 1.0 and predict the AGN X-ray luminosity function (XLF). We start with measurements of the stellar mass function of galaxies (from the Prism Multi-object Survey) and populate galaxies with AGNs using models for the probability of a galaxy hosting an AGN as a function of specific accretion rate. Our model is based on measurements indicating that the specific accretion rate distribution is a universal function across a wide range of host stellar masses with slope γ 1 ≈ −0.65 and an overall normalization that evolves with redshift. We test several simple assumptions to extend this model to high specific accretion rates (beyond the measurements) and compare the predictions for the XLF with the observed data. We find good agreement with a model that allows for a break in the specific accretion rate distribution at a point corresponding to the Eddington limit, a steep power-law tail to super-Eddington ratios with slope γ 2 = −2.1 +0.3 −0.5 , and a scatter of 0.38 dex in the scaling between black hole and host stellar mass. Our results show that samples of low luminosity AGNs are dominated by moderately massive galaxies (M * ∼ 10 10 -10 11 M ) growing with a wide range of accretion rates due to the shape of the galaxy stellar mass function rather than a preference for AGN activity at a particular stellar mass. Luminous AGNs may be a severely skewed population with elevated black hole masses relative to their host galaxies and in rare phases of rapid accretion.

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Section: The Nature Of the Agn Populationmentioning

confidence: 65%

PRIMUS: AN OBSERVATIONALLY MOTIVATED MODEL TO CONNECT THE EVOLUTION OF THE ACTIVE GALACTIC NUCLEUS AND GALAXY POPULATIONS OUT TOz∼ 1

Aird¹,

Coil²,

Moustakas³

et al. 2013

ApJ

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“…Given the importance of these BH scaling relations in our understanding of galaxy formation and evolution, there have been extensive observational efforts in the past decade both to refine the measurements of the local relations (e.g., Ferrarese & Merritt 2000;Gebhardt et al 2000a;Graham et al 2001Graham et al , 2011Tremaine et al 2002;Marconi & Hunt 2003;Häring and Rix 2004;Aller & Richstone 2007;Bentz et al 2009;Gültekin et al 2009;Kormendy & Ho 2013;McConnell & Ma 2013, and references therein) and to probe their possible redshift evolution (e.g., Treu et al 2004Treu et al , 2007Peng et al 2006aPeng et al , 2006bWoo et al 2006Woo et al , 2008Salviander et al 2007;Shen et al 2008b;Jahnke et al 2009;McLeod & Bechtold 2009;Bennert et al 2010;Decarli et al 2010;Merloni et al 2010;Cisternas et al 2011;Canalizo et al 2012;Hiner et al 2012;Targett et al 2012;Salviander & Shields 2013;Bongiorno et al 2014;Matsuoka et al 2014). Given the small angular size of the sphere of influence of the BH, so far all measurements beyond the local universe are based on broad-line quasar samples, where the BH mass can be estimated using the properties of the broad lines, instead of spatially resolved gas or stellar kinematics.…”

Section: Introductionmentioning

confidence: 99%

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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110

151

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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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“…Other less important quenching mechanisms that affect central galaxies are mergers which could deplete the amount of cold gas available in the galaxy by triggering star formation (Mihos & Hernquist, 1996;Lambas et al, 2003;Woods et al, 2006;Bridge et al, 2007), secular processes such as morphological quenching (Kormendy & Kennicutt, 2004;Martig et al, 2009;Cisternas et al, 2011), and halo or mass quenching which ties quenching together with hot gas mass (Dekel & Birnboim, 2006;Cattaneo et al, 2006;Birnboim et al, 2007;Dekel et al, 2009;Gabor & Davé, 2015).…”

Section: Introductionmentioning

confidence: 99%

The diversity of growth histories of Milky Way-mass galaxies

Terrazas

Bell

Henriques

et al. 2016

Mon. Not. R. Astron. Soc.

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We use the semi-analytic model developed by Henriques et al. (2015) to explore the origin of star formation history diversity for galaxies that lie at the centre of their dark matter haloes and have present-day stellar masses in the range 5 − 8 × 10 10 M , similar to that of the Milky Way. In this model, quenching is the dominant physical mechanism for introducing scatter in the growth histories of these galaxies. We find that present-day quiescent galaxies have a larger variety of growth histories than starformers since they underwent 'staggered quenching' -a term describing the correlation between the time of quenching and present-day halo mass. While halo mass correlates broadly with quiescence, we find that quiescence is primarily a function of black hole mass, where galaxies quench when heating from their active galactic nuclei becomes sufficient to offset the redshift-dependent cooling rate. In this model, the emergence of a prominent quiescent population is the main process that flattens the stellar masshalo mass relation at mass scales at or above that of the Milky Way.

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SECULAR EVOLUTION AND A NON-EVOLVING BLACK-HOLE-TO-GALAXY MASS RATIO IN THE LAST 7 Gyr

Cited by 222 publications

References 50 publications

PRIMUS: AN OBSERVATIONALLY MOTIVATED MODEL TO CONNECT THE EVOLUTION OF THE ACTIVE GALACTIC NUCLEUS AND GALAXY POPULATIONS OUT TOz∼ 1

PRIMUS: AN OBSERVATIONALLY MOTIVATED MODEL TO CONNECT THE EVOLUTION OF THE ACTIVE GALACTIC NUCLEUS AND GALAXY POPULATIONS OUT TOz∼ 1

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

The diversity of growth histories of Milky Way-mass galaxies

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