THE RELATION BETWEEN LUMINOUS AGNs AND STAR FORMATION IN THEIR HOST GALAXIES

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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“…Moreover, a recent study of luminous quasars also suggests that their BHAR might be primarily related to M * rather than SFR (Xu et al 2015).…”

Section: Bhar/sfr Ratio As a Function Of M *mentioning

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

134

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“…Simulations find that the physical processes that feed BH growth on small spatial scales are unlikely to be smooth or continuous, leading them to vary dramatically on short timescales (Hopkins & Quataert 2010;Hickox et al 2014). This variation may hide a strong underlying correlation with longer-lived SF activity (e.g., Gabor & Bournaud 2013;Hickox et al 2014;Neistein & Netzer 2014;Thacker et al 2014;Delvecchio et al 2015;Xu et al 2015). The relation between average BH growth and global SFRs, combined with the parallel redshift evolution of SF and AGN activity (see Madau & Dickinson 2014, for a review) and possible observations of an AGN MS (Mullaney et al 2012b), suggest an important link, the nature of which is still heavily debated.…”

Section: The Co-evolution Of Sf and Agns In Clustersmentioning

confidence: 99%

STAR FORMATION AND AGN ACTIVITY IN GALAXY CLUSTERS FROM z = 1–2: A MULTI-WAVELENGTH ANALYSIS FEATURING HERSCHEL/PACS

Alberts

Pope

Brodwin

et al. 2016

ApJ

100

117

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We present a detailed, multi-wavelength study of star formation (SF) and active galactic nucleus (AGN) activity in 11 near-infrared (IR) selected, spectroscopically confirmed massive (10 14 M e ) galaxy clusters at 1 < z < 1.75. Using new deep Herschel/PACS imaging, we characterize the optical to far-IR spectral energy distributions (SEDs) for IR-luminous cluster galaxies, finding that they can, on average, be well described by field galaxy templates. Identification and decomposition of AGNs through SED fittings allows us to include the contribution to cluster SF from AGN host galaxies. We quantify the star-forming fraction, dust-obscured SF rates (SFRs) and specific SFRs for cluster galaxies as a function of cluster-centric radius and redshift. In good agreement with previous studies, we find that SF in cluster galaxies at z  1.4 is largely consistent with field galaxies at similar epochs, indicating an era before significant quenching in the cluster cores (r < 0.5 Mpc). This is followed by a transition to lower SF activity as environmental quenching dominates by z ∼ 1. Enhanced SFRs are found in lower mass (   < < M M 10.1 log 10.8) cluster galaxies. We find significant variation in SF from cluster to cluster within our uniformly selected sample, indicating that caution should be taken when evaluating individual clusters. We examine AGNs in clusters from z = 0.5-2, finding an excess AGN fraction at z  1, suggesting environmental triggering of AGNs during this epoch. We argue that our results-a transition from field-like to quenched SF, enhanced SF in lower mass galaxies in the cluster cores, and excess AGNs-are consistent with a co-evolution between SF and AGNs in clusters and an increased merger rate in massive halos at high redshift.

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“…Quasi-stellar objects (QSOs), the manifestation of dramatic accretion onto SMBHs, are the key stage of SMBH growth and represent an important phase in the evolution of massive galaxies (Sanders et al 1988;Hopkins et al 2006). Probing the properties of quasar hosts, e.g., host morphology (Dunlop et al 2003), color (Jahnke et al 2004), interstellar medium (Xia et al 2012;Petric et al 2015), and star formation behavior (Shi et al 2007(Shi et al , 2014Xu et al 2015a), is essential to understanding the environment where SMBHs grow, and to gain insights into the circumstances influencing coevolution.…”

Section: Introductionmentioning

confidence: 99%

Distribution of Quasar Hosts on the Galaxy Main Sequence Plane

Zhang

Shi

Rieke

et al. 2016

ApJL

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The relation between star formation rates (SFRs) and stellar masses, i.e., the galaxy main sequence, is a useful diagnostic of galaxy evolution. We present the distributions relative to the main sequence of 55 optically selected PG and 12 near-IR-selected Two Micron All Sky Survey (2MASS) quasars at z0.5. We estimate the quasar host stellar masses from Hubble Space Telescope or ground-based AO photometry, and the SFRs through the midinfrared aromatic features and far-IR photometry. We find that PG quasar hosts more or less follow the main sequence defined by normal star-forming galaxies while 2MASS quasar hosts lie systematically above the main sequence. PG and 2MASS quasars with higher nuclear luminosities seem to have higher specific SFRs (sSFRs), although there is a large scatter. No trends are seen between sSFRs and SMBH masses, Eddington ratios, or even morphology types (ellipticals, spirals, and mergers). Our results could be placed in an evolutionary scenario with quasars emerging during the transition from ULIRGs/mergers to ellipticals. However, combined with results at higher redshift, they suggest that quasars can be widely triggered in normal galaxies as long as they contain abundant gas and have ongoing star formation.

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THE RELATION BETWEEN LUMINOUS AGNs AND STAR FORMATION IN THEIR HOST GALAXIES

Cited by 57 publications

References 92 publications

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

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

STAR FORMATION AND AGN ACTIVITY IN GALAXY CLUSTERS FROM z = 1–2: A MULTI-WAVELENGTH ANALYSIS FEATURING HERSCHEL/PACS

Distribution of Quasar Hosts on the Galaxy Main Sequence Plane

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