The Biases of Optical Line-Ratio Selection for Active Galactic Nuclei and the Intrinsic Relationship Between Black Hole Accretion and Galaxy Star Formation

Trump, Jonathan R.; Sun, Mouyuan; Zeimann, Gregory R.; Luck, Cuyler; Bridge, Joanna S.; Grier, C. J.; Hagen, Alex; Juneau, Stéphanie; Montero-Dorta, Antonio D.; Rosario, D. J.; Brandt, W. N.; Ciardullo, Robin; Schneider, Donald P.

doi:10.1088/0004-637x/811/1/26

Cited by 153 publications

(160 citation statements)

References 146 publications

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“…The best-fit intercept (−3.89) is »0.4 dex lower than that expected from the H14 model (i.e., −3.48; shown as the dotted lines in Figure 4); possible reasons are explained in Sections 3.3 and 3.5.1. Our intercept is also similar to the value (»-3.6) derived from Trump et al (2015), which is based on optically selected AGNs in the local universe ( < z 0.1). 26 In general, X-ray emission from XRBs (the dashed lines) is lower compared to that from AGNs, and it is less significant at high SFR.…”

Section: Bhar Dependence On Sfrsupporting

confidence: 86%

“…, especially in the low-z range (see the rightmost M * bins in the left panels of Figure 5); the dependence of á ñ BHAR on SFR in the high-M * regime is also suggested by some previous studies (e.g., Delvecchio et al 2015;Rodighiero et al 2015;Trump et al 2015). Rosario et al (2013) suggest that among massive galaxies with *  M 10 10.5 ☉ M , X-ray AGNs are more prevalent in high-SFR systems (see also, e.g., Azadi et al 2015).…”

Section: Bhar Dependence On Both Sfr and M *supporting

confidence: 81%

“…(e.g., Volonteri 2010;Miller et al 2015;Trump et al 2015). Due to the Eddington limit, the X-ray emission from accretion onto IMBHs is likely to be much weaker than that from SMBHs.…”

Section: Discussionmentioning

confidence: 99%

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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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Section: Bhar Dependence On Sfrsupporting

confidence: 86%

Section: Bhar Dependence On Both Sfr and M *supporting

confidence: 81%

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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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“…Thus, our measurements of p(λsBHAR) may not reflect the underlying distribution of Eddington ratios; in fact, our measurements track the convolution of the probability distribution of Eddington ratios and the distribution of black hole masses at a given galaxy stellar mass. Our measurements are also degenerate with the overall black hole occupation fraction: the low AGN duty cycle that we find could indicate that a large fraction of galaxies in this mass regime simply lack central massive black holes and thus would never be observed as an AGN (see also Trump et al 2015). It is not possible with the current data to break such degeneracies, although our measurements do provide a lower limit on the occupation fraction and show that actively accreting massive black holes can exist in such lowmass galaxies.…”

Section: Agn Activity In Dwarf Galaxiesmentioning

confidence: 80%

X-rays across the galaxy population – II. The distribution of AGN accretion rates as a function of stellar mass and redshift

Aird

Coil

Georgakakis

2017

Monthly Notices of the Royal Astronomical Society

167

266

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We use deep Chandra X-ray imaging to measure the distribution of specific black hole accretion rates (L X relative to the stellar mass of the galaxy) and thus trace AGN activity within star-forming and quiescent galaxies, as a function of stellar mass (from 10 8.5 -10 11.5 M ⊙ ) and redshift (to z ∼ 4). We adopt near-infrared selected samples of galaxies from the CANDELS and UltraVISTA surveys, extract X-ray data for every galaxy, and use a flexible Bayesian method to combine these data and to measure the probability distribution function of specific black hole accretion rates, λ sBHAR . We identify a broad distribution of λ sBHAR in both starforming and quiescent galaxies-likely reflecting the stochastic nature of AGN fuelling-with a roughly power-law shape that rises toward lower λ sBHAR , a steep cutoff at λ sBHAR 0.1−1 (in Eddington equivalent units), and a turnover or flattening at λ sBHAR 10 −3 − 10 −2 . We find that the probability of a star-forming galaxy hosting a moderate λ sBHAR AGN depends on stellar mass and evolves with redshift, shifting toward higher λ sBHAR at higher redshifts. This evolution is truncated at a point corresponding to the Eddington limit, indicating black holes may self-regulate their growth at high redshifts when copious gas is available. The probability of a quiescent galaxy hosting an AGN is generally lower than that of a star-forming galaxy, shows signs of suppression at the highest stellar masses, and evolves strongly with redshift. The AGN duty cycle in high-redshift (z 2) quiescent galaxies thus reaches ∼20 per cent, comparable to the duty cycle in star-forming galaxies of equivalent stellar mass and redshift.

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“…Most of these galaxies do not show signatures of AGNs in their optical emission line ratios, suggesting heavy obscuration or dilution of emission line ratios by vigorous star formation, both of which are well-known limitations to optical spectroscopic surveys in finding low luminosity AGNs (e.g., Goulding & Alexander 2009;Hopkins et al 2009;Trump et al 2015).…”

Section: Introductionmentioning

confidence: 99%

OBSCURED AGNs IN BULGELESS HOSTS DISCOVERED BY WISE: THE CASE STUDY OF SDSS J1224+5555

Satyapal¹,

Secrest²,

Rothberg³

et al. 2016

ApJ

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There is mounting evidence that supermassive black holes form and grow in bulgeless galaxies. However, a robust determination of the fraction of AGNs in bulgeless galaxies, an important constraint to models of supermassive black hole seed formation and merger-free models of AGN fueling, is unknown, since optical studies have been shown to be incomplete for low mass AGNs. In a recent study using the Wide-field Infrared Survey Explorer, we discovered hundreds of bulgeless galaxies that display mid-infrared signatures of extremely hot dust suggestive of powerful accreting massive black holes, despite having no signatures of black hole activity at optical wavelengths. Here we report X-ray follow-up observations of J122434.66+555522.3, a nearby (z = 0.052) isolated bulgeless galaxy that contains an unresolved X-ray source detected at the 3σ level by XMM-Newton with an observed luminosity uncorrected for intrinsic absorption of L 2−10 keV = (1.1 ± 0.4) × 10 40 erg s −1 . Groundbased near-infrared spectroscopy with the Large Binocular Telescope together with multiwavelength observations from ultraviolet to millimeter wavelengths together suggest that J1224+5555 harbors a highly absorbed AGN with an intrinsic absorption of N H > 10 24 cm −2 . The hard X-ray luminosity of the putative AGN corrected for absorption is L 2−10 keV ∼ 3 × 10 42 erg s −1 , which, depending on the bolometric correction factor, corresponds to a bolometric luminosity of the AGN of 6 × 10 43 erg s3 × 10 44 erg s −1 , and a lower mass limit for the black hole of M BH ≃ 2 × 10 6 M ⊙ , based on the Eddington limit. While enhanced X-ray emission and hot dust can be produced by star formation in extremely low metallicity environments typical in dwarf galaxies, J1224+5555 has a stellar mass of ∼ 2.0 × 10 10 M ⊙ , and an above solar metallicity (12+log O/H=9.11), typical of our WISE-selected bulgeless galaxies sample. While collectively, these observations suggest the presence of an AGN, we caution that identifying obscured AGNs in the low luminosity regime is challenging, and often requires multi wavelength observations.These observations suggest that low luminosity AGNs can be heavily obscured and reside in optically quiescent galaxies, adding to the growing body of evidence that the fraction of bulgeless galaxies with accreting black holes may be significantly underestimated based on optical studies.

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The Biases of Optical Line-Ratio Selection for Active Galactic Nuclei and the Intrinsic Relationship Between Black Hole Accretion and Galaxy Star Formation

Cited by 153 publications

References 146 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

X-rays across the galaxy population – II. The distribution of AGN accretion rates as a function of stellar mass and redshift

OBSCURED AGNs IN BULGELESS HOSTS DISCOVERED BY WISE: THE CASE STUDY OF SDSS J1224+5555

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