THE SPATIAL CLUSTERING OF<i>ROSAT</i>ALL-SKY SURVEY ACTIVE GALACTIC NUCLEI. IV. MORE MASSIVE BLACK HOLES RESIDE IN MORE MASSIVE DARK MATTER HALOS

Krumpe, M.; Miyaji, Takeshi; Fanidakis, N.; Coil, Alison L.; Aceves, H.

doi:10.1088/0004-637x/815/1/21

Cited by 45 publications

(64 citation statements)

References 111 publications

(221 reference statements)

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“…Future observations and modelling can reduce uncertainties in bolometric corrections and the contribution of obscured accretion. They can also test our predictions against direct observations of the (non)-evolving M bh -Mstar relation (Suh et al 2019, submitted), AGN and quasar clustering (e.g., Shankar et al 2010), and the cross-correlation of AGN and galaxies (e.g., Krumpe et al 2015).…”

Section: Discussionmentioning

confidence: 61%

Probing black hole accretion tracks, scaling relations, and radiative efficiencies from stacked X-ray active galactic nuclei

Shankar

Weinberg

Marsden

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The masses of supermassive black holes at the centres of local galaxies appear to be tightly correlated with the mass and velocity dispersions of their galactic hosts. However, the local M bh -M star relation inferred from dynamically measured inactive black holes is up to an order-of-magnitude higher than some estimates from active black holes, and recent work suggests that this discrepancy arises from selection bias on the sample of dynamical black hole mass measurements. In this work we combine X-ray measurements of the mean black hole accretion luminosity as a function of stellar mass and redshift with empirical models of galaxy stellar mass growth, integrating over time to predict the evolving M bh -M star relation. The implied relation is nearly independent of redshift, indicating that stellar and black hole masses grow, on average, at similar rates. Matching the de-biased local M bh -M star relation requires a mean radiative efficiency ε 0.15, in line with theoretical expectations for accretion onto spinning black holes. However, matching the "raw" observed relation for inactive black holes requires ε ∼ 0.02, far below theoretical expectations. This result provides independent evidence for selection bias in dynamically estimated black hole masses, a conclusion that is robust to uncertainties in bolometric corrections, obscured active black hole fractions, and kinetic accretion efficiency. For our fiducial assumptions, they favour moderate-to-rapid spins of typical supermassive black holes, to achieve ε ∼ 0.12 − 0.20. Our approach has similarities to the classic Soltan analysis, but by using galaxy-based data instead of integrated quantities we are able to focus on regimes where observational uncertainties are minimized.

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Section: Discussionmentioning

confidence: 61%

Probing black hole accretion tracks, scaling relations, and radiative efficiencies from stacked X-ray active galactic nuclei

Shankar

Weinberg

Marsden

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Assuming a bolometric correction, the specific BHAR can be considered as a proxy of the Eddington ratio (Equation 1). Krumpe et al (2015) found no statistically significant clustering dependence on λ Edd for RASS Type 1 AGN at 0.16 < z < 0.36. Our results suggest the same constant bias evolution with Eddington ratio for both RASS Type 1 and COSMOS Type 2 AGN at different redshifts.…”

Section: Clustering Dependence On λ Bhar and Sfrmentioning

confidence: 66%

ChandraCOSMOS Legacy Survey: Clustering dependence of Type 2 active galactic nuclei on host galaxy properties

Allevato

Viitanen

Finoguenov

et al. 2019

A&A

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Aims. We perform clustering measurements of 800 X-ray selected Chandra COSMOS Legacy (CCL) Type 2 AGN with known spectroscopic redshift to probe the halo mass dependence on AGN host galaxy properties, such as galaxy stellar mass M star , star formation rate (SFR) and specific black hole accretion rate λ BHAR , in the redshift range z = [0 -3]. Methods. We split the sample of AGN with known spectroscopic redshits according to M star , SFR and λ BHAR , while matching the distributions in terms of the other parameters, including redshift. We measure the projected two-point correlation function w p (r p ) and model it with the 2-halo term to derive the large-scale bias b and the corresponding typical mass of the hosting halo, for the different subsamples.Results. We found no significant dependence of the large-scale bias and typical halo mass on galaxy stellar mass and specific BHAR for CCL Type 2 AGN at mean z∼1, while a negative dependence on SFR is observed, with lower SFR AGN residing in richer environment. Mock catalogs of AGN matched to have the same X-ray luminosity, stellar mass, λ BHAR and SFR of CCL Type 2 AGN, almost reproduce the observed M star − M h , λ BHAR − M h and SFR-M h relations, when assuming a fraction of satellite AGN f sat AGN ∼ 0.15, which corresponds to a ratio between the probabilities of satellite and central AGN of being active Q ∼ 2. Mock matched normal galaxies follow a slightly steeper M star − M h relation -with low mass mock galaxies residing in less massive halos than mock AGN of similar mass, and are less biased than mock AGN with similar specific BHAR and SFR, at least for Q > 1.

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“…These results indicate that the existence of an active SMBH does no seem to affect the clustering properties of the galaxy it lives in. Previous clustering studies that used X-ray and optically-selected AGN found a weak clustering dependence on black hole mass and no significant dependence on Eddington ratio (Krumpe et al 2015). Therefore, the AGN clustering seems to be (nearly) independent of the AGN properties, but it depends on the properties of the host galaxy.…”

Section: Discussionmentioning

confidence: 82%

The dependence of the X-ray AGN clustering on the properties of the host galaxy

Mountrichas

Georgakakis

Georgantopoulos

2018

Monthly Notices of the Royal Astronomical Society

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We study the clustering dependence of X-ray AGN and normal galaxies on the stellar mass (M ), star-formation rate (SFR) and specific star-formation rate (sSFR) of the (host) galaxy. Towards this end, we use 407 X-ray AGN from the XMM-XXL survey (∼ 25 deg 2 in the North) and ∼ 45, 000 galaxies in the VIPERS field (W1: ∼16 deg 2 ). We match the AGN and galaxy samples to have the same M , SFR and redshift distributions. Based on our results, the two populations live in DMHs with similar mass (log M/(M h −1 ) ≈ 12.8) and have similar dependence on the galaxy properties. Specifically, our measurements show a positive dependence of the AGN and galaxy clustering on M and a negative dependence on SFR and sSFR. We also find that the X-ray clustering is independent of the location of the host galaxy above or below the star-forming main sequence.

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THE SPATIAL CLUSTERING OFROSATALL-SKY SURVEY ACTIVE GALACTIC NUCLEI. IV. MORE MASSIVE BLACK HOLES RESIDE IN MORE MASSIVE DARK MATTER HALOS

Cited by 45 publications

References 111 publications

Probing black hole accretion tracks, scaling relations, and radiative efficiencies from stacked X-ray active galactic nuclei

Probing black hole accretion tracks, scaling relations, and radiative efficiencies from stacked X-ray active galactic nuclei

ChandraCOSMOS Legacy Survey: Clustering dependence of Type 2 active galactic nuclei on host galaxy properties

The dependence of the X-ray AGN clustering on the properties of the host galaxy

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