The clustering amplitude of X-ray-selected AGN at<i>z</i>∼ 0.8: evidence for a negative dependence on accretion luminosity

Mountrichas, G.; Georgakakis, A.; Menzel, Marie-Luise; Fanidakis, N.; Merloni, A.; Liu, Z.; Salvato, M.; Nandra, K.

doi:10.1093/mnras/stw281

Cited by 24 publications

(50 citation statements)

References 80 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…potential causes for this bias are discussed in the following section. Our lower-luminosity bin, on the other hand, resides in lower-mass halos consistent with the quasar and other X-ray AGN samples at similar luminosities and redshifts (e.g., quasars at z ∼ 1, log L bol ∼ 45; Laurent et al 2017; X-ray AGN at z ∼ 0.8, log L bol ∼ 44.9 and z ∼ 0.42, log L bol ∼ 45.2; Mountrichas et al 2016;Krumpe et al 2012), although the errors on our measurement are large. This indicates that there are also redshift and luminosity dependencies on the effective host halo masses found for AGN, due to both the growth of structure over cosmic time, as well as the scaling relations between supermassive black holes and their galaxies.…”

Section: Discussionsupporting

confidence: 80%

“…We selected the AGN in XMM-XXL-north with spectroscopic redshifts in the DR12 BOSS footprint. While the incompleteness of the spectroscopic redshifts affects the clustering on small angular scales (< 0.03 deg; Mountrichas et al 2016), this effect is small for the projected scales that we are interested in at the effective redshifts of our samples (z ∼ 0.7 and z ∼ 1.8, corresponding to 0.9 and 1.2 Mpc h −1 , respectively). The integrated sensitivity curves are shown in Figure 1 (Georgakakis et al 2008).…”

Section: Xmm-xxlmentioning

confidence: 92%

See 1 more Smart Citation

The Clustering of X-Ray Luminous Quasars

Powell

Urry

Cappelluti

et al. 2020

ApJ

View full text Add to dashboard Cite

The clustering of active galactic nuclei (AGN) sheds light on their typical large (Mpc-scale) environments, which can constrain the growth and evolution of supermassive black holes. Here we measure the clustering of luminous X-ray-selected AGN in the Stripe 82X and XMM-XXL-north surveys around the peak epoch of black hole growth, in order to investigate the dependence of luminosity on largescale AGN environment. We compute the auto-correlation function of AGN in two luminosity bins, 10 43 ≤ L X < 10 44.5 erg s −1 at z ∼ 0.8 and L X ≥ 10 44.5 erg s −1 at z ∼ 1.8, and calculate the AGN bias taking into account the redshift distribution of the sources using three different methods. Our results show that while the less luminous sample has an inferred typical halo mass that is smaller than for the more luminous AGN, the host halo mass may be less dependent on luminosity than suggested in previous work. Focusing on the luminous sample, we calculate a typical host halo mass of ∼ 10 13 M h −1 , which is similar to previous measurements of moderate-luminosity X-ray AGN and significantly larger than the values found for optical quasars of similar luminosities and redshifts. We suggest that the clustering differences between different AGN selection techniques are dominated by selection biases, and not due to a dependence on AGN luminosity. We discuss the limitations of inferring AGN triggering mechanisms from halo masses derived by large-scale bias.

show abstract

Section: Discussionsupporting

confidence: 80%

Section: Xmm-xxlmentioning

confidence: 92%

The Clustering of X-Ray Luminous Quasars

Powell

Urry

Cappelluti

et al. 2020

ApJ

View full text Add to dashboard Cite

show abstract

“…This is highlighted by the use of large values of π max 200 h −1 Mpc (Georgakakis et al 2014;Allevato et al 2016) versus studies with only spectroscopic redshifts with π max 100 h −1 Mpc (e.g. Coil et al 2009;Allevato et al 2011;Mountrichas et al 2016). Therefore, we select only Pdfs based on the following quality criteria: the comoving distance separation between the z min and z max may not exceed a critical value of ∆d = 100 h −1 Mpc.…”

Section: Generalized Estimatormentioning

confidence: 99%

The XMM-Newton wide field survey in the COSMOS field: Clustering dependence of X-ray selected AGN on host galaxy properties

Viitanen

Allevato

Finoguenov

et al. 2019

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We study the spatial clustering of 632 (1130) XMM-COSMOS Active Galactic Nuclei (AGNs) with known spectroscopic (spectroscopic or photometric) redshifts in the range z = [0.1 − 2.5] in order to measure the AGN bias and estimate the typical mass of the hosting dark matter (DM) halo as a function of AGN host galaxy properties. We create AGN subsamples in terms of stellar mass M * and specific black hole accretion rate L X /M * , to probe how AGN environment depends on these quantities. Further, we derive the M * − M halo relation for our sample of XMM-COSMOS AGNs and compare it to results in literature for normal non-active galaxies. Methods. We measure the projected two-point correlation function w p (r p ) using both the classic and the generalized clustering estimator based on photometric redshifts as probability distribution functions in addition to any available spectroscopic redshifts. We measure the large-scale (r p 1 h −1 Mpc) linear bias b by comparing the clustering signal to that expected of the underlying DM distribution. The bias is then related to the typical mass of the hosting halo M halo of our AGN subsamples. Since M * and L X /M * are correlated, we match the distribution in terms of one quantity, while split the distribution in the other. Results. For the full spectroscopic AGN sample, we measure a typical DM halo mass of log(M halo /h −1 M ⊙ ) = 12.79 +0.26 −0.43 , similar to galaxy group environments and in line with previous studies for moderate-luminosity X-ray selected AGN. We find no significant dependence on specific accretion rate L X /M * , with log(M halo /h −1 M ⊙ ) = 13.06 +0.23 −0.38 and log(M halo /h −1 M ⊙ ) = 12.97 +0.39 −1.26 for low and high L X /M * subsamples, respectively. We also find no difference in the hosting halos in terms of M * with log(M halo /h −1 M ⊙ ) = 12.93 +0.31 −0.62 (low) and log(M halo /h −1 M ⊙ ) = 12.90 +0.30 −0.62 (high). By comparing the M * − M halo relation derived for XMM-COSMOS AGN subsamples with what is expected for normal non-active galaxies by abundance matching and clustering results, we find that the typical DM halo mass of our high M * AGN subsample is similar to that of non-active galaxies. However, AGNs in our low M * subsample are found in more massive halos than non-active galaxies. By excluding AGNs in galaxy groups from the clustering analysis, we find evidence that the result for low M * may be due a larger fraction of AGNs as satellites in massive halos.

show abstract

“…This figure compares the observed r-band magnitude distribution of the sample of the XMM-XXL AGN presented by Georgakakis et al (2017a) in the photometric or spectroscopic redshift interval 0.6 < z < 1.0 with that predicted from the simulation. The magnitude limit r < 22.5 mag is applied to the XXM-XXL AGN light cone to mimic the spectroscopic follow-up selection of the Mountrichas et al (2016) sample.…”

Section: Appendix B: Light-cone For Vipers Galaxies and Xmm-xxl Agnmentioning

confidence: 99%

“…For the latter the observational and model histograms are normalised to the same area. The simulations corresponding to the Mountrichas et al (2016) sample (Appendix B) are shown on the left. These are compared with the redshift distribution of the AGN sample presented by Mountrichas et al (2016) in the interval of the mock light-cone z ≈ 0.6 − 1.0.…”

Section: Appendix E: Redshift Distributions Of Mock Agnmentioning

confidence: 99%

Exploring the halo occupation of AGN using dark-matter cosmological simulations

Georgakakis

Comparat

Merloni

et al. 2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

A semi-empirical model is presented that describes the distribution of Active Galactic Nuclei (AGN) on the cosmic web. It populates dark-matter halos in N-body simulations (MultiDark) with galaxy stellar masses using empirical relations based on abundance matching techniques, and then paints accretion events on these galaxies using stateof-the-art measurements of the AGN occupation of galaxies. The explicit assumption is that the large-scale distribution of AGN is independent of the physics of blackhole fueling. The model is shown to be consistent with current measurements of the two-point correlation function of AGN samples. It is then used to make inferences on the halo occupation of the AGN population. Mock AGN are found in halos with a broad distribution of masses with a mode of ≈ 10 12 h −1 M and a tail extending to cluster-size halos. The clustering properties of the model AGN depend only weakly on accretion luminosity and redshift. The fraction of satellite AGN in the model increases steeply toward more massive halos, in contrast with some recent observational results. This discrepancy, if confirmed, could point to a dependence of the halo occupation of AGN on the physics of black-hole fueling.

show abstract

The clustering amplitude of X-ray-selected AGN atz∼ 0.8: evidence for a negative dependence on accretion luminosity

Cited by 24 publications

References 80 publications

The Clustering of X-Ray Luminous Quasars

The Clustering of X-Ray Luminous Quasars

The XMM-Newton wide field survey in the COSMOS field: Clustering dependence of X-ray selected AGN on host galaxy properties

Exploring the halo occupation of AGN using dark-matter cosmological simulations

Contact Info

Product

Resources

About