Advances in Astronomy

Review Article

Clustering of X-Ray-Selected AGN

Table 1

Cappelluti, Allevato, and Finoguenov.


Survey	Band keV
Survey				arcsec	h⁻¹ Mpc

EMSS	0.5–2	183	<0.2		<10
RASS	0.1–2.4	2158	1–1.5	~10	<10
RASS	0.1–2.4	2096	0.1	~3.7
ROSAT-NEP	0.1–2.4	220	0.22
AXIS¹	0.5–2	31288	0.96
AXIS¹	2–10	9188	0.94
AXIS¹	5–10	1259	0.77
ELAIS-S1	0.5–2	392	0.4			1.8
ELAIS-S1	2–10	205	0.4			1.8
CDFS	0.5–2	97	0.84
CDFN²	0.5–2	164	0.96
XMM-2dF³	0.5–2	432	1.2		16	1.8	1.9–2.7	12.5–13.1
XMM-LSS	0.5–2	1130	0.7
XMM-LSS	2–10	413	0.7
CLASXS	0.5–8	233	1.2
CDFN⁴	0.5–8	252	0.8
XMM-COSMOS⁵	0.5–2	1037	1.1		,	1.8
XMM-COSMOS⁵	2–4.5	545	0.9			1.8	2.5
XMM-COSMOS⁵	4.5–10	151	0.6			1.8	3.8
XMM-COSMOS⁶	0.5–2	538	0.98
XMM-COSMOS⁷	0.5–2	593	1.21
SWIFT-BAT	15–55	199	0.045				1.21
AEGIS	0.5–2	113	0.9				1.97
AGES	0.5–2	362	0.51
ROSAT + SDSS	0.1–2.4	1552	0.27
XMM-LSS	0.5–2	4360	1.1
XMM-LSS	2–10	1712	1.0

X: Unconstrained or undetermined, ^a: Bias factors converted to a common cosmology (, , ), ^b: DMH masses estimated using van den Bosch [54] and Sheth et al. [55], ¹: Ebrero et al. [42], fit , assuming no redshift evolution of the correlation length, ²: Gilli et al. [33], ³: Basilakos et al. [30], using the LDDE model, ⁴: Yang et al. [34], ⁵: Miyaji et al. [41], fit with integral constrain, assuming redshift evolution of the correlation length, ⁶: Gilli et al. [44], ⁷: Allevato et al. [45].