Table 2.
Number of X-ray AGNs divided into bins of redshift and obscuration, and the results of the large-scale bias model.
zmin |
![]() |
zmax | NH, min |
![]() |
NH, max |
![]() |
N |
![]() |
![]() |
log MA11 | bA11 | b2 − halo | log M2 − halo |
---|---|---|---|---|---|---|---|---|---|---|---|---|---|
0.30 | 1.26 | 3.00 | − |
![]() |
− |
![]() |
5565 |
![]() |
0.95 |
![]() |
![]() |
![]() |
![]() |
0.30 | 1.23 | 3.00 | − |
![]() |
1022.0 |
![]() |
3660 |
![]() |
0.90 |
![]() |
![]() |
![]() |
![]() |
0.30 | 1.28 | 3.00 | 1022.0 |
![]() |
1023.5 |
![]() |
1664 |
![]() |
1.05 |
![]() |
![]() |
![]() |
![]() |
0.30 | 1.41 | 3.00 | 1023.5 |
![]() |
− |
![]() |
241 |
![]() |
1.33 |
![]() |
![]() |
![]() |
![]() |
0.30 | 0.69 | 1.10 | − |
![]() |
− |
![]() |
2642 |
![]() |
0.64 |
![]() |
![]() |
![]() |
![]() |
0.30 | 0.69 | 1.10 | − |
![]() |
1022.0 |
![]() |
1764 |
![]() |
0.62 |
![]() |
![]() |
![]() |
![]() |
0.30 | 0.69 | 1.10 | 1022.0 |
![]() |
1023.5 |
![]() |
769 |
![]() |
0.64 |
![]() |
![]() |
![]() |
![]() |
0.30 | 0.77 | 1.10 | 1023.5 |
![]() |
− |
![]() |
109 |
![]() |
0.87 |
![]() |
![]() |
![]() |
![]() |
1.10 | 1.77 | 3.00 | − |
![]() |
− |
![]() |
2923 |
![]() |
1.64 |
![]() |
![]() |
![]() |
![]() |
1.10 | 1.74 | 3.00 | − |
![]() |
1022.0 |
![]() |
1896 |
![]() |
1.62 |
![]() |
![]() |
![]() |
![]() |
1.10 | 1.79 | 3.00 | 1022.0 |
![]() |
1023.5 |
![]() |
895 |
![]() |
1.68 |
![]() |
![]() |
![]() |
![]() |
1.10 | 1.93 | 3.00 | 1023.5 |
![]() |
− |
![]() |
132 |
![]() |
1.76 |
![]() |
![]() |
![]() |
![]() |
Notes. Columns 1–8 correspond to the minimum, mean, and maximum redshift, z; the minimum, median, and maximum AGN hydrogen column density, NH (in cm−2); the median X-ray luminosity (in erg s−1 cm−2); and the number of AGNs. For NH and LX (large-scale bias and typical DM halo mass), the lower and upper limits correspond to 16% and 84% percentiles of the (bootstrap) distribution. Note that we consider 1020 cm−2 as the lower limit for unobscured AGNs. Columns 9–12 correspond to the weighted large-scale bias, weighted mean redshift, typical DM halo mass, and the corresponding large-scale bias assuming the results from Sheth et al. (2001) and van den Bosch (2002) and using the methodology set forth by Allevato et al. (2011). The last two columns show the best-fit two-halo bias as defined in Eq. (4) and the corresponding typical DM halo mass using the results from Sheth et al. (2001) and van den Bosch (2002).
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