A new method to assign galaxy cluster membership using photometric redshifts

G. Castignani; C. Benoist

doi:10.1051/0004-6361/201528009

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Volume 595 (November 2016)

A&A, 595 (2016) A111

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Table 3

Richness results for different redshift intervals.

					N_halos	Log	z
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)

0.19 ± 0.11	−0.039 ± 0.10	0.11	0.14	0.14	179	14.01 ± 0.24	0.0–0.5
0.23 ± 0.13	−0.0069 ± 0.14	0.11	0.14	0.15	175	14.00 ± 0.21	0.5–0.75
0.25 ± 0.14	−0.0043 ± 0.14	0.12	0.17	0.18	245	13.90 ± 0.21	0.75–1.0
0.27 ± 0.15	0.0034 ± 0.17	0.12	0.19	0.21	229	13.84 ± 0.22	1.0–1.25
0.26 ± 0.14	−0.017 ± 0.15	0.12	0.17	0.18	159	13.79 ± 0.19	1.25–1.5
0.27 ± 0.15	0.0050 ± 0.17	0.15	0.19	0.21	127	13.73 ± 0.20	1.5–1.75
0.33 ± 0.14	0.061 ± 0.17	0.13	0.14	0.17	60	13.70 ± 0.18	1.75–2.0
0.29 ± 0.13	0.017 ± 0.15	0.13	0.16	0.18	33	13.68 ± 0.19	2.0–2.5

Notes. Column description. (1) Mean logarithmic difference between the estimated richness λ₁ = N_estimated and the true richness N_true, where the reported uncertainty is the rms dispersion around the mean and the richness λ₁ = N_estimated refers to galaxies with P_mem>Pthr = 20%; (2) as in Col. 1, but here the estimated richness λ₂ = ∑ P_mem is used; (3) rms dispersion around the mean of the logarithmic difference between the halo mass M_halo and the halo occupation number N_true; (4) rms dispersion around the mean of the logarithmic difference between the halo mass M_halo and the estimated richness λ₁ = N_estimated; (5) as in Col. 4, but here the estimated richness λ₂ = ∑ P_mem is used; (6) number of halos considered; (7) median logarithmic halo mass, the reported uncertainty is the rms dispersion; (8) redshift bin.

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