The role of environment in the morphological transformation of galaxies in 9 rich intermediate redshift clusters

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Volume 505 / No 1 (October I 2009)

A&A, 505 1 (2009) 83-96

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Table 1:

Main properties of clusters in our sample.
ID	$\alpha$ (J2000)	$\delta$ (J2000)	z	L_X	r₂₀₀
				(10^-37 W)	(Mpc)
MS 0015.9+1609	00:18:33.33	+16:26:44.6	0.54 [2]	15.5 [2]	2.11 [3]
MS 0451.5-0305	04:54:10.796	-03:00:53.0	0.54 [2]	23.7 [2]	1.47 [3]
MS 1621.5+2640	16:23:35.6277	+26:34:09.49	0.43 [2]	9.47 [2]	1.5 [3]
MS1241.5+1710	12:44:01.4	+16:53:42	0.55 [2]	1.73 [2]	1.7 [3]
RXC J0856.1+3756	08:56:08.5	+37:56:52	0.41 [1]	15.76 [1]	1.59 [3]
RX J1003.0+3757	10:03:02.74	+37:57:51.5	0.41 [1]	8.29 [1]	1.48 [3]
RX J1120+4318	11:20:07.5	+43:18:05	0.60 [2]	6.07 [2]	1.3 [3]
RXC J1206.2-0848	12:06:13.1	-08:47:43	0.44	-	2.0 [3]
RXC J2228.6+2036	22:28:37.1	+20:36:31	0.41 [1]	29.62 [1]	1.62 [3]

[1] Böhringer et al. (2000); [2] Sadat et al. (2004); [3] Foex et al. 2009, in prep. r₂₀₀ are computed through a 1D weak-lensing analysis, i.e. fit of the radial shear profile and are defined as the radius at which the density is 200 times the critical density of the Universe at the cluster redshift.

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