The GALEX Ultraviolet Virgo Cluster Survey (GUViCS) - IV. The role of the cluster environment on galaxy evolution

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Volume 570 (October 2014)

A&A, 570 (2014) A69

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Table 3

Properties of the different cluster substructures (see Fig. 1).

Substructure	RA(J2000)	Dec	Radius	Velocity range	Dist^a	⟨ vel ⟩	σ	N .	ρ ^b	Central galaxy
	°	°	°	km s^-1	Mpc	km s^-1	km s^-1		N gal Mpc^-3

Cluster A	187.71	12.39	<2.692^c	<3500	17	955	799	234	110	M87
Cluster B	187.44	8.00	<1.667^c	<3500	23	1134	464	66	53	M49
Cluster C	190.85	11.45	<0.7	<3500	17	1073	545	19	507	M60
W cloud	185.00	5.80	<1.2	1000 <vel< 3500	32	2176	416	66	52	NGC 4261
W′ cloud	186.00	7.20	<0.8	<2000	23	1019	416	28	202	NGC 4365
M cloud	183.00	13.40	<1.5	1500 <vel< 3500	32	2109	280	21	9	NGC 4168
LVC cloud	184.00	13.40	<1.5	vel< 400	17	85	208	21	57	NGC 4216
Field	187.20	11.20	>6.1	<3500	17	1537	635	138	0.05^d	–

Notes. Galaxies in the overlapping regions that satisfy the membership criteria of two different structures are assumed to be members of the smallest structure.

^(a)

Mean distance of each single substructure taken from Gavazzi et al. (1999).

^(b)

Mean density assuming a spherical geometry of the substructure.

^(c)

Radius corresponding to half of the virial radius from McLaughlin (1999) and Ferrarese et al. (2012).

^(d)

The mean density at the periphery of the cluster is probably underestimated because there the GALEX observation are, on average, less deep than in the inner ~100 deg².

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