Table 1: Surveyed clusters.
Cluster Cluster centre ${r}_{\rm A}$ ${r}_{\rm vir}$ $z_{o}^{\dagger}$ $\sigma_{v}^{\dagger}$ $n^{\dagger}$
  RA (1950) Dec. l b (arcmin) (Mpc) ( ${r}_{\rm A}$)   (km ${\rm s}^{-1}$)  
Abell 262 1$^{\rm h}$ 49 $.\!\!^{\rm m}$9 35$^{\circ}$ 54$^{\prime}$ 136 $.\!\!^\circ$59 -25 $.\!\!^\circ$09 105 1.83 0.86 0.0167 537 38
Abell 347 2 22.7 41 39 141.17 -17.63 91 1.87 0.87 0.0192 550 14
Abell 400 2 55.0 5 50 170.25 -44.93 72 1.32 0.62 0.0227 392 10
Abell 426 3 15.3 41 20 150.39 -13.38 96 3.67 1.72 0.0177 1076 55
Abell 569 7 5.4 48 42 168.58 22.81 88 1.42 0.66 0.0198 417 26
Abell 779 9 16.8 33 59 191.07 44.41 75 0.98 0.46 0.0232 290 11
Abell 1367 11 41.9 20 7 234.81 73.03 80 2.58 1.21 0.0216 762 62
Abell 1656 12 57.4 28 15 58.09 87.96 74 3.01 1.41 0.0232 890 131
$^{\dagger}$ E-S0/a galaxies only. Cluster centres are taken from Abell et al. (1989). The Abell radius (Abell 1958), ${r}_{\rm A}$, corresponds to $\sim$ 1.5  h-1 Mpc. Values for the virial radius, ${r}_{\rm vir}$, are from Moss (2006), where h=0.75 is assumed. Cluster mean redshifts, z0, and velocity dispersions, $\sigma_{\rm v}$, are based on n redshifts of galaxies of types E-S0/a only. These objects are more likely to be in dynamic equilibrium with the cluster potential and follow a Gaussian distribution, as expected for virially relaxed galaxies within the cluster (see Moss 2006). The mean redshift has been corrected to the centroid of the Local Group following RC2 (de Vaucouleurs et al. 1976).


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