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Table 3

Additional parameters defining the “default” cluster models.

Cluster z d ⟨⟨β⟩⟩ σ(⟨ β⟩) f1(θ) α c,J2000 δ c,J2000 r min r max θ min θ max Δθ
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12)
CL 0030+2618 0.50 0.348† 0.024† 0.152† X +26°18′16″ 0.2   Mpc 5.0   Mpc 23″
CL 0159+0030 0.39 0.447 0.023 0.087 X +00°30′09″ 0.2   Mpc 5.0   Mpc 79″§
CL 0230+1836 0.80 0.168 0.020 0.321 X +18°36′22″ 0.2   Mpc 5.0   Mpc 20″
CL 0809+2811 0.40 0.437 0.023 0.105 X +28°11′58″ 0.2   Mpc 5.0   Mpc 178″§
CL 1357+6232 0.53 0.324 0.024 0.198 – +62°32′42″ 0.2   Mpc 5.0   Mpc 50″
CL 1416+4446 0.40 0.437 0.023 0.136 – +44°46′38″ 0.2   Mpc 5.0   Mpc 19″
CL 1641+4001 0.46 0.381 0.024 0.127 – +40°01′27″ 0.2   Mpc 5.0   Mpc 95″
CL 1701+6414 0.45 0.381 0.024 0.134 – +64°14′08″ 0.2   Mpc 5.0   Mpc 66″

Notes. Columns (1) to (5) tabulate the cluster redshift zd, the average ⟨⟨β⟩⟩ and dispersion σ(⟨ β⟩) of the distance ratio estimated from the CFHTLS Deep fields, the estimated fraction of residual foreground galaxies in the lensing catalogue, based on the same Ilbert et al. (2006) photo-z catalogue, and whether or not a dilution correction f1(θ) has been applied. Columns (6) and (7) present the celestial coordinates of the assumed cluster centre, with respect to which the fitting range rmin ≤ θ ≤ rmax in Cols. (8) and (9) is defined. Columns (10) and (11) repeat the fitting range in terms of angular separation. Finally, we give the separation between ROSAT and lensing centres in Col. (12).

(†)

We use an improved fit for the redshift distribution and corrected for CL 0030+2618 with respect to Paper I.

(§)

Lensing centre is within a large masked area, which probably diminished the accuracy.

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