Table 4: Single halo models. The Einstein radius is the same in the best models for strong lensing : $R_{\rm E} \simeq 50 ~h^{-1}~{\rm kpc}$ . For our two strong lensing models, the total mass inside this radius is $M(r<R_{\rm E}) = (2.8\pm0.1)\times 10^{13}~h^{-1}~{M}_\odot$ . Errors due to uncertainties in arcs redshift are omitted. Also reported previous works results for comparison. Me93 refers to Mellier et al. (1993), Ha97 to Hammer et al. (1997), Mi95 to Miralda-Escudé (1995) EF99 to Ettori & Fabian (1999) and Al02 to Allen et al. (2002). When known, the authors' values are recomputed in our adopted cosmology and with the 1.6 sources redshifts. For both papers, the center of potential location is assumed to match the center of cD or is not reported. Me93 core radii have been scaled in order to take into account the departs between their profile and an exact softened isothermal sphere. As well, Ha97 find a slope $\beta \approx 0.85$ instead we have only considered models with $\beta = 1$ (see Eq. (2)). Al02 uses a NFW profile and only gives the scale radius value but we report on the same line our own measured values for ellipticity and position angle from Chandra X-ray brightness. The third column $r_{\rm c} \backslash r_{\rm s}$ corresponds either to the scale radius either to the core radius. Here, we convert all the position angles in a common definition, which is clockwise from North to East. The original paper do not report angles in the same frame but we made the correction except for Ha97 for which we do not know what is the reference. But in any case, the position angle is so constrained that these authors must have found a similar orientation as the other ones. Our definition is more valuable and self-consistent between Chandra, ROSAT, VLT and HST data. Models labels with a S refer to purely strong lensing modeling whereas a W stands for purely weak lensing fits. The last row (cD+DM) concerns the last family of profiles with a cD and dark matter halo components and which is simultaneously constrained by strong+weak lensing. In the first column, we report the permitted inner slope for generalized NFW profiles (see Sect. 3.4.3).
model $\sigma_{\rm v}$ $r_{\rm c} \backslash r_{\rm s}$ $\kappa_{\rm s}$ $r_{\rm 200}$ c $M_{\rm 200}$ $\epsilon$ PA $x_{\rm c}$ $y_{\rm c}$

(km s^-1) $(~h^{-1}~{\rm kpc})$ $(~h^{-1}~{\rm kpc})$ $(10^{14}~h^{-1}~{M}_\odot)$ deg arcsec arcsec

S-NFW - $\rm 90^{+35}_{-25}$ $\rm0.6^{+0.5}_{-0.3}$ $\rm 920^{+180}_{-80}$ $\rm 12.5^{+5}_{-6}$ $\sim$ 5.5 $\rm0.24^{+0.04}_{-0.07}$ $58\pm1$ $0.1\pm0.4$ $0.2\pm0.4$

W-NFW - $\rm 67^{+300}_{-24}$ $\rm0.74_{-0.5}^{+1.6}$ $\rm 890^{+160}_{-130}$ $\rm 12_{-8}^{+12}$ - - - -

S-isoT $\rm 1022^{+40}_{-30}$ $10.4\pm1.8$ - $\sim$ 1000 - $\sim$ 11. $0.25\pm0.05$ $59\pm1$ $0.2\pm0.4$ $0.2\pm0.4$

W-isoT $900 \pm 150$ <45 - - - - - - -

Me93 $\sim$ 1000 4.5-7 - - - - 0.15-0.33 51-66 - -

Mi95 $\sim$ 1200 $\sim$ 10 - - - - $\sim$ 0.22 $\sim$ 58 - -

Ha97 $\sim$ 1100 5-10 - - - - 0.18-0.23 $?47.5\pm5?$ - -

EF99 $\sim$ 930 $\sim$ 90 - $r_{500}\sim540$ - - - - - -

Al02 - 107-120 - - - - $\sim$ 0.20 $58\pm7$ - -

cD+DM $0.8<\alpha<1.1$ $\sim$ 85 $\sim$ 0.6 - - - $0.22\pm0.06$ $58\pm2$ 0! 0!

**Table 4:** Single halo models. The Einstein radius is the same in the best models for strong lensing : $R_{\rm E} \simeq 50 ~h^{-1}~{\rm kpc}$ . For our two strong lensing models, the total mass inside this radius is $M(r<R_{\rm E}) = (2.8\pm0.1)\times 10^{13}~h^{-1}~{M}_\odot$ . Errors due to uncertainties in arcs redshift are omitted. Also reported previous works results for comparison. Me93 refers to Mellier et al. (1993), Ha97 to Hammer et al. (1997), Mi95 to Miralda-Escudé (1995) EF99 to Ettori & Fabian (1999) and Al02 to Allen et al. (2002). When known, the authors' values are recomputed in our adopted cosmology and with the 1.6 sources redshifts. For both papers, the center of potential location is assumed to match the center of cD or is not reported. Me93 core radii have been scaled in order to take into account the departs between their profile and an exact softened isothermal sphere. As well, Ha97 find a slope $\beta \approx 0.85$ instead we have only considered models with $\beta = 1$ (see Eq. (2)). Al02 uses a NFW profile and only gives the scale radius value but we report on the same line our own measured values for ellipticity and position angle from Chandra X-ray brightness. The third column $r_{\rm c} \backslash r_{\rm s}$ corresponds either to the scale radius either to the core radius. Here, we convert all the position angles in a common definition, which is clockwise from North to East. The original paper do not report angles in the same frame but we made the correction except for Ha97 for which we do not know what is the reference. But in any case, the position angle is so constrained that these authors must have found a similar orientation as the other ones. Our definition is more valuable and self-consistent between Chandra, ROSAT, VLT and HST data. Models labels with a S refer to purely strong lensing modeling whereas a W stands for purely weak lensing fits. The last row (cD+DM) concerns the last family of profiles with a cD and dark matter halo components and which is simultaneously constrained by strong+weak lensing. In the first column, we report the permitted inner slope for generalized NFW profiles (see Sect. 3.4.3).
model	$\sigma_{\rm v}$	$r_{\rm c} \backslash r_{\rm s}$	$\kappa_{\rm s}$	$r_{\rm 200}$	c	$M_{\rm 200}$	$\epsilon$	PA	$x_{\rm c}$	$y_{\rm c}$
	(km s^-1)	$(~h^{-1}~{\rm kpc})$		$(~h^{-1}~{\rm kpc})$		$(10^{14}~h^{-1}~{M}_\odot)$		deg	arcsec	arcsec
S-NFW	-	$\rm 90^{+35}_{-25}$	$\rm0.6^{+0.5}_{-0.3}$	$\rm 920^{+180}_{-80}$	$\rm 12.5^{+5}_{-6}$	$\sim$ 5.5	$\rm0.24^{+0.04}_{-0.07}$	$58\pm1$	$0.1\pm0.4$	$0.2\pm0.4$
W-NFW	-	$\rm 67^{+300}_{-24}$	$\rm0.74_{-0.5}^{+1.6}$	$\rm 890^{+160}_{-130}$	$\rm 12_{-8}^{+12}$	-	-	-	-
S-isoT	$\rm 1022^{+40}_{-30}$	$10.4\pm1.8$	-	$\sim$ 1000	-	$\sim$ 11.	$0.25\pm0.05$	$59\pm1$	$0.2\pm0.4$	$0.2\pm0.4$
W-isoT	$900 \pm 150$	<45	-	-	-	-	-	-	-
Me93	$\sim$ 1000	4.5-7	-	-	-	-	0.15-0.33	51-66	-	-
Mi95	$\sim$ 1200	$\sim$ 10	-	-	-	-	$\sim$ 0.22	$\sim$ 58	-	-
Ha97	$\sim$ 1100	5-10	-	-	-	-	0.18-0.23	$?47.5\pm5?$	-	-
EF99	$\sim$ 930	$\sim$ 90	-	$r_{500}\sim540$	-	-	-	-	-	-
Al02	-	107-120	-	-	-	-	$\sim$ 0.20	$58\pm7$	-	-
cD+DM	$0.8<\alpha<1.1$	$\sim$ 85	$\sim$ 0.6	-	-	-	$0.22\pm0.06$	$58\pm2$	0!	0!

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