Table 1: Best fit NFW model parameters and their 68% CL uncertainty (marginalized over all the other parameters). (SL) corresponds to a model in which weak lensing constraints are ignored whereas (SL+WL) takes both strong and weak lensing constraints into account. (1) Refers to the CHANDRA X-rays values of Allen et al. (2001). The apparent disagreement between their estimates and ours is discussed in the text.
(SL) (SL+WL) (1) Unit

$\kappa_{\rm s}$ $0.67\pm0.05$ $0.66\pm0.03$ $0.30\pm0.15$

$r_{\rm s}$ $\rm 158^{+15}_{-13}$ $\rm 162^{+11}_{-9}$ $160\pm30$ $~h_{\rm 70}^{-1}~{\rm kpc}$

$r_{\rm 200}$ $1.88\pm{0.05}$ $1.89\pm{0.04}$ $\rm 1.39^{+0.49}_{-0.38}$ $~h_{\rm 70}^{-1}~{\rm Mpc}$

$M_{\rm 200}$ $\rm 7.56^{+0.63}_{-0.54}$ $\rm 7.72^{+0.47}_{-0.42}$ - $10^{14}~h_{\rm 70}^{-1}~M_{\odot}$

c $\rm 11.92^{+0.77}_{-0.74}$ $11.73\pm0.55$ $\rm 8.7^{+1.2}_{-0.9}$

q $0.774\pm0.010$ $0.777\pm0.007$ -

$\psi_0$ $5.86\pm0.14$ $5.88\pm0.13$ - deg

$\Upsilon_V$ $2.40\pm0.45$ $2.48\pm0.39$ - $~h_{\rm 70}~(M/L)_\odot$

**Table 1:** Best fit NFW model parameters and their 68% CL uncertainty (marginalized over all the other parameters). (SL) corresponds to a model in which weak lensing constraints are ignored whereas (SL+WL) takes both strong and weak lensing constraints into account. (1) Refers to the CHANDRA X-rays values of Allen et al. (2001). The apparent disagreement between their estimates and ours is discussed in the text.
	(SL)	(SL+WL)	(1)	Unit
$\kappa_{\rm s}$	$0.67\pm0.05$	$0.66\pm0.03$	$0.30\pm0.15$
$r_{\rm s}$	$\rm 158^{+15}_{-13}$	$\rm 162^{+11}_{-9}$	$160\pm30$	$~h_{\rm 70}^{-1}~{\rm kpc}$
$r_{\rm 200}$	$1.88\pm{0.05}$	$1.89\pm{0.04}$	$\rm 1.39^{+0.49}_{-0.38}$	$~h_{\rm 70}^{-1}~{\rm Mpc}$
$M_{\rm 200}$	$\rm 7.56^{+0.63}_{-0.54}$	$\rm 7.72^{+0.47}_{-0.42}$	-	$10^{14}~h_{\rm 70}^{-1}~M_{\odot}$
c	$\rm 11.92^{+0.77}_{-0.74}$	$11.73\pm0.55$	$\rm 8.7^{+1.2}_{-0.9}$
q	$0.774\pm0.010$	$0.777\pm0.007$	-
$\psi_0$	$5.86\pm0.14$	$5.88\pm0.13$	-	deg
$\Upsilon_V$	$2.40\pm0.45$	$2.48\pm0.39$	-	$~h_{\rm 70}~(M/L)_\odot$

Source LaTeX | All tables | In the text

	1 Introduction
	2 Lens modelling
	3 Dynamics of stars in the BCG
	4 Discrepancies between mass estimates
	5 Discrepancies: an expected general trend
	6 Discussion and conclusion
	References
	Online Material
	Appendix A: LOSVD of stars in the BCG
	Appendix B: Further evidence for triaxiality