Radio counterpart of the lensed submm emission in the cluster MS0451.6-0305: new evidence for the merger scenario

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Volume 509 (January 2010)

A&A, 509 (2010) A54

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Table 8:

Most likely mass model parameters.
Clump	X	Y	$\epsilon$	$\theta$	$\sigma_{0}$	$r_{\rm core}$	$r_{\rm cut}$
	( $\hbox{$^{\prime\prime}$ }$ )	( $\hbox{$^{\prime\prime}$ }$ )		(deg)		(kpc)	(kpc)
Cluster	$\rm -0.5^{+4.1}_{-1.2}$	2.7 $\pm$ 1.5	$\rm0.69^{+0.0}_{-0.1}$	31.3 $\pm$ 1.1	1144.8 $\pm$ 36	60.8 $\pm$ 24	[1500]
L^* elliptical galaxy	-	-	-	-	135.1 $\pm$ 43.9	[0]	$\rm 30.1^{+43.6}_{-4.9}$

The columns show: position respect to the brightest cluster galaxy (X,Y), ellipticity of the mass distribution ( $\epsilon$ , expressed as a²-b²/a²+b², were a and b are the semi-major and semi minor axes of the ellipse that describes the light distribution of the clump), position angle ( $\theta$ ), velocity dispersion ( $\sigma_{0}$ ), core radius ( $r_{\rm core}$ ) and scale radius ( $r_{\rm cut}$ ). Error bars correspond to $1\sigma$ confidence level as inferred from the MCMC optimization. Values into brackets are not optimized. When the posterior distribution is not Gaussian, we report the mode and asymmetric error bars. The coordinates of the brightest cluster galaxy are $\rm RA=4^{h} 54^{m} 10.87^{s}$ , $\rm Dec=-3^{\circ} 0\hbox{$^\prime$ } 54.00\hbox{$^{\prime\prime}$ }$ .

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