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 9:

Best mass model.
Clump	X	Y	$\epsilon$	$\theta$	$\sigma_{0}$	$r_{\rm core}$	$r_{\rm cut}$
	( $\hbox{$^{\prime\prime}$ }$ )	( $\hbox{$^{\prime\prime}$ }$ )		(deg)	(km s^-1)	(kpc)	(kpc)
Cluster	-0.771414	2.256631	0.695267	31.146240	1117.322994	7.667450	[1500]
L^* elliptical galaxy	-	-	-	-	150.421411	[0]	3.880257

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 ( $r_{\rm cut}$ ). Values into brackets are not optimized. 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{$^{\prime\prime}$ }$ .

Source LaTeX | All tables | In the text

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