Table 2: Fit results for spatially-resolved RGS spectra. We model the plasma with two thermal components. Abundances are given with respect to the proto-solar values by Lodders (2003). The emission measures are given in 1064 cm-3.
Par. -0.5 / 0.5 $\hbox {$^\prime $ }$ 0.5 / 1.5 $\hbox {$^\prime $ }$ 1.5 / 2.5 $\hbox {$^\prime $ }$ 2.5 / 3.5 $\hbox {$^\prime $ }$
Y1 $0.82\pm 0.04$ $0.23\pm0.03$ $0.16\pm0.02$ $0.18\pm0.02$
Y2 $10.83\pm0.17$ $8.38\pm0.08$ $6.18\pm0.10$ $4.79\pm0.07$
kT1 $0.79\pm 0.01$ $0.81\pm0.03$ $0.69\pm0.02$ $0.69\pm0.03$
kT2 $1.69\pm 0.03$ $1.87\pm0.04$ $1.88\pm0.05$ $1.66\pm0.05$
C $0.63\pm 0.16$ $0.44\pm0.13$ $0.30\pm0.16$ <0.18
N $1.64\pm 0.24$ $0.62\pm0.18$ $0.67\pm0.22$ <0.23
O $0.58\pm 0.03$ $0.48\pm0.02$ $0.52\pm0.03$ $0.45\pm0.03$
Ne $1.41\pm 0.12$ $1.17\pm0.13$ $0.89\pm0.17$ <0.23
Fe $0.95\pm 0.03$ $0.78\pm0.03$ $0.65\pm0.03$ $0.50\pm0.03$
Scale s $2.14\pm 0.10$ $1.10\pm0.05$ $1.18\pm0.09$ $1.42\pm0.08$
$\chi^{2}$ / $\nu$ 1308/918 1265/918 1199/918 1187/918


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