Table 3: TWA 5 best fit paramenters.
  PN MOS RGS
  Abundancesa, b ( $A_{\rm X}/A_{\rm X\odot}$)
C =Fe =Fe $\rm0.26^{+0.30}_{-0.08}$
N =Fe =Fe $\rm0.55^{+0.61}_{-0.18}$
O $\rm0.15^{+0.11}_{-0.07}$ $\rm0.28^{+0.14}_{-0.14}$ $\rm0.31^{+0.29}_{-0.07}$
Ne $\rm0.34^{+0.27}_{-0.16}$ $\rm0.93^{+0.37}_{-0.51}$ $\rm0.92^{+0.74}_{-0.26}$
Mg $\rm0.07^{+0.15}_{-0.06}$ $\rm0.14^{+0.20}_{-0.13}$ $\rm0.51^{+0.16}_{-0.38}$
Si $\rm0.21^{+0.20}_{-0.16}$ $\rm0.19^{+0.22}_{-0.15}$ =Fe
S $\rm0.32^{+0.36}_{-0.31}$ $\rm0.36^{+0.38}_{-0.32}$ =Fe
Fe $\rm0.05^{+0.04}_{-0.02}$ $\rm0.09^{+0.06}_{-0.05}$ 0.1
Ni $\rm 1.08^{+1.17}_{-0.98}$ $\rm0.06^{+1.31}_{-0.06}$ =${\rm Fe}$
  Temperatureb (K)
$\log T_{1}$ $\rm 6.17^{+0.56}_{-0.20}$ $\rm 6.56^{+0.14}_{-0.14}$  
$\log T_{2}$ $\rm 6.70^{+0.17}_{-0.05}$ $\rm 6.90^{+0.19}_{-0.25}$  
$\log T_{3}$ $\rm 7.27^{+0.09}_{-0.06}$ $\rm 7.27^{+0.33}_{-0.09}$  
  Emission measureb $N_{\rm e}N_{\rm H}V\;({\rm cm^{-3}})$
$\log EM_{1}$ $\rm 52.71^{+0.79}_{-0.63}$ $\rm 52.45^{+0.60}_{-0.37}$  
$\log EM_{2}$ $\rm 53.21^{+0.26}_{-0.31}$ $\rm 52.76^{+0.34}_{-0.70}$  
$\log EM_{3}$ $\rm 52.72^{+0.10}_{-0.26}$ $\rm 52.64^{+0.15}_{-0.30}$  
  Column densityb ( ${\rm 10^{20}~ cm^{-2}}$)
$N_{\rm H}$ $\rm 2.8^{+3.9}_{-2.5}$ $\le$3.3 =1
  Best fit statistics
$\chi^{2}_{\rm red}$ 0.89 0.99  
d.o.f. 404 285  
$P(\chi^{2}>\chi^{2}_{\rm obs})$ 94% 54%  
a Solar photospheric abundances are from Anders & Grevesse (1989).
b All the uncertainties correspond to the 68% confidence level.

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