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Table 2

Fit results on line emission.

Expected Line energy (keV) Δ   χ2 Intensitya EW (eV)
Observation (keV) Mar. 2006 Sep. 2010 Mar. 2006 Sep. 2010 Mar. 2006 Sep. 2010 Mar. 2006 Sep. 2010
(d.o.f. = 205) (d.o.f. = 206)

O Heα 0.568 0.568(fixed) 0.568(fixed) 0.09(fixed) 0.09(fixed) 3.2(2) 1.3(2)
O Lyα 0.653 0.661(8) 0.66(2) 59 5.4b 3.0 4(4) 13(4) 7(3)
Ne Heαc 0.914 0.930(8) 0.929(8) 105 119 1.3(3) 7(1) 8(1) 14(1)
Ne Lyα 1.021 1.025(3) 1.031(2) 878 1699 3.3(2) 24(1) 22.6(2) 50.9(8)
Ne Heβc 1.084 1.084(fixed) 1.13(3) 39 0.2(fixed) 3(1) 3.7(2) 6(2)
Ne Lyβ 1.210 1.210(fixed) 1.25(1) 6 96 0.2(fixed) 2(1) 1.8(2) 9(4)
Mg Heα 1.34 1.32(2) 1.38(2) 36 31 0.4(1) 1.8 4(1) 5(1)
Ne Recombod 1.362 1.48(2) 1.52(2) 137 154 0.9(2) 5(1) 11.1(3) 15(5)
Fe K-fluor. linee 6.4 6.5(2) 6.78(7) 59 30 0.8 1.3(5) 42.2(3) 33(1)

Notes. The widths of the low-energy lines were fixed to the ASCA values (10 eV for all but the 1.362 keV line with 57 eV).

(a)

photons 10-4 cm-2 s-1.

(b)

We note that, for the 2010 observation, the Δ   χ2 for this line is not well computed due to the spectral model not being able to adequately fit this line (see Fig. 2, right panel).

(c)

The abundances of the lines at 0.914 and 1.084 keV can also be consistent with a blend of several L-shell iron line emission (see Angelini et al. 1995).

(d)

The Mg Hα line emission occurs at 1.471 keV (here not resolved, and thus not detected, by Suzaku), and therefore this Mg line may be contributing to this feature.

(e)

For the iron line the widths were fitted (0.5(3) keV and 0.14(7) keV, respectively).

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