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Table 2:

Energy and intensity of the lines detected in the combined RGS spectrum of NGC 1365.
Energy (eV) Intensity (I) I/I[ O VII(f)] I/I[ O VII(f)] Transition $(E_{{\rm lab}})$a Contribution by
(eV) (10-5 s-1 cm-2) NGC 1365 NGC 1068 (eV) thermal plasma (%)b
$367.4\pm0.2$ $1.4\pm^{0.4}_{0.5}$ $0.60\pm^{0.18}_{0.19}$ $1.16\pm^{0.05}_{0.19}$ C VI Ly-$\alpha $ (367.56) $100 \pm 50$
$430.72\pm^{0.02}_{0.09}$ $0.7\pm0.4$ $0.30\pm^{0.15}_{0.17}$ $0.35\pm^{0.02}_{0.17}$ N VI He-$\alpha $ (r) (430.75) $90 \pm 50$
(r) - 4.4 <0.6 <0.25 $0.08 \pm 0.02$ N VI He-$\alpha $ (i) (426.37) $\le$100
(r) - 10.8 $1.8\pm0.3$ $0.73\pm^{0.13}_{0.14}$ $0.89\pm^{0.03}_{0.14}$ N VI He-$\alpha $ (f) (419.86) $26 \pm 7$
$435.26\pm^{0.16}_{0.30}$ $0.6\pm^{0.2}_{0.3}$ $0.27\pm^{0.10}_{0.11}$ <0.06 C VI Ly-$\beta$ (435.91) $70 \pm 40$
$459.0\pm^{0.5}_{0.3}$ $0.40\pm^{0.17}_{0.18}$ $0.16\pm 0.07$ $0.11\pm^{0.01}_{0.07}$ C VI Ly-$\gamma$ (459.42) $90 \pm 50$
$499.96\pm^{0.04}_{0.22}$ $1.2\pm0.2$ $0.52\pm^{0.09}_{0.10}$ $0.41\pm^{0.02}_{0.10}$ N VII Ly-$\alpha $ (500.31) $100 \pm 30$
$573.99\pm^{0.05}_{0.05}$ $1.0 \pm 0.2$ $0.41\pm^{0.09}_{0.10}$ $0.38\pm^{0.03}_{0.10}$ O VII He-$\alpha $ (r) (574.02) $110 \pm 30$
(r) - 5.3 $0.6\pm0.2$ $0.23\pm^{0.09}_{0.10}$ $0.12\pm^{0.02}_{0.10}$ O VII He-$\alpha $ (i) (569.07) $34 \pm 12$
(r) - 13.0 $2.4\pm0.3$ $1.00\pm0.13$ $1.00\pm^{0.04}_{0.13}$ O VII He-$\alpha $ (f) (561.06) $40 \pm 8$
$653.4\pm0.6$ $2.5\pm0.2$ $1.03\pm^{0.08}_{0.09}$ $0.52\pm^{0.02}_{0.09}$ O VII Ly-$\alpha $ (653.70) $110 \pm 20$
$726.00\pm^{0.35}_{0.13}$ $1.89\pm^{0.18}_{0.19}$ $0.78\pm0.08$ $0.14\pm^{0.01}_{0.08}$ Fe XVII 3s2p (726.29) $86 \pm 11$
$738.1\pm^{0.3}_{0.9}$ $0.47 \pm^{0.15}_{0.13}$ $0.20 \pm 0.06$ $0.104 \pm 0.014$ O VII RRCc (739.11) $60 \pm 20$
$773.54\pm^{0.02}_{0.34}$ $0.75\pm^{0.13}_{0.13}$ $0.31\pm^{0.05}_{0.06}$ $0.09\pm^{0.01}_{0.06}$ O VIII Ly-$\beta$ (774.71)d $83 \pm 16$
$824.57\pm0.07$ $1.49\pm^{0.16}_{0.17}$ $0.62\pm 0.07$ $0.12\pm^{0.01}_{0.07}$ Fe XVIII 3d2p (824.72) $98 \pm 14$
$872.0\pm0.7$ $0.42\pm^{0.12}_{0.13}$ $0.18\pm 0.05$ $0.06\pm^{0.01}_{0.05}$ OVIII RRC (871.52)e $60 \pm^{70}_{40}$
$921.63\pm^{0.25}_{0.12}$ $0.42\pm^{0.17}_{0.18}$ $0.18\pm^{0.07}_{0.08}$ $0.10\pm^{0.01}_{0.08}$ Ne IX He-$\alpha $ (r) (922.14) $130 \pm 60$
(r) - 7.2 <0.33 <0.14 <0.05 Ne IX He-$\alpha $ (i) (915.13) <100
(r) - 13.0 $0.40\pm^{0.11}_{0.12}$ $0.17\pm 0.05$ $0.10\pm^{0.01}_{0.05}$ Ne IXHe-$\alpha $ (f) (905.11) $90 \pm 30$
$1021.13\pm^{1.20}_{0.10}$ $1.0 \pm 0.2$ $0.43\pm^{0.09}_{0.10}$ $0.11\pm^{0.01}_{0.10}$ Ne X Ly-$\alpha $ (1021.92) $120 \pm 30$
$1353.2\pm^{2.1}_{1.4}$ $0.57\pm^{0.15}_{0.16}$ $0.24\pm^{0.06}_{0.07}$ <0.05 Mg XI He-$\alpha $ (r) (1352.24) $110 \pm 15$
(r) - 8.0 <0.6 <0.25 <0.04 Mg XI He-$\alpha $ (i) (1343.44) $\le$100
(r) - 21.0 $0.33\pm^{0.15}_{0.16}$ $0.14\pm^{0.06}_{0.07}$ <0.04 Mg XI He-$\alpha $ (f) (1331.90) $90 \pm 50$
$1473.0\pm^{3.7}_{1.7}$ $0.50\pm^{0.18}_{0.19}$ $0.21\pm^{0.07}_{0.08}$ <0.04 Mg XII Ly-$\alpha $ (1472.51) $90 \pm 30$
$1896.9\pm0.7$ <47 <33 <0.33 Si XIII He-$\alpha $ (r) (1867.47) $\le$100
(r) - 13.8 <2.4 <1.0 <0.05 Si XIII He-$\alpha $ (i) (1853.61) $\le$100
(r) - 27.8 $1.9\pm^{1.1}_{0.7}$ $0.8\pm^{0.5}_{0.3}$ <0.04 Si XIII He-$\alpha $ (f) (1839.76) $90 \pm 30$
$1892.7\pm0.8$f $1.1\pm0.4$ $0.46\pm 0.18$ <0.05   ...
a Most likely identification. The laboratory energy is shown in brackets. b Contribution to the total intensity due to the best-fit model in Table 3. Values higher than 100% mean that the model over-predicts the data at that energy. c Fit with a single Gaussian ( $\sigma \le 8$ eV). Possible blending with Fe XVII 2$^{\rm s}$2$^{\rm p}$ (738.98 eV): see Sect. 4.1 for the results of a fit with two Gaussians. d Possible blending with Fe XVIII 3$^{\rm s}$2$^{\rm p}$ (773.02 eV). e Fit with a single Gaussian ( $\sigma \le 3$ eV). Possible blending with Fe XVIII 2$^{\rm s}$2$^{\rm p}$ (872.75 eV). See Sect. 4.1 for the results of a fir with two Gaussians. f Unidentified.

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