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Table 1

Detected emission lines in the XMM-Newton RGS spectra of NGC 424.

Line Id. λ T E T Energy kT Fluxes
(a) (b) (c) (d)

C vi Kα 33.736 0.367 1.10 0.5 0.6
29.534 0.420 (f) 0.9 0.04 0.86
N vi Kα 29.082 0.426 (i) 0.426  <0.8 0.2 0.03 0.17
28.787 0.431 (r)  <1.2 0.3 0.05 0.25
C vi RRC 25.303 0.490 0.8 0.35 0.45
N vii Kα 24.781 0.500 0.3 0.21 0.09
22.101 0.561 (f) 3.5 0.4 3.1
O vii Kα 21.807 0.569 (i) 0.569  <0.8 0.9 0.1 0.8
21.602 0.574 (r) 0.81 0.15 0.66
O viii Kα 18.968 0.654 1.06 0.93 0.13
O vii Kβ 18.627 0.666 0.04 0.02 0.02
Fe xvii M2 17.097 0.725 0.003 0.003
Fe xvii 3G 17.050 0.727 0.02 0.02
O vii RRC 16.769 0.739 0.6 0.14 0.47
Fe xvii 3F 16.777 0.739 0.01 0.01
O viii Kβ 16.005 0.775  <0.3 0.04 0.03 0.01
O viii RRC 14.228 0.871 * 0.59 0.53 0.07
13.698 0.905 (f) 0.40 0.22 0.18
Ne ix Kα 13.551 0.915 (i) 0.916 0.13 0.07 0.06
13.447 0.922 (r) 0.17 0.1 0.07
Ne x Kα 12.133 1.022 0.13 0.13
Fe xvii 4C 12.119 1.023
Fe xviii L 10.524 1.178 0.006 0.006
Fe xvii 7D 10.500 1.181
Mg xi (f) 9.168 1.352 0.05 0.04 0.01

Notes. Energies are in keV units, wavelengths in Å, fluxes in 10-5 ph cm s, kT in eV. Theoretical energies and wavelengths are from CHIANTI (Dere et al. 1997, 2009). The labelling for Fe xvii lines follows that of Brown et al. (1998). (a) Calculated fluxes with the phenomenological analysis; (b) Line fluxes extrapolated from the RGS1+RGS2 best fit with CLOUDY; (c) Line fluxes arising from the component with higher photoionisation parameter (, ); (d) Line fluxes arising from the second photoionised phase (, ).

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