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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