Table E.3
Spectral results, abundances, fluxes, and Fe K line properties of SNR 1987A.
| Epoch | Age | low-kT component | 1.15 keV component | high-kT component | ionisation age | |||
|
|
||||||||
| kT | EM | EM | kT | EM | ||||
| (days) | keV | (1058 cm-3) | (1058 cm-3) | (keV) | (1058 cm-3) | (1011 s cm-3) | ||
|
|
||||||||
| 2007 Jan. | 7267 | 0.35 ±0.01 | 35.69 |
7.31 |
13.89 |
0.55 |
4.42 |
|
| 2008 Jan. | 7626 | 0.36 |
42.63 |
7.80 |
5.82 |
1.06 |
4.60 |
|
| 2009 Jan. | 8013 | 0.37 ±0.01 | 49.66 |
11.89 |
10.86 |
0.90 |
5.27 |
|
| 2009 Dec. | 8328 | 0.40 ±0.01 | 47.29 |
12.97 |
5.98 |
1.40 |
4.77 |
|
| 2010 Dec. | 8693 | 0.42 |
48.13 |
13.40 |
3.80 |
2.43 |
4.98 |
|
| 2011 Dec. | 9048 | 0.44 |
45.72 |
15.92 |
5.66 |
2.20 |
4.84 |
|
| 2012 Dec. | 9423 | 0.44 |
44.56 |
19.90 |
7.66 |
1.95 |
5.76 |
|
|
|
||||||||
| N | O | Ne | Mg | Si | S | Fe | ||
|
|
||||||||
| 1.35 ±0.06 | 0.08 ±0.01 | 0.29 ±0.01 | 0.26 ±0.01 | 0.51± 0.01 | 0.48 ±0.02 | 0.24 ±0.01 | ||
|
|
||||||||
| Epoch | Age | Flux (0.5–2 keV) | Flux (3–10 keV) | ΔFX | E line | σ-width | Flux | EW |
| (days) |  erg s-1 cm |
(%) | (keV) | (eV) | (10-6 ph cm-2 s-1) | (eV) | ||
|
|
||||||||
| 2007 Jan. | 7267 | 33.51 |
4.09 |
– | – | – | – | – |
| 2008 Jan. | 7626 | 43.34 |
5.22 |
29.8 | 6.58 |
46 (<146) | 1.07 |
174 |
| 2009 Jan. | 8013 | 52.77 |
6.31 |
20.5 | 6.55 |
125 (<433) | 0.94 |
169 |
| 2009 Dec. | 8328 | 59.04 |
7.42 |
13.8 | 6.63 |
229 (<424) | 2.64 |
432 |
| 2010 Dec. | 8693 | 65.90 |
8.16 |
11.6 | 6.61 |
105 (<227) | 2.51 |
344 |
| 2011 Dec. | 9048 | 70.69 |
11.31 |
7.5 | 6.61 |
83 (<178) | 2.08 |
238 |
| 2012 Dec. | 9423 | 74.60 |
11.65 |
5.4 | 6.78 |
84 (<155) | 2.11 |
230 |
Notes. Top panel: best-fit values and 90% C. L. uncertainties for the parameters of the three-components spectral model described in Sect. 5.3, in spectra obtained from 2007 to 2012. Middle panel: best-fit abundances relative to the solar values as listed in Wilms et al. (2000). Bottom panel: fluxes and Fe K line properties. Columns (3) and (4) list the soft and hard X-ray fluxes with 3σ errors (99.73% C.L.). Column (5) gives the increase rate of the flux (in %) since previous measurement, normalised to one year. Columns (6) to (9) give the central energy, σ-width, total photon flux and equivalent width (EW) of the Gaussian used to characterise the Fe K feature in the spectra of SNR 1987A (with 90% C. L. uncertainties).
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