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Table 2
Fe K line properties of LMC SNRs.
| MCSNR | Alt. name | type | Energy centroid (eV) | Line luminosity (1042 ph s-1) | ||
| XMM-Newton | Suzaku | XMM-Newton | Suzaku | |||
|
|
||||||
| J0509−6731 | B0509−675 | Ia | 6432 |
6425 |
0.87 ± 0.21 | 0.96 ± 0.12 |
| J0505−6753 | DEM L71 | Ia | 6494 ± 58 | – | 0.26 |
– |
| J0509−6844 | N103B | Ia | 6514 |
6545 ± 6 | 5.10 ± 0.87 | 6.43 ± 0.30 |
| J0519−6902 | B0519−690 | Ia | 6543 |
6498 |
1.71 ± 0.45 | 2.78 ± 0.15 |
| J0526−6605 | N49 | CC | – | 6628 |
<4.75a | 0.54 ± 0.12 |
| J0535−6916 | SNR 1987Ab | CC | 6635 ± 70 | 6646 |
0.64 ± 0.18 | 0.57 ± 0.24 |
| J0535−6602 | N63A | CC | 6683 |
6647 |
2.36 |
2.57 ± 0.36 |
| J0525−6938 | N132D | CC | 6685 |
6656 ± 9 | 4.58 ± 0.58 | 5.47 ± 0.51 |
Notes. Suzaku results are from Yamaguchi et al. (2014).
(b)
The quoted numbers are average values over the last six epochs, and the uncertainties are the rms scatter. Note that we found the energy centroid to evolve rapidly at recent epochs (see Sect. 5.3).
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