Table 1
Parameters used to derive the filament profiles and spectra.
| SNR | Age | Distance | r s | v s | w | B min | |||||
|
|
|
|
|
||||||||
| [yr] | [kpc] | Reference | [arcmin]a | [pc]b | [km s-1] | Reference | [arcsec] | [pc]b | Reference | [μG]c | |
|
|
|||||||||||
| SN 1006d | 1000 | 2.2 | 1 | 15 | 10 | 4900 | 2 | 20 | 0.2 | 3 | 10 |
| (2900) | |||||||||||
| Cas A | 330e | 3.4 | 4 | 2.5 | 2.5 | 5200 | 5 | 1.5 | 0.03 | 6, 7 | 10 |
| Tycho | 440 | 2.5 | 8 | 4 | 3 | 5000 | 9 | 5 | 0.06 | 6 | 10 |
| Keplerf | 410 | 4.8 | 10 | 1.5 | 2 | 5040 | 11 | 3.5 | 0.08 | 6 | 10 |
| (6.4) | (3) | (6720) | (0.11) | ||||||||
Notes. s = 2 and Bohm diffusion are assumed in all SNRs.
Taken from Green (2009).
The shock velocity in the northwestern limb (value in brackets) is used, as well as in the northeastern limb, where strong electron acceleration appears to occur.
The supernova explosion may have been observed in 1680 (Ashworth 1980). Otherwise, the detection of radioactive 44Ti (Hartmann et al. 1997) and the analysis of the dynamics of this remnant (Fesen et al. 2006) also suggest an explosion date in the late 17th century.
Distance to this remnant is uncertain. Calculation is performed for the lower and upper limit (values in brackets) to the distance.
References. (1) Winkler et al. (2003); (2) Ghavamian et al. (2002) + Katsuda et al. (2009); (3) Bamba et al. (2003); (4) Reed et al. (1995); (5) Vink et al. (1998); (6) Bamba et al. (2005); (7) Araya et al. (2010); (8) Tian & Leahy (2011); (9) Hughes (2000) + distance; (10) Reynoso & Goss (1999); (11) Vink (2008) + distance.
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