Table 1
γ-ray SNRs.
| SNR | Type | Age (kyr) | d (kpc) | Refs. |
|
|
||||
| Cas A | II | 0.33 | 3.4 |
1 |
| Tycho | Ia | 0.44 | 1.5–4.0 | 2 |
| RX J1713.7-3946 | II(?) | 1.6 | 0.9–1.7 | 3, 4 |
| RX J0852.0-4622 | II(?) | 1.7–4.3 | 0.75 | 5, 6 |
| CTB 37A | II | 2 ± 0.5 | 6–9.5 | 7, 8 |
| W49B | II | 1–4 | 8–11 | 9 |
| IC443 | Ib(?) | 3–30a | ~1.5 | 10 |
| W51C | II | 10–30 | 7 ± 1.5 | 11 |
| G359.1-0.5 | >10 | 7.6 | 12, 13 | |
| W44 | II | 15–20 | ~3 | 14, 15 |
| G8.7-0.1 | IIb | 15–28 | 4.8–6.0 | 16, 12 |
| W28 | II | 35–45 | 1.9 ± 0.3 | 17,18 |
| W41 | IIc | 60–200 | 3.9–4.5 | 19, 20 |
Notes. Except for W44, all SNRs are detected at TeV energies.
Troja et al. (2008) argue from XMM-Newton X-ray observations that the age is <10 kyr.
This shell-type SNR is probably a core-collapse SNR given its proximity to molecular clouds. The TeV radiation might also be powered by a pulsar wind, in which case this analysis would not apply; see Mukherjee et al. (2009).
Possibly associated with PSR 1800-21; see Kassim & Weiler (1990). TeV emission could also be powered by the pulsar wind.
Reference. 1. Abdo et al. (2010a); 2. Giordano et al. (2012); 3. Abdo et al. (2011); 4. Fesen et al. (2012); 5. Tanaka et al. (2011); 6. Aharonian et al. (2007); 7. Brandt (2013); 8. Tian et al. (2012); 9. Abdo et al. (2010b); 10. Abdo et al. (2010e); see also Caprioli (2011); 11. Abdo et al. (2009); 12. Aharonian et al. (2006); 13. Hui et al. (2011); 14. Abdo et al. (2010c); 15. Wolszczan et al. (1991); 16. Ajello et al. (2012); 17. Abdo et al. (2010d); 18. Velázquez et al. (2002); 19. Leahy & Tian (2008); 20. Tian et al. (2007).
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