Table 2
Summary of the physical properties of the known TeV shell morphology SNRs.
RX J1713 | RX J0852 | HESS J1731 | RCW 86 | SN 1006 | |
|
|||||
SN nature | CC | CC | CC | Type Ia | Type Ia |
Distance (kpc) | 0.9−1.3 | 0.6-0.9 | ≥3.2 | 2.3-2.8 | 2.0-2.4 |
Radius (pc) | 10 | 12 | 14 | 15 | 10 |
Age (kyr) | 1.6 | 2−4 | 2-6 | 1.8 | 1 |
Density (cm-3) | <0.02 | <0.03 | <0.01 | 0.1−0.5 | <0.05 |
ΓHE | 1.5 ± 0.1 | 1.85 ± 0.06 | ≤1.5* | 1.4 ± 0.2 | ≤1.7* |
ΓVHE | 2.32 ± 0.01 | 2.22 ± 0.06 | 2.32 ± 0.06 | 2.41 ± 0.16 | 2.30 ± 0.15 |
References | 12, 17, 11, 6, 1 | 13, 7, 18, 20, 9 | 21, 3, 22, 5 | 19, 10, 15, 8, 24 | 23, 2, 14, 4, 16 |
se | 2.15 | 2.15 | 2.02 | 2.30 | 2.10 |
Ecut (TeV) | 51 | 25 | 24 | 22 | 10 |
We (1048 erg) | 0.55 | 0.38 | 0.18 | 1.2 | 0.21 |
References | Yuan et al. (2011) | Tanaka et al. (2011) | Yang et al. (2014) | Yuan et al. (2014) | Acero et al. (2010) |
Notes. The corresponding nature of the SN explosion is noted as core collapse (CC) or thermonuclear (Type Ia). The ambient medium densities shown in this table have been derived from the presence/lack of X-ray thermal emission. The best-fit spectral indices at HE and VHE are reported under a power-law hypothesis in the corresponding energy band and the errors reported are statistical. In the second part of the table, the best-fit leptonic model for each SNR is reported. The electron energy budget (We) is given for Ee> 1 GeV. For RX J0852.0−4622 and SN 1006, We was given for E> 10 MeV (respectively 100 MeV), and the values in the table have been rescaled.
Reference. 1) Abdo et al. (2011); 2) Acero et al. (2007); 3) Acero et al. (2009); 4) Acero et al. (2010); 5) Abramowski et al. (2011); 6) Aharonian et al. (2007a); 7) Aharonian et al. (2007b); 8) Aharonian et al. (2009); 9) Allen et al. (2015); 10) Bocchino et al. (2000); 11) Cassam-Chenaï et al. (2004); 12) Fesen et al. (2012); 13) Katsuda et al. (2008); 14) Katsuda et al. (2009); 15) Lemoine-Goumard et al. (2012); 16) Miceli et al. (2012); 17) Moriguchi et al. (2005); 18) Paz Arribas et al. (2012); 19) Sollerman et al. (2003); 20) Tanaka et al. (2011); 21) Tian et al. (2008); 22) Tian et al. (2010); 23) Winkler et al. (2003); 24) Yuan et al. (2014).
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