Table 1.
CCOs with basic properties of their host SNRs.
| SNR | CCO | Distance | Age | References |
|---|---|---|---|---|
| (kpc) | (yr) | |||
| G15.9+0.2 | CXOU J181852.0−150213 | 7 − 16 | 2900 − 5700 | 1,2,3 |
| Kes 79 | CXOU J185238.6+004020 | 3.5 − 7.1 | 4400 − 6700 | 4,5,6,7 |
| Cas A | CXOU J232327.9+584842 | 3.4 | ∼350 | 8,9 |
| Puppis A | RX J0822−4300 | 1.3 − 2.2 | 2000 − 5300 | 10,11,12,13,14 |
| G266.1−1.2 (Vela Jr.) | CXOU J085201.4−461753 | 0.5 − 1.0 | 2400 − 5100 | 15 |
| PKS 1209−51/52 (G296.5+10.0) | 1E 1207.4−5209 | 1.3 − 3.9 | ∼7000 | 16,17 |
| G330.2+1.0 | CXOU J160103.1−513353 | 4.9 − 10.0 | ≲1000 | 18,19,20 |
| RX J1713.7−3946 (G347.3−0.5) | 1WGA J1713.4−3949 | 1.0 − 1.3 | 1500 − 2300 | 21,22,23,24 |
| G350.1−0.3 | XMMU J172054.5−372652 | 4.5 | ∼600 | 25,26,27 |
| G353.6−0.7 | XMMU J173203.3−344518 | ∼3.2 | ∼27 000 | 28,29 |
Notes. The two SNRs G349.7+0.2 (Lazendic et al. 2005) and G296.8−0.3 (Sánchez-Ayaso et al. 2012) have been claimed to potentially host CCOs. Since Chandra data suitable for our purposes do not exist for either SNR, these sources are not considered further in our work.
References. (1) Tian et al. (2019), (2) Sasaki et al. (2018), (3) Maggi & Acero (2017), (4) Ranasinghe & Leahy (2018), (5) Kuriki et al. (2018), (6) Kilpatrick et al. (2016), (7) Zhou et al. (2016), (8) Fesen et al. (2006), (9) Alarie et al. (2014), (10) Reynoso et al. (2017), (11) Reynoso et al. (2003), (12) Aschenbach (2015), (13) Winkler et al. (1988), (14) Mayer et al. (2020), (15) Allen et al. (2015), (16) Giacani et al. (2000), (17) Roger et al. (1988), (18) McClure-Griffiths et al. (2001), (19) Williams et al. (2018), (20) Borkowski et al. (2018), (21) Fukui et al. (2003), (22) Cassam-Chenaï et al. (2004), (23) Acero et al. (2017), (24) Tsuji & Uchiyama (2016), (25) Lovchinsky et al. (2011), (26) Bitran et al. (1997), (27) Borkowski et al. (2020), (28) Maxted et al. (2018), (29) Tian et al. (2008).
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