Table 2.
Overview of direct proper motion measurements and exact positions for all CCOs.
| SNR | CCO | α0 (J2000.) | δ0 (J2000.) | t0 | μα | μδ | μtot | d′ | vproj | Reference |
|---|---|---|---|---|---|---|---|---|---|---|
| (h:m:s) | (d:m:s) | (MJD) | (mas yr−1) | (mas yr−1) | (mas yr−1) | (kpc) | (km s−1) | |||
| G15.9+0.2 | CXOU J181852.0−150213 | 18:18:52.072 |
−15:02:14.05 |
57 233 | −17 ± 12 | −4 ± 10 | < 25 | 10 | < 1200 | This work |
| Kes 79 | CXOU J185238.6+004020 | 18:52:38.561 |
+00:40:19.60 |
57 441 |
 |
 |
< 19 | 5.0 | < 450 | This work |
| Cas A | CXOU J232327.9+584842 | 23:23:27.932 |
+58:48:42.05 |
55 179 |
 |
 |
 |
3.4 | 570 ± 260 | This work |
| Puppis A | RX J0822−4300 | 08:21:57.274 |
−43:00:17.33 |
58 517 |
 |
−30.3 ± 6.2 | 80.4 ± 7.7 | 2.0 | 763 ± 73 (b) | 1 |
| G266.1−1.2 (Vela Jr.) | CXOU J085201.4−461753 | 08:52:01.37 (a) | −46:17:53.5 (a) | 51 843 | ...(c) | ...(c) | < 300 | 1.0 | < 1400 | 2,3 |
| PKS 1209−51/52 | 1E 1207.4−5209 | 12:10:00.913 |
−52:26:28.30  |
54 823 | ...(c) | ...(c) | 15 ± 7 | 2.0 | < 180 | 4 |
| G330.2+1.0 | CXOU J160103.1−513353 | 16:01:03.148 |
−51:33:53.82 |
57 878 |
 |
 |
< 9.9 | 5.0 | < 230 | This work |
| RX J1713.7−3946 | 1WGA J1713.4−3949 | 17:13:28.30 (a) | −39:49:53.1 (a) | 56 360 |
 |
−20 ± 29 | < 48 | 1.0 | < 230 | This work |
| G350.1−0.3 | XMMU J172054.5−372652 | 17:20:54.585 |
−37:26:52.85 |
58 308 | −3 ± 8 |
 |
 |
4.5 |
 |
This work |
| G353.6−0.7 | XMMU J173203.3−344518 | 17:32:03.41 (a) | −34:45:16.6 (a) | 54 584 | ... | ... | ...(d) | 3.2 | ...(d) | 5,6 |
Notes. To provide a complete four-parameter astrometric solution, we display the best-fit positions of the CCO (α0, δ0) at a given epoch t0, corresponding to the latest available observation of the respective target. The values for the projected physical velocity vproj are scaled to an assumed distance d′, without the inclusion of any additional errors to account for uncertainties in d′. The measurements of total proper motion μtot and projected velocity vproj from this work have been corrected for the effect of Galactic rotation. All our measurements and errors correspond to the median and 68% central interval of the underlying probability distribution. All upper limits derived in this work are at 90% confidence.
The positions without listed uncertainties have not been corrected for Chandra’s absolute astrometric inaccuracy, and therefore have estimated 1σ–errors on the order of 0.4″, corresponding to an 0.8″ radius of the two-dimensional 90% confidence region.
The most recent distance measurement of around 1.3 kpc (Reynoso et al. 2017) to Puppis A would imply a transverse velocity of vproj = (496 ± 47) km s−1 for the CCO.
Due to the lack of suitable data, no proper-motion measurement currently exists for the CCO of G353.6−0.7.
References. (1) Mayer et al. (2020), (2) Mignani et al. (2007), (3) Mignani et al. (2019), (4) Halpern & Gotthelf (2015), (5) Halpern & Gotthelf (2010b), (6) Maxted et al. (2018).
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