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Table B.1.

Full results of proper motion measurements and astrometric calibration of the individual observations for the six CCOs targeted in this work.

SNR CCO μα μδ α0 δ0
(mas yr−1) (mas yr−1) (arcsec) (arcsec)
G15.9+0.2 CXOU J181852.0−150213
Kes 79 CXOU J185238.6+004020
Cas A CXOU J232327.9+584842
G330.2+1.0 CXOU J160103.1−513353
RX J1713.7−3946 1WGA J1713.4−3949 ...(a) ...(a)
G350.1−0.3 XMMU J172054.5−372652

SNR Observation ID Δxi Δyi ri − 1 θi
(arcsec) (arcsec) (10−4) (10−4 rad)

G15.9+0.2 5530
6288
6289
16766

Kes 79 17453
17659
1982

Cas A 1505
Late (b)

G330.2+1.0 19163
20068
6687

RX J1713.7−3946 5559 − 13284 (a)

G350.1−0.3 10102
20312
20313
21118
21119
21120

Notes. The upper part of the table displays the best-fit astrometric solution for each CCO – proper motion and position at a reference time – as resulting from our fit. In the lower part, we show for all systems the optimal determined astrometric calibration parameters – describing translation, stretch and rotation of the coordinate system – for each individual observation.

(a)

For RX J1713.7−3946, only relative astrometric analysis was performed, via direct subtraction of positions from the two epochs. Therefore, our fit provides no absolute source positions.

(b)

For Cas A, the closely spaced individual observations (IDs 11240, 12057, 12058, 12059) were merged to create a single late-time data set. The tangent points that we used for conversion of celestial coordinates to a (right-handed) local Cartesian coordinate system and as center of scaling and rotation, were for G15.9+0.2, for Kes 79, for Cas A, for G330.2+1.0, for RX J1713.7−3946, and for G350.1−0.3.

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