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.
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.
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.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.