Table 3
Compilation of astrometric measurements for the AB Dor B system.
| Relative positions AB Dor Bb − AB Dor Ba | ||||
| Epoch | Instrument | Δα (mas) | Δδ (mas) | Reference |
|
|
||||
| 2004.091 | VLT (IR) | −56.8 ± 3.0 | −33.1 ± 3.0 | (1) |
| 2005.019 | ″ | −64.6 ± 3.0 | −27.4 ± 3.0 | (1) |
| 2005.909 | ″ | −66.7 ± 3.0 | −4.0 ± 3.0 | (1) |
| 2008.650a | ″ | 9.6 ± 3.0 | −16.4 ± 3.0 | (1) |
| 2008.855 | ″ | −61.3 ± 3.0 | −9.9 ± 3.0 | (1) |
| 2008.967 | ″ | −61.5 ± 3.0 | −24.8 ± 3.0 | (1) |
| 2009.003 | ″ | −57.3 ± 3.0 | −26.7 ± 3.0 | (1) |
| 2009.131 | ″ | −45.6 ± 3.0 | −32.7 ± 3.0 | (1) |
| 2007.863 | LBA (radio) | −62.0 ± 0.3 | −10.5 ± 0.7 | (2) |
| 2010.816 | ″ | −60.3 ± 1.5 | −9.7 ± 1.4 | (2) |
| 2013.625 | ″ | −31.3 ± 0.4 | 9.3 ± 0.9 | (2) |
|
|
||||
| Absolute positions AB Dor B (LBA) | ||||
| Epoch | Component | RA (h m s) | Dec (° ′ ′′) | |
|
|
||||
| 1992.685 | Bb | 5 28 44.41973 ± 0.00060 | −65 26 47.0047 ± 0.0021 | (3) |
| 1993.123 | Ba | 5 28 44.40441 ± 0.00080 | −65 26 46.9869 ± 0.0028 | (3) |
| 2007.863 | Ba | 5 28 44.57761 ± 0.00008 | −65 26 45.1002 ± 0.0010 | (2) |
| Bb | 5 28 44.56766 ± 0.00008 | −65 26 45.1107 ± 0.0010 | (2) | |
| 2010.816 | Ba | 5 28 44.61098 ± 0.00019 | −65 26 44.7132 ± 0.0008 | (2) |
| Bb | 5 28 44.60130 ± 0.00014 | −65 26 44.7229 ± 0.0008 | (2) | |
| 2013.625 | Ba | 5 28 44.63954 ± 0.00015 | −65 26 44.2920 ± 0.0009 | (2) |
| Bb | 5 28 44.63453 ± 0.00013 | −65 26 44.2827 ± 0.0008 | (2) | |
Notes.
In Wolter et al. (2014) this position was instead considered to be an upper bound of 19 mas for the separation of Ba/Bb at 2008.855. (1) Wolter et al. (2007); (2) This study; (3) Guirado et al. (2006). The standard deviation of the relative position corresponds to the uncertainty based on the signal-to-noise ratio of the peaks of brightness of AB Dor Ba and Bb. The absolute positions were obtained with reference to the IERS coordinate of the external quasar PKS 0516−621 (
). The standard deviation of the absolute position includes, in addition to the uncertainty of their respective peaks of brightness, the contribution of the propagation media and the reference source structure.
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