Table 6
Epochs, flux ratios, positions, proper motions, and accelerations used to simulate the DSO and the neighboring stars with results shown in Fig. A.1.
| Name | Flux | Epoch | Δα | Δδ | pmα | pmδ | accα | accδ |
| ratio | year | mas | mas | mas yr-1 | mas yr-1 | mas yr-2 | mas yr-2 | |
|
|
||||||||
| S23 | 1.01 | 2005.47 | 307.4 | −89.1 | 14.81 | 11.17 | −0.953 | 0.525 |
| S57 | 1.24 | 2007.46 | 393.6 | −147.4 | 9.99 | 4.05 | 0.000 | 0.000 |
| S63 | 0.83 | 2004.00 | 245.0 | −150.0 | 13.00 | −3.60 | 0.000 | 0.000 |
| DSO | 0.30 | 2002.00 | 295.0 | −160.0 | 17.60 | −14.00 | −0.160 | −0.240 |
| S54 | 1.36 | 2006.59 | 115.4 | −60.1 | 1.05 | 26.90 | 0.000 | 0.000 |
Notes. The flux ratios have been calculated with respect to the mean flux derived (mK = 17.6) from the Ks-band magnitudes of S23, S54, S57, and S63 as given by Gillessen et al. (2009). They correspond (with an estimated uncertainty of 30%) to the relative fluxes suggested by the modeling presented in the figures listed above. From the quality of the fit in these figures we estimate that the uncertainties are 10 mas for the coordinates, 1 mas yr-1 for the proper motions, and 0.1 mas yr-1 for the accelerations.
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