Table 2
Apparent separations from the star (in arcseconds) of the maximum elevation from midplane of the five arch-like structures, named A to E, observed in the AU Mic debris disk in 2010, 2011, and 2014.
| Date | A | B | C | D | E | Reference |
|
|
||||||
| 2014.69 | 1.017 ± 0.025 | 1.714 ± 0.037 | 2.961 ± 0.073 | 4.096 ± 0.049 | 5.508 ± 0.074 | Boccaletti et al. (2015) |
| 2011.63 | 0.750 ± 0.025 | 1.384 ± 0.025 | 2.554 ± 0.025 | 3.491 ± 0.025 | 4.912 ± 0.208 | Boccaletti et al. (2015) |
| 2010.69 | – | 1.259 ± 0.037 | 2.459 ± 0.049 | 3.369 ± 0.061 | 4.658 ± 0.245 | Boccaletti et al. (2015) |
|
|
||||||
| 2004.75 | – | – | – | 2.52 | 3.22 | Fitzgerald et al. (2007) |
| 2004.58 | – | – | – | 2.52 | 3.12 | Liu (2004) |
| 2004.51 | – | – | – | 2.21 | 3.22 | Metchev et al. (2005) |
| 2004.34 | – | – | – | 2.62 | 3.32 | Krist et al. (2005) |
|
|
||||||
| 2004.545 ± 0.147 | – | – | – | 2.468 ± 0.154 | 3.220 ± 0.071 | |
Notes. In 2010, structure A is angularly too close to the star to be detectable. For consistency among all the features, the uncertainties on the positions of features A and B in 2011 have been re-estimated to twice their values, as published in Boccaletti et al. (2015). The next four rows give the positions of brightness enhancements (and not the maximum elevation positions) identified in 2004 and associated a posteriori to structures D and E. The last row shows the mean positions and uncertainties on the structures seen in 2004.
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