Table 5
Summary of possible pole solutions in ecliptic coordinates (see Fig. 7) from our analysis of the combined visual and thermal data set.
| Pole solution | Psid | |||
| ID | λ [°] | β [°] | [h] | Zone |
|
|
||||
| 1 | 290 | –20 | 7.63108 | A |
| 2 | 340 | –40 | 7.63109 | A |
| 3 | 310 | –40 | 7.63001 | A |
| 4 | 100 | –70 | 7.63254 | B |
| 5 | 90 | –80 | 7.62997 | B |
| 6 | 130 | –40 | 7.63256 | C |
| 7 | 100 | –40 | 7.63005 | C |
| 8 | 170 | 10 | 7.63123 | D |
| 9 | 190 | 0 | 7.63001 | D |
| 10 | 200 | 20 | 7.63001 | D |
| 11 | 350 | –20 | 7.63256 | E |
Notes. Zone “A” is our preferred solution because this zone is connected to the lowest χ2 and stable against the limit of inertia ratio, the minimum value of Γ, and different resolutions of the shape model (see also Sect. 4.2).
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