Table 7
Estimations of the threshold times needed to detect different effects with the S2 star, considering various astrometric and spectroscopic accuracies.
| Detected effects | |||||
|
|
|||||
| model A | 10 μas | 30 μas | 50 μas | 100 μas | |
|
|
|||||
| Roemer | 1 km s-1 | 1 month | 1 month | 2 months | 4(2) months |
| TD | 10 km s-1 | 2 months | 4 months | 6(4) months | 1 an (10 months) |
| Grav. | 100 km s-1 | 4 months | 10(6) months | 4(1) yr | 16(4) yr |
|
|
|||||
| model B | 10 μas | 30 μas | 50 μas | 100 μas | |
|
|
|||||
| TD | 1 km s-1 | 1 month | 1 month | 2 months | 4 months |
| Grav. | 10 km s-1 | 2 months | 4 months | 6(4) months | 10 months |
| 100 km s-1 | 4 yr (10 months) | 18(10) yr | 18 yr | 18 yr | |
|
|
|||||
| model C | 10 μas | 30 μas | 50 μas | 100 μas | |
|
|
|||||
| PA | 1 km s-1 | 10(6) months [8(2) yr] | 14(12) yr | 18(14) yr | 18 yr |
| GL | 10 km s-1 | 6(4) yr [8(6) yr] | 18 yr | 18 yr | 20 yr |
| HOPC | 100 km s-1 | 6 yr | 18 yr | 18 yr | 20 yr |
|
|
|||||
| model D | 10 μas | 30 μas | 50 μas | 100 μas | |
|
|
|||||
| GL | 1 km s-1 | 6 months | >30 yr | / | / |
| HOPC | 10 km s-1 | 18(4) yr | >30 yr | / | / |
| 100 km s-1 | / | / | / | / | |
|
|
|||||
| model E | 10 μas | 30 μas | 50 μas | 100 μas | |
|
|
|||||
| GL | 1 km s-1 | 6 months | >30 yr | / | / |
| HOPC | 10 km s-1 | 18(6) yr | >30 yr | / | / |
| 100 km s-1 | / | / | / | / | |
|
|
|||||
| model F | 10 μas | 30 μas | 50 μas | 100 μas | |
|
|
|||||
| GL | 1 km s-1 | 18 yr (10 months) | >30 yr | / | / |
| HOPC | 10 km s-1 | >30 yr | >30 yr | / | / |
| 100 km s-1 | / | / | / | / | |
Notes. The main effects that cause each model to fail to explain the full-GR observations are listed in the left column (see Table 2 for the different acronyms). Threshold times given in brackets correspond to those obtained considering a percentage of failure of 60%, instead of 90%. When there are no brackets it means that the thresholds are similar for both percentages. The times given in square brackets for model C are obtained considering mock observations of the S2 star generated with model D instead of model G.
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