Table B.1.
Best-fit orbit parameters of the four-star fit determining fSP.
| this paper | Grav. Coll. 2020 | Gillessen+ 2017 | Do+ 2019 | |||||
|---|---|---|---|---|---|---|---|---|
| M• [106M⊙] | 4.297 | 0.012 | 4.261 | 0.012 | 4.280 | 0.100 | 3.975 | 0.058 |
| R0 [pc] | 8277 | 9 | 8247 | 9 | 8320 | 70 | 7959 | 59 |
| M• [106M⊙]8277 pc | 4.297 | 0.012 | 4.292 | 0.012 | 4.236 | 0.100 | 4.299 | 0.063 |
| x0 [mas] | -0.69 | 0.10 | -0.90 | 0.14 | -0.08 | 0.37 | 1.22 | 0.32 |
| y0 [mas] | 0.18 | 0.10 | 0.07 | 0.12 | -0.89 | 0.31 | -0.88 | 0.34 |
| vx0 [mas/yr] | 0.066 | 0.006 | 0.080 | 0.010 | 0.039 | 0.041 | -0.077 | 0.018 |
| vy0 [mas/yr] | 0.009 | 0.009 | 0.034 | 0.010 | 0.058 | 0.037 | 0.226 | 0.019 |
| vz0 [km/s] | -1.8 | 1.3 | -1.6 | 1.4 | 14.2 | 3.6 | -6.2 | 3.7 |
| fSP | 0.997 | 0.144 | 1.10 | 0.19 | ||||
| S2 | S38 | |||||||
| a [as] | 0.12495 | 0.00004 | 0.14254 | 0.00004 | ||||
| e | 0.88441 | 0.00006 | 0.8145 | 0.0002 | ||||
| i [°] | 134.70 | 0.03 | 166.65 | 0.40 | ||||
| Ω [°] | 228.19 | 0.03 | 109.45 | 1.00 | ||||
| ω [°] | 66.25 | 0.03 | 27.17 | 1.02 | ||||
| tperi [yr] | 2018.3789 | 0.0001 | 2022.7044 | 0.0080 | ||||
| S29 | S55 | |||||||
| a [as] | 0.3975 | 0.0016 | 0.10440 | 0.00005 | ||||
| e | 0.9693 | 0.0001 | 0.7267 | 0.0002 | ||||
| i [°] | 144.37 | 0.07 | 158.52 | 0.22 | ||||
| Ω [°] | 7.00 | 0.33 | 314.94 | 1.14 | ||||
| ω [°] | 205.79 | 0.33 | 322.78 | 1.13 | ||||
| tperi [yr] | 2021.4104 | 0.0002 | 2021.6940 | 0.0083 | ||||
The line M• [106M⊙]8277 pc gives the masses rescaled to a common distance of R0 = 8277 pc, using 
(Gillessen et al. 2017). For a discussion of the differences in R0 see the appendix of GRAVITY Collaboration (2021). The orbital elements are meant in the sense of osculating orbit parameters, using a conversion time close to the respective apocenter times, i.e., 2010.35 for S2, 1977 for S29, 2000 for S38, and 2012 for S55. The coordinate system offsets x0, y0 refer to the epoch 2000.0.
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