Table 5.
Best-fit orbital elements of the dusty sources.
| ID | Source | a [mpc] | e | i [°] | ω [°] | Ω [°] | tclosest [yr] | PA [°] |
|---|---|---|---|---|---|---|---|---|
| 1 | D2 | 30.01 ± 0.04 | 0.15 ± 0.02 | 57.86 ± 1.71 | 44.11 ± 1.14 | 221.16 ± 1.43 | 2002.16 ± 0.03 | 129.9 |
| 2 | D23 | 44.24 ± 0.03 | 0.06 ± 0.01 | 95.68 ± 1.14 | 93.39 ± 1.89 | 120.89 ± 3.15 | 2016.00 ± 0.03 | –84.2 |
| 3 | D3 | 35.20 ± 0.01 | 0.24 ± 0.02 | 50.99 ± 1.20 | 63.59 ± 2.29 | 206.26 ± 1.76 | 2002.23 ± 0.01 | 147.6 |
| 3/1 | D3.1 | 31.46 ± 0.01 | 0.06 ± 0.02 | 63.02 ± 1.04 | 231.47 ± 1.18 | 47.89 ± 0.96 | 2004.37 ± 0.008 | –137.5 |
| 4 | D5 | 2983.10 ± 2.11 | 0.991 ± 0.001 | 100.84 ± 4.58 | 343.20 ± 8.02 | 73.33 ± 3.89 | 2008.95 ± 3.43 | 103.1 |
| 5 | D9 | 44.00 ± 1.145 | 0.32 ± 0.01 | 102.55 ± 1.14 | 127.19 ± 8.02 | 257.25 ± 1.71 | 2309.13 ± 7.01 | –45.9 |
| 6 | OS1 | 16.53 ± 0.50 | 0.758 ± 0.075 | 107.71 ± 20.68 | 93.96 ± 8.42 | 88.23 ± 16.50 | 2020.68 ± 0.02 | –86.6 |
| 7 | OS2 | 12.54 ± 0.19 | 0.633 ± 0.019 | 95.11 ± 4.98 | 138.65 ± 4.92 | 114.01 ± 2.17 | 2029.41 ± 0.05 | –122.8 |
| 8 | G1 | 48.58 ± 0.05 | 0.968 ± 0.009 | 108.28 ± 1.79 | 114.59 ± 4.69 | 99.69 ± 4.89 | 2001.08 ± 0.05 | –80.9 |
| 9 | G2/DSO | 17.23 ± 0.20 | 0.963 ± 0.004 | 120.32 ± 2.40 | 92.81 ± 1.60 | 63.02 ± 1.37 | 2014.43 ± 0.01 | –59.4 |
| 10 | X7 | 149.99 ± 0.36 | 0.76 ± 0.05 | 74.82 ± 7.84 | 190.22 ± 17.47 | 25.15 ± 10.77 | 1975.85 ± 0.30 | 178.7 |
| 11 | X7.1 | 171.34 ± 5.27 | 0.97 ± 0.02 | 89.38 ± 3.72 | 28.64 ± 17.18 | 60.90 ± 8.59 | 2040.99 ± 15.41 | 117.7 |
| 12 | X8 | 48.69 ± 1.12 | 0.99 ± 0.01 | 95.11 ± 5.61 | 57.24 ± 5.90 | 40.10 ± 4.52 | 1992.92 ± 10.54 | –33.4 |
Notes. See Fig. 1 for the related ID of the dusty sources. The uncertainties are adapted from the MCMC simulations. The first column indicates the ID as provided in the inset in Fig. 1, where we mark the approximate position of the related dusty source (second column). As proposed in Peißker et al. (2020c), D3.1 is most likely a dust and gas filament, such as the Brγ-bar (see Schödel et al. 2011) with a weak radio/submillimeter counterpart (Yusef-Zadeh et al. 2017b).
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