Table E.3
Hot star candidates with proper motion measurement.
| Source name | pml[mas· yr−1] | σ pml [mas· yr−1] | pmb[mas· yr−1] | σ pmb [mas· yr−1] | H - KS [mag] | xoffset [arcsec] | yoffset [arcsec] | PQ |
|---|---|---|---|---|---|---|---|---|
| F2_26653311-28833078_Ks12.48 | -2.64131 | 0.17644 | -2.06506 | 0.18685 | 0.14 | 727.90 | 14.55 | 0.0 |
| F2_26653436-28831776_Ks99.00 | -2.22163 | 0.15722 | -0.15861 | 0.16876 | ... | 733.96 | 13.62 | 0.68 |
| F2_26653812-28830481_Ks13.48 | -3.25798 | 0.10660 | 0.96662 | 0.11696 | 0.12 | 744.11 | 5.92 | 0.0 |
| F2_26654034-28827679_Ks11.74 | -4.26246 | 0.08474 | 0.09750 | 0.09223 | 1.64 | 756.36 | 5.18 | 0.0 |
| F2_26654547-28825665_Ks11.71 | -2.56479 | 0.06036 | -0.40243 | 0.06097 | 1.66 | 770.97 | -4.87 | 0.92 |
| F2_26654773-28826262_Ks12.68 | -2.48197 | 0.05071 | -0.48074 | 0.05188 | 1.60 | 772.84 | -12.07 | 0.93 |
| F2_26655209-28824980_Ks10.63 | -2.63055 | 0.06036 | -0.31353 | 0.06097 | 1.60 | 783.93 | -21.42 | 0.86 |
| F2_26655139-28821077_Ks12.61 | -2.56704 | 0.07745 | -0.32171 | 0.07290 | 1.49 | 794.79 | -12.23 | 0.91 |
| F2_26654932-28818583_Ks10.55 | -2.57111 | 0.09681 | -0.48814 | 0.09113 | 1.54 | 799.06 | -1.98 | 0.88 |
| F2_26655266-28819681_Ks11.80 | -2.56853 | 0.08713 | -0.35771 | 0.08202 | 1.49 | 801.18 | -13.06 | 0.91 |
| F2_26655383-28816727_Ks8.90 | -2.51840 | 0.14313 | -0.15156 | 0.13062 | 2.07 | 812.17 | -10.66 | 0.80 |
| F2_26655600-28816496_Ks9.86 | -2.73455 | 0.13345 | -0.41186 | 0.12151 | 1.73 | 816.44 | -16.07 | 0.71 |
Notes. The columns denote the source name, proper motion from Hosek et al. (2022) along Galactic longitude l, associated uncertainty, proper motion along Galactic latitude b, associated uncertainty, colour H - KS, offset coordinates from Sgr A*, and Quintuplet membership probability PQ assigned by Hosek et al. (2022). We note the systematic offset to Table E.1 since the proper motions are in the absolute Gaia reference frame. The motion of Quintuplet is pml=−2.45528 mas· yr−1, pmb=-0.3705 mas· yr−1.
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