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Table 2.

Fit position and relative brightness of the faint star.

Date of the δ RA δ RA err. δ Dec δ Dec err. Relative Relative 1-σ Number of
averaged image (mas) (mas) (mas) (mas) brightness brightness of S2 noise level frames used
2019.30 (Apr.18) −19.18 0.18 20.78 0.27 0.009 0.013 0.0019 27
2019.47 (Jun.19) −18.78 0.14 19.80 0.23 0.009 0.011 0.0018 15
2019.54 (Jul.17) −18.62 0.26 19.73 0.30 0.007 0.009 0.0017 39
2019.62 (Aug.16) −18.49 0.11 19.88 0.29 0.008 0.009 0.0014 83
2019.70 (Sep.12) −18.14 0.15 19.57 0.34 0.009 0.011 0.0017 31

Notes. Fit position of our detected target relative to Sgr A* and the image noise level for the best Sgr A*-removed image per month. The positive sign signals the east and north of Sgr A* in the right ascension and declination directions, respectively. The brightness level is a normalized quantity, with the maximum unity, which corresponds to the brightness of S2, if it were in the field center. Here, the brightness levels do not reflect the physical brightness of the stars, as they are also affected by bandwidth smearing and fiber damping.

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