Table 4
Best-fit model parameters for Nuker fits to faint stars.
| ID | rb | γ | β | ρ(rb) |
|
| (pc) | (pc-3) | ||||
|
|
|||||
| 1a | 5.2 ± 0.6 | 1.45 ± 0.03 | 4.6 ± 0.7 | 40 ± 7 | 1.7 |
| 2b | 5.0 ± 0.5 | 1.44 ± 0.03 | 4.1 ± 0.5 | 46 ± 7 | 1.7 |
| 3c | 5.0 ± 0.5 | 1.44 ± 0.03 | 4.1 ± 0.5 | 46 ± 7 | 1.7 |
| 4d | 4.8 ± 0.5 | 1.43 ± 0.03 | 3.5 ± 0.3 | 53 ± 7 | 1.7 |
| 5e | 4.9 ± 0.5 | 1.42 ± 0.03 | 3.5 ± 0.3 | 53 ± 7 | 1.7 |
| 6f | 5.0 ± 0.7 | 1.43 ± 0.03 | 3.6 ± 0.6 | 46 ± 14 | 2.0 |
| 7g | 5.0 ± 0.5 | 1.46 ± 0.03 | 3.6 ± 0.3 | 46 ± 7 | 1.7 |
| 8h | 5.3 ± 0.7 | 1.41 ± 0.03 | 3.7 ± 0.4 | 39 ± 14 | 1.7 |
| 9i | 4.8 ± 0.4 | 1.43 ± 0.03 | 3.5 ± 0.3 | 53 ± 7 | 1.7 |
| 10j | 4.3 ± 0.5 | 1.29 ± 0.05 | 3.4 ± 0.3 | 72 ± 14 | 2.0 |
| 11k | 4.4 ± 0.4 | 1.29 ± 0.05 | 3.4 ± 0.2 | 72 ± 14 | 1.9 |
Notes.
Fit range: 0.04 ≤ R ≤ 20 pc. Fore-/background emission model 1 of Table 2 in Schödel et al. (2014a).
Fit range: 0.04 ≤ R ≤ 20 pc. Fore-/background emission model 2 of Table 2 in Schödel et al. (2014a).
Fit range: 0.04 ≤ R ≤ 20 pc. Fore-/background emission model 3 of Table 2 in Schödel et al. (2014a).
Fit range: 0.04 ≤ R ≤ 20 pc. Fore-/background emission model 4 of Table 2 in Schödel et al. (2014a).
Fit range: 0.04 ≤ R ≤ 20 pc. Fore-/background emission model 5 of Table 2 in Schödel et al. (2014a).
Fit range: 0.04 ≤ R ≤ 10 pc. Fore-/background emission model 5 of Table 2 in Schödel et al. (2014a).
Fit range: 0.04 ≤ R ≤ 20 pc. Fore-/background emission model 5 of Table 2 in Schödel et al. (2014a). Lower integration boundary at r = R + 0.01 pc.
Fit range: 0.04 ≤ R ≤ 20 pc. Fore-/background emission model 5 of Table 2 in Schödel et al. (2014a). α = 5.
Fit range: 0.04 ≤ R ≤ 20 pc. Fore-/background emission model 5 of Table 2 in Schödel et al. (2014a). α = 20.
Fit range: 0.04 ≤ R ≤ 20 pc. Fore-/background emission model 5 of Table 2 in Schödel et al. (2014a). Subtracted potential contamination by pre-MS stars as in model 4 of Table 3.
Fit range: 0.04 ≤ R ≤ 20 pc. Fore-/background emission model 5 of Table 2 in Schödel et al. (2014a). Subtracted potential contamination by pre-MS stars as in model 1 of Table 3.
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