Table 6.
Comparison with previous studies.
| Study | Wavelength | Angular resolution | Scales | q | n | Re |
|---|---|---|---|---|---|---|
| (μm) | (arcsec) | (pc2) | (pc) | |||
| Schödel et al. (2014a,b) | 4.5 | 2 | 200 × 200 | 0.71 ± 0.02 | 2 ± 0.2 | 4.2 ± 0.4 |
| Fritz et al. (2016) | 2.2 | 1 | 80 × 80 | 0.80 ± 0.04 | 1.5 ± 0.1 | 7 ± 2 |
| Present work NIR | 2.2 | 0.2 | 86 × 20.2 | 0.75 ± 0.01 | 2.26 ± 0.21 | 5.36 ± 0.35 |
| Present work MIR | 4.5 | 2 | 300 × 250 | 0.66 ± 0.03 | 1.8 ± 0.1 | 4.9 ± 0.5 |
Notes. Fritz et al. (2016) use data with different resolution. We show the resolution for larger distances (R > 2.72 pc) where they used VISTA data. For distances R ≤ 0.8 pc, they use NACO data with an angular resolution of 0.08″. For distances 0.8 pc ≤ R ≤2.72 pc they use (HST) WFC3/IR data with an angular resolution of 0.15″. The present study presents results for stars with magnitudes in the range 11.0 ≤ Ks ≤ 16.0 (ID 3 in Table 3). We show the resolution for larger distances where we use the GALACTICNUCLEUS survey. For distances R ≤ 2 pc, we use NACO data with an angular resolution of 0.05″. We also present the results from using MIR.
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