Table 2.
Summary of constraints for the ambient density close to the GC at the S2 periapse based on the two extinction limits, 1σ and fractional variability, and analytical bow-shock models for both the ambient shock and the stellar-wind shock thermal emission.
| Thermal emission – upper limit | Power-law slope | Ambient number density (periapse) |
|---|---|---|
| Ambient shock (A = 0.04) | 3.20 | 1.87 × 109 cm−3 |
| Stellar-wind shock (A = 0.04) | 1.57 | 1.86 × 105 cm−3 |
| Thermal emission – upper limit | Power-law slope | Ambient number density (periapse) |
| Ambient shock (A = 0.02) | 3.03 | 7.15 × 108 cm−3 |
| Stellar-wind shock (A = 0.02) | 1.41 | 7.53 × 104 cm−3 |
| Non-thermal emission – upper limit | Power-law slope | Ambient number density (periapse) |
| Peak flux density of 0.91 mJy (maximum flux difference) | 1.47 | 1.01 × 105 cm−3 |
| Peak flux density of 0.22 mJy (fractional variability) | 1.17 | 1.88 × 104 cm−3 |
Notes. In addition, we include the ambient density upper limit for the non-thermal synchrotron emission based on the maximum flux difference of 0.90 mJy and the fractional variability of 0.2 mJy.
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