Table 1
Results from the spectral fit of datasets S2–S4 and H1–H2.
| Dataset | texp (a) (h) | rh (au) | ρ(b) (km) (m−2) |  |
fatten |  (K) |
 (K) |
OPR(d) |
|---|---|---|---|---|---|---|---|---|
| S2 | 18.0 | 1.310 | 305 | (6.50 ± 0.18) × 1018 | – | – | 38±2 | 2.79 ± 0.13 |
| S3 | 70.5 | 2.292 | 4.60 | (4.76 ± 0.08) × 1019 | – | – | 68 ± 2 | 2.53 ± 0.10 |
| S4 | 13.6 | 1.543 | 12.0 | (4.61 ± 0.08) × 1019 | – | – | 48 ± 1 | 2.26 ± 0.07 |
| H1 | 72.4 | 1.319 | 3.15 | (13.7 ± 0.34) × 1020 | 0.47 ± 0.01 | 120±1 | 136±4 | 2.62 ± 0.16 |
| H2 | 26.9 | 1.525 | 8.83 | (1.23 ± 0.15) × 1020 | 0.62 ± 0.12 | 54± 10 | 59±1 | 2.73 ± 0.56 |
Notes. (a)Total exposure time. (b)Mean distance of the FOV to comet centre. (c)For datasets S2, S3, and S4, the column density is 
derived from the intensity in the MB (2.590–2.760 μm) spectral region; for datasets H1 and H2, the column density is 
, derived from the intensity in the HB (2.774–2.91 μm) spectral region. (d)For datasets S1, S2, and S3, the OPR is derived by fitting the MB spectral range; for datasets H1 and H2, the OPR is derived by fitting the HB range.
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