Table 2
Obtained values for α and A1.61 using the grid method.
| αJH | αHK | A1.61_JH | A1.61_HK | Δα | |
|---|---|---|---|---|---|
| Central | 2.40 ± 0.07 | 2.20 ± 0.12 | 3.40 ± 0.12 | 3.39 ± 0.12 | 0.20 ± 0.12 |
| NSD E | 2.42 ± 0.07 | 2.25 ± 0.12 | 3.29 ± 0.12 | 3.29 ± 0.12 | 0.17 ± 0.12 |
| NSD W | 2.38 ± 0.08 | – | 2.96 ± 0.12 | – | – |
| T E | 2.45 ± 0.09 | 2.32 ± 0.16 | 2.56 ± 0.12 | 2.56 ± 0.12 | 0.13 ± 0.15 |
| T W | 2.45 ± 0.10 | 2.21 ± 0.16 | 2.47 ± 0.12 | 2.47 ± 0.12 | 0.24 ± 0.15 |
| I B S | 2.40 ± 0.08 | 2.21 ± 0.15 | 2.71 ± 0.12 | 2.70 ± 0.12 | 0.19 ± 0.14 |
| I B N | 2.50 ± 0.11 | 2.17 ± 0.18 | 2.12 ± 0.12 | 2.11 ± 0.12 | 0.33 ± 0.17 |
Notes. A1.61_ JH and A1.61_ HK indicate the value of the extinction at 1.61 μm obtained using the bands JH and HKs, respectively. The uncertainties correspond to the systematic ones. The statistical uncertainties are negligible given the high number of stars used for the calculation. The αHK and A1.61_HK values for the NSD W were not computed due to the low number of stars detected in the RC feature and the bad weather conditions when observing Ks band. It affected the photometry as indicated by the scattering in Fig. 7 of Nogueras-Lara et al. (2019a) and might lead to biased results.
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