Table 2.
NIR photometry of the local sequences for LSQ13abf in the “standard” system.
| ID | α(2000) | δ(2000) | Y | N | J | N | H | N |
|---|---|---|---|---|---|---|---|---|
| 101 | 177.25798 | 19.14391 | 17.270(047) | 1 | 16.899(042) | 3 | 16.434(111) | 3 |
| 102 | 177.30806 | 19.14254 | 17.342(062) | 1 | 17.666(042) | 1 | 16.530(198) | 2 |
| 103 | 177.28269 | 19.19284 | 17.937(123) | 4 | 18.039(093) | 3 | 17.262(093) | 1 |
| 104 | 177.29263 | 19.18621 | 18.482(349) | 2 | 18.231(012) | 2 | 17.338(072) | 1 |
| 105 | 177.25755 | 19.16376 | 18.893(137) | 1 | 18.175(152) | 2 | 17.263(147) | 1 |
| 107 | 177.27550 | 19.14922 | 17.517(069) | 1 | … | … | … | … |
Notes. Values in parenthesis are 1-σ uncertainties computed by taking the weighted average of the instrumental errors of the photometry obtained during the nights photometric standard fields were observed. N represents the number of photometric nights that the local sequence stars were calibrated relative to standard field observations.
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