Table 2.
Calibrator stars for the data set analyzed.
| Star | H | K | L | M |
|---|---|---|---|---|
| S1 | 16.5 ± 0.1 | 14.6 ± 0.1 | 13.0 ± 0.6 | 12.6 ± 0.4 |
| S2 | 15.9 ± 0.1 | 14.1 ± 0.1 | 12.6 ± 0.7 | 12.8 ± 0.1 |
| S4 | 16.2 ± 0.1 | 14.4 ± 0.1 | 13.1 ± 0.6 | 13.1 ± 0.2 |
| IRS16NW | 12.0 ± 0.02 | 10.0 ± 0.04 | 8.4 ± 0.1 | 6.9 ± 0.1 |
| IRS2L | 14.2 ± 0.2 | 10.6 ± 0.2 | 6.4 ± 0.1 | 5.5 ± 0.1 |
Notes. We adapt the listed magnitude values for IRS16NW from Blum et al. (1996), Stolte et al. (2010), and Gautam et al. (2019). The magnitudes for IRS2L are from Viehmann et al. (2006) and Viehmann (2007). The magnitudes for S1, S2, and S4 are estimated with these two IRS stars. All listed and independent derived magnitudes for the S-stars are in agreement with the literature (S1–S4, L/M-band: Clénet et al. 2004a; S2, K-band: Sabha et al. 2012; S1–S4, K-band: Habibi et al. 2017). With the listed reference stars, we estimate the NIR and MIR magnitudes of S2. Inter alia, we calculate the L-band magnitude of this star to 12.6 ± 0.7 in agreement with Witzel et al. (2014). The magnitude of the standard deviation based uncertainty reflects the admissible fluctuation of S2 (Hosseini et al. 2020). The NIR values of S1 and S4 are calculated with the numerical magnitude results for S2, whereas IRS16NW is used for the MIR magnitude of the S-cluster star. See Appendix D for the complete list of all individual estimated magnitudes over a time of 12 yr.
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