Table 8.
LLs of the form m = α(log P − 10)+β fit to LMC Cepheids.
| Band | LMC |
WIS | ||
|---|---|---|---|---|
| β | α | nLMC | ||
| (mag) | (mag/log P) | (mag) | ||
| Bp | 14.329 ± 0.016 | −2.717 ± 0.055 | 546 | 0.23 |
| V | 14.187 ± 0.014 | −2.669 ± 0.049 | 701 | 0.22 |
| G | 14.066 ± 0.013 | −2.857 ± 0.046 | 546 | 0.19 |
| Rp | 13.611 ± 0.011 | −2.962 ± 0.037 | 546 | 0.16 |
| I | 13.580 ± 0.011 | −2.872 ± 0.038 | 712 | 0.14 |
| F160Wa | 12.923 ± 0.014 | −3.229 ± 0.056 | 68 | 0.09 |
| WVI | 12.870 ± 0.008 | −3.181 ± 0.029 | 684 | 0.08 |
| WG | 12.669 ± 0.005 | −3.347 ± 0.020 | 543 | 0.10 |
 |
12.643 ± 0.011 | −3.290 ± 0.044 | 68 | 0.06 |
Notes. β is expressed here in apparent magnitudes. The last column indicates the intrinsic width of the LL due to the finite width of the instability strip (WIS), adopted from Breuval et al. (2022). Superscript a indicates that no HST F160W-IR CRNL corrections were applied to observations of LMC Cepheids for this comparison. Magnitudes in the NIR Wesenheit function were recomputed using Eq. (5) based on the observations reported by Riess et al. (2019a).
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