Table 5.
Comparison between present results for ACs in the LMC, the SMC, and the literature.
| Relation | Galaxy | Mode | α | σα | α0 | σα0 | β | σβ | RMS | n.stars | Author |
|---|---|---|---|---|---|---|---|---|---|---|---|
| mag | mag | mag | mag | mag/dex | mag/dex | mag | |||||
| PLG | LMC | F | 17.78 | 0.04 | −0.69 | 0.05 | −2.99 | 0.20 | 0.24 | 83 | TW |
| PLV | theory | F | – | – | −0.69 | 0.14 | −2.73 | – | 0.14 | – | Marconi et al. (2004) |
| PLV | LMC | F | – | – | −0.56 | 0.04 | −3.21 | 0.21 | 0.20 | 32 | Ripepi et al. (2014) |
| PLV | LMC | F | 17.80 | 0.04 | −0.68 | 0.05 | −2.82 | 0.19 | 0.22 | 80 | TW |
| PLV | theory | 1O | – | – | −1.56 | 0.25 | −2.95 | – | 0.25 | – | Marconi et al. (2004) |
| PLV | LMC | 1O | – | – | −1.26 | 0.09 | −3.14 | 0.37 | 0.23 | 10 | Ripepi et al. (2014) |
| PLV | LMC | 1O | 17.10 | 0.04 | −1.38 | 0.05 | −3.31 | 0.32 | 0.22 | 35 | TW |
| PLK | LMC | F | 16.74 | 0.02 | – | – | −3.54 | 0.15 | 0.10 | 32 | Ripepi et al. (2014) |
| PLK | LMC | F | 16.69 | 0.03 | −1.79 | 0.04 | −3.12 | 0.13 | 0.16 | 78 | TW |
| PLK | LMC | 1O | 16.06 | 0.07 | – | – | −4.18 | 0.33 | 0.10 | 10 | Ripepi et al. (2014) |
| PLK | LMC | 1O | 16.13 | 0.02 | −2.35 | 0.04 | −3.41 | 0.18 | 0.13 | 33 | TW |
| PWVI | theory | F | – | – | −1.93 | – | −3.34 | – | 0.20 | – | Marconi et al. (2004) |
| PWVI | LMC | F | 16.59 | 0.02 | – | – | −3.41 | 0.16 | 0.15 | 32 | Ripepi et al. (2014) |
| PWVI | LMC | F | 16.61 | 0.02 | – | – | −3.16 | 0.14 | 0.15 | 62 | Groenewegen & Jurkovic (2017) |
| PWVI | LMC | F | 16.59 | 0.02 | – | – | −2.96 | 0.12 | – | 94 | Iwanek et al. (2018) |
| PWVI | LMC | F | 16.60 | 0.02 | −1.88 | 0.04 | −3.12 | 0.12 | 0.14 | 79 | TW |
| PWVI | SMC | F | 16.95 | 0.02 | – | – | −2.89 | 0.14 | – | 72 | Iwanek et al. (2018) |
| PWVI | SMC | F | 16.95 | 0.03 | – | – | −3.03 | 0.17 | 0.14 | 44 | TW |
| PWVI | LMC | 1O | 16.03 | 0.06 | – | – | −3.37 | 0.25 | 0.14 | 19 | Groenewegen & Jurkovic (2017) |
| PWVI | LMC | 1O | 16.05 | 0.05 | – | – | −3.44 | 0.22 | 0.13 | 10 | Ripepi et al. (2014) |
| PWVI | LMC | 1O | 16.04 | 0.04 | – | – | −3.30 | 0.20 | – | 39 | Iwanek et al. (2018) |
| PWVI | LMC | 1O | 16.10 | 0.03 | −2.38 | 0.03 | −3.10 | 0.21 | 0.15 | 32 | TW |
| PWVI | SMC | 1O | 16.55 | 0.05 | – | – | −3.69 | 0.28 | – | 39 | Iwanek et al. (2018) |
| PWVI | SMC | 1O | 16.38 | 0.02 | – | – | −4.30 | 0.23 | 0.10 | 22 | TW |
| PWVK | theory | F | – | – | −1.71−1.83logM | – | −2.93 | – | 0.04 | – | Marconi et al. (2004) |
| PWVK | LMC | F | 16.58 | 0.02 | – | – | −3.58 | 0.15 | 0.10 | 32 | Ripepi et al. (2014) |
| PWVK | LMC | F | 16.54 | 0.02 | −1.94 | 0.04 | −3.17 | 0.12 | 0.14 | 75 | TW |
| PWVK | LMC | 1O | 15.93 | 0.07 | – | – | −4.14 | 0.33 | 0.10 | 10 | Ripepi et al. (2014) |
| PWVK | LMC | 1O | 15.99 | 0.03 | −2.49 | 0.04 | −3.42 | 0.20 | 0.14 | 33 | TW |
Notes. The different columns report (1) the type of relationship and the band of interest; (2) the galaxy or the theory where the relation was tested; (3) the pulsating mode; (4)–(5) the α coefficient (relative intercept) and relative uncertainty; (6)–(7) the α0 coefficient (absolute intercept) and relative uncertainty; (8)–(9) the β coefficient (slope) and relative uncertainty; (10) the root mean square (RMS) of the relation; (11) the number of stars used in the fit; (12) the authors. The term “TW” (gray shading) refers to “this work”.
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