Table 10.
Information used for determining the Galactic LL using cluster Cepheids.
| Name | Period | ϖ | σstat | σcov | σtotal | WG |
 |
[Fe/H] | Reference | E(B − V) |
|---|---|---|---|---|---|---|---|---|---|---|
| (d) | (μas) | (μas) | (μas) | (μas) | (mag) | (mag) | (mag) | |||
| CE Cas A | 5.141 | 322.5 | 3.1 | 6.7 | 7.4 | 7.628 ± 0.073 | ||||
| CE Cas B | 4.479 | 322.5 | 3.1 | 6.7 | 7.4 | 7.759 ± 0.081 | ||||
| CF Cas | 4.875 | 322.5 | 3.1 | 6.7 | 7.4 | 7.642 ± 0.010 | 7.641 ± 0.030 | 0.02 ± 0.06 | LL11 | 0.556 ± 0.021 |
| CG Cas | 4.366 | 335.7 | 3.0 | 6.7 | 7.3 | 7.687 ± 0.030 | 7.652 ± 0.034 | 0.09 ± 0.06 | LL11 | 0.667 ± 0.009 |
| CM Sct | 3.917 | 442.9 | 2.2 | 6.2 | 6.6 | 7.046 ± 0.014 | 0.15 ± 0.06 | LL11 | 0.775 ± 0.045 | |
| CS Vel | 5.905 | 281.2 | 2.8 | 6.7 | 7.3 | 7.676 ± 0.006 | 7.669 ± 0.029 | 0.12 ± 0.06 | G14 | 0.716 ± 0.027 |
| CV Mon | 5.379 | 585.2 | 6.9 | 6.6 | 9.6 | 6.198 ± 0.006 | 6.205 ± 0.029 | 0.09 ± 0.09 | G14 | 0.705 ± 0.018 |
| DL Cas | 8.001 | 556.6 | 2.2 | 6.5 | 6.9 | 5.597 ± 0.006 | 5.645 ± 0.021 | −0.01 ± 0.08 | L11 | 0.487 ± 0.005 |
| EV Sct( * ) | 3.090 | 504.0 | 2.8 | 6.4 | 7.0 | 6.541 ± 0.010 | 0.09 ± 0.07 | G15 | ||
| GH Lup | 9.276 | 877.8 | 6.1 | 6.4 | 8.8 | 4.448 ± 0.008 | 0.13 ± 0.06 | G14 | 0.328 ± 0.011 | |
| IQ Nor | 8.220 | 543.6 | 7.2 | 6.1 | 9.4 | 5.711 ± 0.016 | 0.22 ± 0.07 | G15 | 0.676 ± 0.044 | |
| NO Cas( * ) | 2.582 | 317.0 | 2.7 | 6.4 | 7.0 | 8.113 ± 0.018 | ||||
| QZ Nor( * ) | 3.786 | 513.4 | 1.4 | 6.5 | 6.6 | 6.379 ± 0.006 | 0.21 ± 0.06 | G15 | 0.289 ± 0.020 | |
| RS Ori | 7.567 | 609.6 | 3.5 | 6.3 | 7.2 | 5.571 ± 0.036 | 5.603 ± 0.030 | 0.11 ± 0.09 | G15 | 0.332 ± 0.010 |
| S Nor | 9.754 | 1073.2 | 3.8 | 6.1 | 7.2 | 3.932 ± 0.014 | 3.940 ± 0.014 | 0.02 ± 0.09 | R08 | 0.182 ± 0.008 |
| ST Tau | 4.034 | 953.0 | 5.6 | 6.0 | 8.3 | 5.608 ± 0.019 | −0.14 ± 0.15 | L07 | 0.328 ± 0.006 | |
| SV Vul | 44.993 | 424.8 | 5.9 | 6.6 | 8.9 | 3.393 ± 0.014 | 3.589 ± 0.035 | 0.05 ± 0.08 | L11 | 0.474 ± 0.024 |
| SX Vel | 9.550 | 497.0 | 4.0 | 6.0 | 7.2 | 5.746 ± 0.019 | −0.18 ± 0.07 | L07 | 0.237 ± 0.014 | |
| TW Nor | 10.786 | 421.2 | 3.7 | 6.6 | 7.6 | 5.653 ± 0.022 | 5.855 ± 0.030 | 0.27 ± 0.10 | G15 | 1.190 ± 0.023 |
| U Sgr | 6.745 | 1554.1 | 2.7 | 5.4 | 6.0 | 3.565 ± 0.028 | 0.08 ± 0.08 | L11 | 0.408 ± 0.007 | |
| V Cen | 5.494 | 1336.5 | 2.2 | 6.1 | 6.5 | 4.293 ± 0.014 | 4.258 ± 0.028 | 0.04 ± 0.09 | R08 | 0.265 ± 0.016 |
| V Lac | 4.982 | 519.7 | 4.7 | 6.6 | 8.1 | 6.304 ± 0.013 | 0.06 ± 0.06 | LL11 | 0.293 ± 0.034 | |
| V0340 Nor | 11.289 | 513.2 | 1.4 | 6.5 | 6.6 | 5.293 ± 0.005 | 5.313 ± 0.029 | 0.07 ± 0.07 | G15 | 0.312 ± 0.050 |
| V0367 Sct | 6.295 | 513.6 | 2.7 | 6.7 | 7.2 | 5.865 ± 0.033 | 6.125 ± 0.054 | 0.05 ± 0.08 | G15 | |
| V0378 Cen( * ) | 6.459 | 517.8 | 3.7 | 6.5 | 7.5 | 5.468 ± 0.002 | 0.08 ± 0.06 | LL11 | 0.374 ± 0.049 | |
| V0379 Cas( * ) | 4.305 | 556.6 | 2.2 | 6.5 | 6.9 | 5.876 ± 0.005 | 0.06 ± 0.08 | L11 | ||
| V0438 Cyg | 11.211 | 561.9 | 3.6 | 6.4 | 7.3 | 5.142 ± 0.021 | 0.33 ± 0.06 | LL11 | ||
| VW Cru | 5.265 | 731.8 | 6.1 | 6.3 | 8.7 | 5.601 ± 0.003 | 0.19 ± 0.06 | LL11 | 0.640 ± 0.046 | |
| WX Pup | 8.933 | 344.7 | 4.6 | 6.5 | 8.0 | 6.323 ± 0.004 | 6.326 ± 0.016 | −0.15 ± 0.15 | G14 | 0.306 ± 0.018 |
| X Cru | 6.220 | 639.2 | 2.5 | 6.0 | 6.5 | 5.677 ± 0.008 | 0.15 ± 0.06 | LL11 | 0.294 ± 0.019 | |
| X Lac( * ) | 5.443 | 519.7 | 4.7 | 6.6 | 8.1 | 5.766 ± 0.004 | 0.08 ± 0.06 | LL11 | ||
| X Pup | 25.972 | 363.4 | 3.7 | 5.1 | 6.4 | 4.089 ± 0.345 | 5.023 ± 0.012 | 0.02 ± 0.08 | G15 | 0.396 ± 0.015 |
| X Vul | 6.320 | 879.5 | 3.2 | 6.0 | 6.8 | 4.727 ± 0.007 | 4.860 ± 0.031 | 0.07 ± 0.08 | L11 | 0.775 ± 0.021 |
| XZ Car | 16.652 | 482.1 | 2.5 | 6.6 | 7.1 | 5.269 ± 0.033 | 5.169 ± 0.010 | 0.19 ± 0.06 | LL11 | 0.372 ± 0.026 |
| Y Sct | 10.341 | 503.4 | 2.8 | 6.4 | 7.0 | 5.121 ± 0.171 | 0.23 ± 0.06 | LL11 | 0.792 ± 0.021 |
Notes. Cluster average parallaxes include the corrections as described by L21. Iron abundances were rescaled by Genovali et al. (2015) to the common solar abundance A(Fe) = 7.50 (Grevesse & Sauval 1998). Color excess values E(B − V) are taken from Fernie et al. (1995) and scaled by a factor 0.94 (cf. Groenewegen 2018). The symbol ( * ) denotes Cepheids pulsating in the first overtone mode. (a): Observations reported in the HST system (WH) are computed using Eq. (5) and the individual passband data from Riess et al. (2022a), that is, they do not contain the CRNL correction needed for comparison with the SN-host Cepheid sample.
References: (LL11): Luck & Lambert (2011), (G14): Genovali et al. (2014), (L11): Luck et al. (2011), (G15): Genovali et al. (2015), (R08): Romaniello et al. (2008), (L07): Lemasle et al. (2007).
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