Table 3.
Final sample adopted, combining Cepheids with resolved companions and open cluster Cepheids.
| Cepheid | P | ϖ ( * ) | E(B − V) | mV | mJ | mH | mKS |  (* * ) |
RefNIR |
|---|---|---|---|---|---|---|---|---|---|
| (days) | (mas) | (mag) | (mag) | (mag) | (mag) | (mag) | |||
| Sample of Cepheids with resolved companions | |||||||||
| DF Cas | 3.832 | 0.367±0.104 | 0.564±0.049 | 10.880±0.030 | 8.488±0.025 | 8.036±0.025 | 7.879±0.025 | 7.533±0.066 | G14 |
| CM Sct | 3.917 | 0.518±0.056 | 0.775±0.045 | 11.100±0.030 | 8.300±0.025 | 7.818±0.025 | 7.558±0.025 | 7.240±0.066 | G14 |
| EV Sct | 4.396 ( ⋆ ) | 0.481±0.040 | 0.623±0.015 | 10.130±0.030 | 7.608±0.008 | 7.184±0.008 | 7.018±0.008 | 6.658±0.061 | L92 |
| TV CMa | 4.670 | 0.426±0.054 | 0.574±0.029 | 10.590±0.030 | 8.022±0.008 | 7.582±0.008 | 7.364±0.008 | 7.048±0.061 | M11 |
| V532 Cyg | 4.675 ( ⋆ ) | 0.619±0.033 | 0.519±0.007 | 9.090±0.030 | 6.863±0.025 | 6.393±0.025 | 6.250±0.025 | 5.919±0.066 | 2MASS |
| V950 Sco | 4.814 ( ⋆ ) | 0.893±0.069 | 0.251±0.019 | 7.310±0.030 | 5.681±0.008 | 5.439±0.008 | 5.295±0.008 | 5.083±0.061 | G18 |
| V350 Sgr | 5.154 | 1.015±0.048 | 0.308±0.008 | 7.470±0.030 | 5.625±0.010 | 5.245±0.010 | 5.121±0.010 | 4.844±0.061 | W84 |
| VW Cru | 5.265 | 0.679±0.034 | 0.640±0.046 | 9.600±0.030 | 6.805±0.025 | 6.261±0.025 | 6.051±0.025 | 5.681±0.066 | G14 |
| AX Cir | 5.273 | 1.725±0.527 | 0.265±0.121 | 5.880±0.030 | 4.299±0.025 | 3.879±0.025 | 3.780±0.025 | 3.524±0.066 | G14 |
| δ Cep | 5.366 | 3.364±0.049 | 0.075±0.018 | 3.950±0.030 | 2.683±0.010 | 2.396±0.010 | 2.294±0.010 | 2.104±0.061 | B97 |
| CV Mon | 5.379 | 0.508±0.040 | 0.705±0.018 | 10.310±0.030 | 7.314±0.008 | 6.781±0.008 | 6.529±0.008 | 6.165±0.061 | M11 |
| QZ Nor | 5.401 ( ⋆ ) | 0.452±0.132 | 0.289±0.020 | 8.870±0.030 | 7.085±0.008 | 6.748±0.008 | 6.614±0.008 | 6.360±0.061 | L92 |
| V659 Cen | 5.622 | 1.355±0.448 | 0.151±0.034 | 6.620±0.030 | 5.177±0.025 | 4.907±0.025 | 4.651±0.025 | 4.583±0.066 | G14 |
| CS Vel | 5.905 | 0.222±0.050 | 0.716±0.027 | 11.700±0.030 | 8.771±0.008 | 8.246±0.008 | 8.011±0.008 | 7.643±0.061 | L92 |
| RS Nor | 6.198 | 0.449±0.043 | 0.577±0.036 | 10.000±0.030 | 7.412±0.010 | 6.794±0.010 | 6.683±0.010 | 6.249±0.061 | SPIPS |
| X Cru | 6.220 | 0.609±0.061 | 0.294±0.019 | 8.400±0.030 | 6.521±0.025 | 6.125±0.025 | 5.935±0.025 | 5.717±0.066 | G14 |
| AW Per | 6.464 | 1.046±0.349 | 0.479±0.016 | 7.480±0.030 | 5.213±0.008 | 4.832±0.008 | 4.657±0.008 | 4.354±0.061 | M11 |
| U Sgr | 6.745 | 1.461±0.038 | 0.408±0.007 | 6.690±0.030 | 4.506±0.008 | 4.100±0.008 | 3.912±0.008 | 3.637±0.061 | M11 |
| ER Car | 7.720 | 0.889±0.210 | 0.111±0.016 | 6.820±0.030 | 5.310±0.008 | 5.034±0.008 | 4.896±0.008 | 4.698±0.061 | G18 |
| SX Vel | 9.550 | 0.432±0.086 | 0.237±0.014 | 8.290±0.030 | 6.500±0.008 | 6.133±0.008 | 5.991±0.008 | 5.743±0.061 | L92 |
| SY Nor | 12.646 | 0.414±0.053 | 0.611±0.059 | 9.500±0.030 | 6.574±0.008 | 6.105±0.008 | 5.865±0.008 | 5.504±0.061 | G18 |
| RS Pup | 41.443 | 0.503±0.045 | 0.451±0.010 | 7.010±0.030 | 4.365±0.008 | 3.828±0.008 | 3.619±0.008 | 3.276±0.061 | L92 |
| Sample of open cluster Cepheids | |||||||||
| CG Cas | 4.365 | 0.282±0.041 | 0.667±0.009 | 11.380±0.030 | 8.903±0.025 | 8.299±0.025 | 8.109±0.025 | 7.775±0.066 | G14 |
| EV Sct | 4.398 ( ⋆ ) | 0.468±0.035 | 0.623±0.015 | 10.130±0.030 | 7.608±0.008 | 7.184±0.008 | 7.018±0.008 | 6.658±0.061 | L92 |
| CF Cas | 4.875 | 0.269±0.041 | 0.556±0.021 | 11.060±0.030 | 8.590±0.008 | 8.126±0.008 | 7.900±0.008 | 7.608±0.061 | M11 |
| CV Mon | 5.379 | 0.523±0.043 | 0.705±0.018 | 10.310±0.030 | 7.314±0.008 | 6.781±0.008 | 6.529±0.008 | 6.165±0.061 | M11 |
| QZ Nor | 5.401 ( ⋆ ) | 0.443±0.036 | 0.289±0.020 | 8.870±0.030 | 7.085±0.008 | 6.748±0.008 | 6.614±0.008 | 6.360±0.061 | L92 |
| V Cen | 5.495 | 1.288±0.023 | 0.265±0.016 | 6.820±0.030 | 5.019±0.008 | 4.642±0.008 | 4.498±0.008 | 4.249±0.061 | L92 |
| CS Vel | 5.905 | 0.221±0.042 | 0.716±0.027 | 11.700±0.030 | 8.771±0.008 | 8.246±0.008 | 8.011±0.008 | 7.643±0.061 | L92 |
| V367 Sct | 6.293 | 0.467±0.041 | 1.145±0.043 | 11.610±0.030 | 7.605±0.008 | 6.955±0.008 | 6.651±0.008 | 6.152±0.061 | L92 |
| U Sgr | 6.745 | 1.514±0.024 | 0.408±0.007 | 6.690±0.030 | 4.506±0.008 | 4.100±0.008 | 3.912±0.008 | 3.636±0.061 | M11 |
| RS Ori | 7.567 | 0.553±0.027 | 0.332±0.010 | 8.410±0.030 | 6.398±0.008 | 6.020±0.008 | 5.860±0.008 | 5.589±0.061 | M11 |
| DL Cas | 8.001 | 0.511±0.031 | 0.487±0.005 | 8.970±0.030 | 6.550±0.008 | 6.101±0.008 | 5.892±0.008 | 5.593±0.061 | M11 |
| S Nor | 9.754 | 1.025±0.027 | 0.182±0.008 | 6.420±0.030 | 4.674±0.008 | 4.288±0.008 | 4.149±0.008 | 3.905±0.061 | L92 |
| TW Nor | 10.786 | 0.383±0.042 | 1.190±0.023 | 11.670±0.030 | 7.442±0.008 | 6.712±0.008 | 6.375±0.008 | 5.865±0.061 | L92 |
| V340 Nor | 11.288 | 0.443±0.036 | 0.312±0.009 | 8.370±0.030 | 6.211±0.008 | 5.745±0.008 | 5.573±0.008 | 5.284±0.061 | L92 |
Notes. Parallaxes in the first part of the table are from GDR2 for the companions; parallaxes in the second part are from Cantat-Gaudin et al. (2018) based on GDR2 with revised uncertainties. Reddenings E(B − V) are taken from the DDO database (Fernie et al. 1995), to which we applied a multiplicative factor of 0.94. Mean apparent magnitudes in V, J, H, KS bands are from the catalog compiled by Groenewegen (2018): V band magnitudes are originally from Mel’nik et al. (2015) and NIR magnitudes are converted in the 2MASS system with the original references provided in the last column. Apparent Wesenheit magnitudes on the WFC3 system (
) are also provided; their uncertainties include the photometric transformation errors. ( ⋆ ) Cepheid pulsating in the first-overtone mode. In this case the period was converted following the approach described in Sect. 2.4. ( * ) The parallaxes presented in this table do not include the parallax zero-point offset term.
apparent magnitudes presented in this table do not include the addition of the CRNL term.
References. (G14) Genovali et al. (2014; L92) Laney & Stobie (1992; M11) Monson & Pierce (2011); (2MASS) Skrutskie et al. (2006; G18) Groenewegen (2018; W84) Welch et al. (1984; B97) Barnes et al. (1997); (SPIPS) Light curve fitting with the SPIPS algorithm (Mérand et al. 2015; Trahin 2019).
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