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Table 2

Properties of the Cepheids in the dataset.

Star log P Spectrograph
[mag] [mag] F H N S U
RT Aur 0.571489 0.059 0.079 ⋯ 3 ⋯ 3 89
AD Gem 0.578408 0.173 0.382 ⋯ ⋯ ⋯ ⋯ 1
BF Oph 0.609329 0.235 0.223 ⋯ 2 ⋯ 3 5
T Vul 0.646934 0.060 0.052 ⋯ 3 ⋯ 26 ⋯
FF Aql 0.65039 0.196 0.188 ⋯ ⋯ ⋯ 27 ⋯
δ Cep 0.729678 0.075 0.073 ⋯ ⋯ 104 18 ⋯
BB Sgr 0.821971 0.281 0.302 ⋯ 2 ⋯ 3 5
U Sgr 0.828997 0.402 0.408 ⋯ 2 ⋯ 3 60
W Sgr 0.880529 0.108 0.450 ⋯ 3 ⋯ ⋯ ⋯
S Sge 0.923352 0.099 0.084 ⋯ ⋯ ⋯ 19 ⋯
β Dor 0.993131 0.051 0.042 1 46 ⋯ ⋯ 78
ζ Gem 1.006497 0.014 0.003 ⋯ 47 ⋯ 3 85
Z Sct 1.110645 0.492 0.450 ⋯ ⋯ ⋯ ⋯ 9
TT Aql 1.138459 0.435 0.417 ⋯ 2 ⋯ 3 50
Y Oph 1.233609 0.647 0.450 ⋯ 7 ⋯ ⋯ ⋯
RU Sct 1.29448 0.911 0.924 ⋯ ⋯ ⋯ 2 43
RY Sco 1.307927 0.718 0.746 ⋯ 3 ⋯ 3 9
RZ Vel 1.309564 0.300 0.294 ⋯ 7 ⋯ ⋯ 48
WZ Sgr 1.339443 0.435 0.450 ⋯ 1 ⋯ 3 9
VZ Pup 1.364945 0.455 0.450 ⋯ ⋯ ⋯ 1 60
T Mon 1.431915 0.179 0.165 ⋯ 10 ⋯ 3 55
lCar 1.550816 0.146 0.138 ⋯ 111 ⋯ ⋯ 80
U Car 1.58897 0.263 0.260 ⋯ 6 ⋯ ⋯ 50
RS Pup 1.61742 0.457 0.454 ⋯ 19 ⋯ 3 54
HV 6093 0.679881 0.081 ⋯ ⋯ ⋯ ⋯ ⋯ 4
HV 2405 0.840333 0.114 ⋯ ⋯ ⋯ ⋯ ⋯ 2
HV 12452 0.941454 0.175 ⋯ ⋯ ⋯ ⋯ ⋯ 2
HV 1335 1.157800 0.093 ⋯ ⋯ ⋯ ⋯ ⋯ 3
HV 1328 1.199692 0.058 ⋯ ⋯ ⋯ ⋯ ⋯ 3
HV 1333 1.212084 0.100 ⋯ ⋯ ⋯ ⋯ ⋯ 3
HV 822 1.223807 0.086 ⋯ ⋯ ⋯ ⋯ ⋯ 3
HV 1023 1.424235 0.121 ⋯ ⋯ ⋯ ⋯ ⋯ 2
HV 879 1.566167 0.146 ⋯ ⋯ ⋯ ⋯ ⋯ 2
HV 837 1.630509 0.076 ⋯ ⋯ ⋯ ⋯ ⋯ 2
HV 877 1.655215 0.128 ⋯ ⋯ ⋯ ⋯ ⋯ 2
HV 2369 1.684646 0.142 ⋯ ⋯ ⋯ ⋯ ⋯ 2
HV 2827 1.896354 0.12 ⋯ ⋯ ⋯ ⋯ ⋯ 2

Notes. Columns are: logarithm of the pulsation period (P), E(B − V) from Storm et al. (2011a) used for the IRSB analysis, E(B − V) tabulated by Laney & Caldwell (2007). The table also details the spectroscopic data available for these stars (F: FEROS, H: HARPS, N: HARPS-N, S: STELLA, U:UVES). The upper panel lists Galactic Cepheids, the lower panel Magellanic Cepheids. SMC stars (identified in italics) have not been used for training or testing, but only for assessing that the current relations do not hold anymore at the metallicities of SMC Cepheids (see Sect. 5.1).

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