Table 5
Distances for Cepheids with HST parallax measurements from Benedict et al. (2007).
| (1) | (2) | (3) | (4) | (5) | (6) |
| ID | log (P) | d(HST) | d(IRSB) | Δd | σ(Δd) |
| (pc) | (pc) | (pc) | (pc) | ||
|
|
|||||
| FF Aql | 0.650390 | 355.9 | 369.8 | 14.0 | 42.3 |
| RT Aur | 0.571489 | 416.7 | 389.0 | −27.6 | 33.0 |
| ℓ Car | 1.550820 | 497.5 | 517.6 | 20.1 | 47.9 |
| δ Cep | 0.729678 | 273.2 | 266.7 | −6.5 | 20.3 |
| β Dor | 0.993131 | 318.5 | 326.6 | 8.1 | 22.0 |
| ζ Gem | 1.006500 | 359.7 | 385.5 | 25.8 | 38.3 |
| W Sgr | 0.880529 | 438.6 | 216.8 | −221.8 | 71.1 |
| X Sgr | 0.845893 | 333.3 | 322.1 | −11.2 | 28.1 |
| Y Sgr | 0.761428 | 469.5 | 436.5 | −33.0 | 75.6 |
| T Vul | 0.646934 | 526.3 | 542.0 | 15.7 | 59.4 |
Notes. The HST distances are given in Col. 3, the IRSB distances using our preferred p-factor relation from Eq. (7) are given in Col. 4 and the difference in Col. 5. The uncertainty on the difference is given in the last column. † Not considered in the fits. This star is a known spectroscopic binary.
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