Table 1: Relevant parameters of the observed sample of Cepheids, sorted by increasing period.
  X Sgr $\eta $ Aql W Sgr $\beta $ Dor $\zeta $ Gem Y Oph $\ell $ Car
  HD 161592 HD 187929 HD 164975 HD 37350 HD 52973 HD 162714 HD 84810
mVa 4.581 3.942 4.700 3.731 3.928 6.164 3.771
mKb 2.56 1.966 2.82 1.959 2.11 2.682 1.091
Sp. Type F5-G2II F6Ib-G4Ib F4-G2Ib F4-G4Ia-II F7Ib-G3Ib F8Ib-G3Ib F6Ib-K0Ib
$\pi$ (mas)c $3.03 \pm 0.94$ $2.78 \pm 0.91$ $1.57 \pm 0.93$ $3.14 \pm 0.59$ $2.79 \pm 0.81$ $1.14 \pm 0.80$ $2.16 \pm 0.47$
Min $ T_{{\rm eff}}$ (K) 5670 5400 5355 5025 5150    
Mean $ T_{{\rm eff}}$ (K)d 6150 5870 5769 5490 5430 5300 5090
Max $ T_{{\rm eff}}$ (K) 6820 6540 6324 6090 5750    
Min $\log g$ 1.86 1.25 1.72 1.60      
Mean $\log g^{e}$ 2.14 1.49 1.82 1.83 1.50 1.50 1.50
Max $\log g$ 2.43 1.73 2.02 2.06      
$[{\rm M}/{\rm H}]^{e}$ 0.04 0.05 -0.01 -0.01 0.04 0.05 0.30
T0 (JD- $2.452\times10^6$)f 723.9488 519.2477 726.8098 214.2153 210.7407 715.4809 290.4158
P (days)g 7.013059 7.176769 7.594904 9.842425 10.150967 17.126908 35.551341
Intensity profilesh              
a1 +0.7594 +0.8816 +0.8002 +0.7969 +0.8713 +0.8549 +0.8500
a2 -0.4530 -0.7418 -0.5135 -0.4596 -0.6536 -0.5602 -0.4991
a3 +0.0347 +0.3984 +0.1583 +0.1341 +0.3283 +0.2565 +0.2113
a4 +0.0751 -0.0778 +0.0109 +0.0082 -0.0610 -0.0437 -0.0340
a
mV from Barnes et al. (1987) for X Sgr, from Barnes et al. (1997) for $\eta $ Aql, from Moffett & Barnes (1984) for W Sgr and $\zeta $ Gem, from Berdnikov & Turner (2001) for $\beta $ Dor and $\ell $ Car, and from Coulson & Caldwell (1985) for Y Oph.
b
mK from Welch et al. (1984) for X Sgr, and W Sgr, from Laney & Stobie (1992) for $\beta $ Dor, Y Oph, and $\ell $ Car, from Ducati et al. (2001) for $\zeta $ Gem, from Barnes et al. (1997) for $\eta $ Aql.
c
Parallaxes from the HIPPARCOS catalogue (Perryman et al. 1997).
d
From Kiss & Szatmàry (1998) for $\zeta $ Gem and $\eta $ Aql, Bersier et al. (1997) for W Sgr, and Pel (1978) for X Sgr and $\beta $ Dor.
e
From Andrievsky et al. (2002), Cayrel de Strobel et al. (1997, 2001), and Pel (1978), except for $\log g$ of Y Oph.
f
Reference epoch T0 values have been computed near the dates of the VINCI observations, from the values published by Szabados (1989a).
g
P values from Szabados (1989a). The periods of $\eta $ Aql, $\zeta $ Gem and W Sgr are known to evolve. The values above correspond to the T0 chosen for these stars.
h
Four-parameters intensity profiles from Claret (2000) in the K band, assuming a microturbulence velocity of 4 km s-1 and the average values of $ T_{{\rm eff}}$ and $\log g$.


Source LaTeX | All tables | In the text