Table 11: Order 0. Cepheid average angular diameters and distances derived from the VINCI interferometric measurements, assuming a constant diameter model ( $\Delta D=0$ ), The average diameter $\overline {D}$ is taken from Gieren et al. (1998). Two error bars are given in brackets for the angular diameter: the statistical dispersion and the calibration systematics. The uncertainty mentioned for the distance d is the quadratic sum of the statistical, calibration and P-R a priori diameter errors, the last two being systematic in nature. The three types of errors are also reported separately in brackets. The results for $\ell$ Car are mentioned only for completeness, but are not meant to be used for further analysis, as our observations are inconsistent with a constant diameter model.
Star $\overline{\theta_{\rm LD 0}}$ (mas) d₀ (pc) $\chi^2_0$

X Sgr $1.471 \pm 0.033_{[0.013\ 0.031]}$ $324 \pm 18_{[3\ 7\ 17]}$ 0.38

$\eta$ Aql $1.856 \pm 0.028_{[0.009\ 0.026]}$ $261 \pm 14_{[1\ 4\ 14]}$ 3.98

W Sgr $1.348 \pm 0029_{[0.011\ 0.027]}$ $376 \pm 22_{[3\ 8\ 21]}$ 0.90

$\beta$ Dor $1.926 \pm 0.024_{[0.014\ 0.020]}$ $319 \pm 20_{[3\ 2\ 19]}$ 1.31

$\zeta$ Gem $1.747 \pm 0.061_{[0.025\ 0.056]}$ $360 \pm 25_{[5\ 12\ 22]}$ 0.51

Y Oph $1.459 \pm 0.040_{[0.023\ 0.033]}$ $638 \pm 50_{[10\ 14\ 47]}$ 0.16

( $\ell$ Car) $3.071 \pm 0.012_{[0.004\ 0.011]}$ $524 \pm 49_{[1\ 2\ 49]}$ 23.2

**Table 11:** **Order 0.** Cepheid average angular diameters and distances derived from the VINCI interferometric measurements, assuming a constant diameter model ( $\Delta D=0$ ), The average diameter $\overline {D}$ is taken from Gieren et al. (1998). Two error bars are given in brackets for the angular diameter: the statistical dispersion and the calibration systematics. The uncertainty mentioned for the distance d is the quadratic sum of the statistical, calibration and P-R a priori diameter errors, the last two being systematic in nature. The three types of errors are also reported separately in brackets. The results for $\ell$ Car are mentioned only for completeness, but are not meant to be used for further analysis, as our observations are inconsistent with a constant diameter model.
Star	$\overline{\theta_{\rm LD 0}}$ (mas)	d₀ (pc)	$\chi^2_0$
X Sgr	$1.471 \pm 0.033_{[0.013\ 0.031]}$	$324 \pm 18_{[3\ 7\ 17]}$	0.38
$\eta$ Aql	$1.856 \pm 0.028_{[0.009\ 0.026]}$	$261 \pm 14_{[1\ 4\ 14]}$	3.98
W Sgr	$1.348 \pm 0029_{[0.011\ 0.027]}$	$376 \pm 22_{[3\ 8\ 21]}$	0.90
$\beta$ Dor	$1.926 \pm 0.024_{[0.014\ 0.020]}$	$319 \pm 20_{[3\ 2\ 19]}$	1.31
$\zeta$ Gem	$1.747 \pm 0.061_{[0.025\ 0.056]}$	$360 \pm 25_{[5\ 12\ 22]}$	0.51
Y Oph	$1.459 \pm 0.040_{[0.023\ 0.033]}$	$638 \pm 50_{[10\ 14\ 47]}$	0.16
( $\ell$ Car)	$3.071 \pm 0.012_{[0.004\ 0.011]}$	$524 \pm 49_{[1\ 2\ 49]}$	23.2

Source LaTeX | All tables | In the text