Table 2: The stellar parameters from Decin et al. (2003b) and references therein, and the limits of the grid in which we searched for an optimal fit to the interferometric data ( $\xi _{\rm {t}}$ is the microturbulent velocity).
Parameter Value Lower limit Upper limit

$T_{\rm eff}$ (K) $4320\pm140$ 4250 4500

$\log g \: ({\rm cm/s}^2)$ $1.50\pm0.15$ 1.00 2.00

$[\rm {Fe/H}]$ $-0.5\pm0.20$ -1.0 0.0

$\xi _{\rm {t}}$ (km s^-1) $1.7\pm0.3$

**Table 2:** The stellar parameters from Decin et al. (2003b) and references therein, and the limits of the grid in which we searched for an optimal fit to the interferometric data ( $\xi _{\rm {t}}$ is the microturbulent velocity).
Parameter	Value	Lower limit	Upper limit
$T_{\rm eff}$ (K)	$4320\pm140$	4250	4500
$\log g \: ({\rm cm/s}^2)$	$1.50\pm0.15$	1.00	2.00
$[\rm {Fe/H}]$	$-0.5\pm0.20$	-1.0	0.0
$\xi _{\rm {t}}$ (km s^-1)	$1.7\pm0.3$

Source LaTeX | All tables | In the text

	1 Introduction
	2 The interferometric calibration process: The need for well-known calibrators
	3 The observations
	4 Interpretation of the data: Comparison with theoretical atmosphere models
	5 The binary hypothesis
	6 Conclusions and outlook
	References