All Figures

	Figure 1: Layout of the three baselines used for the VINCI/VLTI Cepheids observations, UT1-UT3 (102.5 m), E0-G1 (66 m) and B3-M0 (140 m).
Open with DEXTER


In the text

	Figure 2: Average wavelets power spectral density of 302 interferograms obtained on X Sgr on . No background or bias is present. The integration of the fringes modulated power is done between 2000 and 8000 cm-1.
Open with DEXTER


In the text

Figure 3: Squared visibilities obtained on  Car on (dashed line) and 2 452 763.555 (solid line), respectively at pulsation phases 0.722 and 0.308. The two UD visibility models correspond to and 3.075 mas, and take the bandwidth smearing effect into account. The first minimum of the visibility function (that never goes down to zero) occurs for baselines of approximately 199 and 181 m, for an effective wavelength of m.

Open with DEXTER


In the text

	Figure 4: Average intensity profiles computed from the four-parameter approximations of Claret (2000) for X Sgr (thin line) and  Car (thick line), using the parameters listed in Table 1.
Open with DEXTER


In the text

	Figure 5: Order 0 model fit for X Sgr.
Open with DEXTER


In the text

	Figure 6: Order 2 model fit for  Aql. The superimposed angular diameter variation curve (thin line) is derived from the integration of the radial velocity curve.
Open with DEXTER


In the text

	Figure 7: Order 2 model fit for W Sgr.
Open with DEXTER


In the text

	Figure 8: Order 2 model fit for  Dor.
Open with DEXTER


In the text

	Figure 9: Order 0 model fit for  Gem. The crosses represent the FLUOR/IOTA data, and the two points are UT1-UT3 observations with VINCI.
Open with DEXTER


In the text

	Figure 10: Order 1 model fit for Y Oph.
Open with DEXTER


In the text

	Figure 11: Order 2 model fit for  Car.
Open with DEXTER


In the text

	Figure 12: Detail of Fig. 11 showing the angular diameter curve of  Car around the maximum diameter.
Open with DEXTER


In the text