All Figures

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{figure1.ps}} \end{figure}$ Figure 1: Diffraction-limited 2.29 $\mu$ m image of the core of the $\eta$ Carinae nebula, taken with the adaptive optics camera NAOS-CONICA at the VLT. The position of the Weigelt Blobs is indicated.
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{figure2_AnA.ps}} \end{figure}$ Figure 2: Upper panel: observed visibility as a function of projected baseline. The full line is the best fit LTE wind model to the VLTI observations. The dashed line is the best fit non-LTE radiative transfer model to the observed visibilities. Lower panel: variation of FWHM fitted to the visibility of $\eta$ Carinae measured with VINCI at the VLTI as a function of projected orientation of the 24 m baseline. The solid line gives the best fit to the measurements, assuming a 2D Gaussian shape of the source at each projected baseline orientation. The amplitude of the size variations gives a ratio of major to minor axis of $1.25\pm 0.05$ . The major axis has a position angle of $134\pm 7$ deg east of north.
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{figure3_AnA.ps}} \end{figure}$ Figure 3: Allowed ranges in mass loss rate and wind clumping factor for the LTE wind model (contours) and the full non-LTE radiative transfer model applied to the Hubble Space Telescope spectra (Hillier et al. 2001) (dashed line). Both data sets agree for a mass loss rate of $1.6\times10^{-3}~M_{\odot}$ /yr and a wind clumping factor of 0.26.
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{figure1.ps}} \end{figure}$	Figure 1: Diffraction-limited 2.29 $\mu$ m image of the core of the $\eta$ Carinae nebula, taken with the adaptive optics camera NAOS-CONICA at the VLT. The position of the Weigelt Blobs is indicated.
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$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{figure3_AnA.ps}} \end{figure}$	Figure 3: Allowed ranges in mass loss rate and wind clumping factor for the LTE wind model (contours) and the full non-LTE radiative transfer model applied to the Hubble Space Telescope spectra (Hillier et al. 2001) (dashed line). Both data sets agree for a mass loss rate of $1.6\times10^{-3}~M_{\odot}$ /yr and a wind clumping factor of 0.26.
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