Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{1395Fig_1a.ps}\hspace*{3mm... ...ps}\hspace*{3mm} \includegraphics[width=6.3cm,clip]{1395Fig_1d.ps} \end{figure}$ Figure 1: From left to right and up to down, J, H, Ks, L' images from NACO shown in logarithmic inverted scale. The L' image is slightly overexposed in spite of the smallest possible integration time.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1395Fig_2.eps} \end{figure}$ Figure 2: Color image combining the flux from L' (red) and Br $\alpha$ (green) and Pf $\gamma$ (blue) filters. At these wavelengths, the hydrogen emission represents only a small amount of the flux: about 10% and 2% of flux recorded with the Br $\alpha$ and Pf $\gamma$ filter respectively. The L' filter shows deeper details of the nebula but is saturated in the 0 $\hbox{$.\!\!^{\prime\prime}$ }5\times 0\hbox{$.\!\!^{\prime\prime}$ }$ 5 core. The white bar represents 1 $\hbox {$^{\prime \prime }$ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1395Fig_3.ps} \end{figure}$ Figure 3: Pf $\gamma$ deconvolved image. The resolution achieved is in the order of 60 mas. To enhance the contrast, the image I^1/4 is shown. The color scale is expressed in Jy/arcsec². Taken into account the large error bars of the photometry, this scale is only indicative of the flux.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1395Fig_4.ps} \end{figure}$ Figure 4: Evolution of the L' magnitude based on aperture photometry with increasing radius. The integrated flux within a circle of 3 $\hbox {$^{\prime \prime }$ }$ is $L'=-1.85 \pm 0.2$ .
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{1395Fig_5.eps} \end{figure}$ Figure 5: Zoom into the deconvolved images from the NB_3.74 ( up) and NB_4.05 ( bottom) filters. The raw images are shown in the left side, the deconvolved images at iteration 10 and 40 are shown in the middle and the in the right side. The resulted images from the two filters are fairly similar except for the size of the central source which is 25% larger in Br $\alpha$ due to a slight non-linearity of the detector at high flux regime.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1395Fig_6a.ps}\par\vspace*{3mm} \includegraphics[width=8.8cm,clip]{1395Fig_6b.ps} \end{figure}$ Figure 6: On the top, radial flux normalized to the peak with NB_3.74 filter for Eta Car (dashed line), and the PSF HD 101104 (dotted line) and their subtraction (solid line). Close to the source, a strong decrease of the flux is clearly seen that we attribute to the dust sublimation region at about 0 $\hbox{$.\!\!^{\prime\prime}$ }$ 1 (230 AU). On the bottom panel the same treatment is applied to the NB_4.05 images. However, the flux reference is chosen to be at $\sim$ 0 $\hbox{$.\!\!^{\prime\prime}$ }$ 05 (2 pixels) from the peak in order to account for the non-linearity of the detector at maximum. The dashed-dotted curve is the residual of the NB_3.74 filter subtraction scaled for comparison. The two curves agree fairly well and the contribution of the Br $\alpha$ line is hardly visible.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1395Fig_7.eps} \end{figure}$ Figure 7: Location of interesting regions in the "butterfly'' dusty nebula close to Eta Car. The naming convention is partly based on Fig. 4 of Smith et al. (2003a).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{1395Fig_8a.ps}\hspace*{3mm} \includegraphics[width=6.7cm,clip]{1395Fig_8b.ps} \end{figure}$ Figure 8: Comparison of the 3.74 $\mu$ m deconvolved NACO image (in contours) with the highest resolution HST images (background, from Morse et al. 1999) at large ( left) and small ( right) scales. The location of the dusty clumps does not coincide with that of the Weigelt blobs, but their structure is somehow complementary to the image. The optical/UV blobs are probably hot regions less shielded from the central star's UV flux which could coincide with the dust clump surfaces facing the star. This is particularly true for Weigelt blobs C and D.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1395Fig_9.ps} \end{figure}$ Figure 9: Deconvolved acquisition image of Eta Car with the 8.7 $\mu$ m filter (UT3). In order to enhance the contrast, the image I^1/4 is shown but the color scale is expressed in Jy/arcsec². The bright spot which emerges in this image is in the position of the central star and at the location where a strong correlated flux has been detected by MIDI (see Fig. 12). The image has been de-rotated with respect to Fig. 10 so that the north is up and east is left.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{1395Fig_10.ps} \end{figure}$ Figure 10: MIDI 8.7 $\mu$ m acquisition image. The north points towards the upper-left side and east the lower-left and the position of the slit is indicated. The slit is 0 $\hbox{$.\!\!^{\prime\prime}$ }$ 6 wide and 3 $\hbox {$^{\prime \prime }$ }$ long. The numbers indicate the central positions of the apertures described in Table 4.
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{1395Fig_11.eps} \end{figure}$ Figure 11: Spatially resolved MIDI spectra expressed in Jansky (grey lines) together with the spectra of the best fit models (solid line). The dotted line shows the olivine contribution, the dashed line the corundum contribution and the long-dashed shows the continuum emission. The spectra are extracted from the north-west ( upper left panel) to the south-east ( lower right panel). The slit is aligned to the nebula. The 9 spectra are spaced by 0 $\hbox{$.\!\!^{\prime\prime}$ }$ 4, the maximum flux in the MIR is in aperture 5 while the star is located in aperture 6. The SE clump and the southern arcs spectra are in apertures 7, 8 and 9.
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{1395Fig_12a.ps}\hspace*{3mm} \includegraphics[width=6.4cm,clip]{1395Fig_12b.ps} \end{figure}$ Figure 12: Left, the figure shows the rms of the fluctuations within the MIDI FOV. The external regions are dominated by the detector noise and the internal regions by the tunnel and sky background fluctuations. The signal from the fringes is strong and centered on the position of the star as seen in the deconvolved acquisition image at 8.7 $\mu$ m. The contour plot represents the contours of the deconvolved MIDI 8.7 $\mu$ m acquisition image. Right, the noise pattern and the fringe pattern from a calibrator have been subtracted from the previous figure in order to show the extended fringe signal. The orientation is the same as in Fig. 10.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1395Fig_13.ps} \end{figure}$ Figure 13: MIDI correlated flux measured with a 74 m (PA = 62 $^\circ$ ) and a 78 m (PA = 56 $^\circ$ ) projected baseline. The solid line denotes the photometric flux as extracted using the mask centered on the star (aperture 6) which can be seen in Fig. 11. The dotted lines represent the correlated flux measured with the aperture 6. scale has been multiplied by 10. The dashed and dashed-dotted lines represent the correlated flux extracted with aperture 5 (dashed) and 7 (dashed-dotted).
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{1395Fig_1a.ps}\hspace{3mm... ...ps}\hspace{3mm} \includegraphics[width=6.3cm,clip]{1395Fig_1d.ps} \end{figure}$	Figure 1: From left to right and up to down, J, H, Ks, L' images from NACO shown in logarithmic inverted scale. The L' image is slightly overexposed in spite of the smallest possible integration time.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1395Fig_3.ps} \end{figure}$	Figure 3: Pf $\gamma$ deconvolved image. The resolution achieved is in the order of 60 mas. To enhance the contrast, the image I^1/4 is shown. The color scale is expressed in Jy/arcsec². Taken into account the large error bars of the photometry, this scale is only indicative of the flux.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1395Fig_4.ps} \end{figure}$	Figure 4: Evolution of the L' magnitude based on aperture photometry with increasing radius. The integrated flux within a circle of 3 $\hbox {$^{\prime \prime }$ }$ is $L'=-1.85 \pm 0.2$ .
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1395Fig_7.eps} \end{figure}$	Figure 7: Location of interesting regions in the "butterfly'' dusty nebula close to Eta Car. The naming convention is partly based on Fig. 4 of Smith et al. (2003a).
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$\begin{figure} \par\includegraphics[width=5.8cm,clip]{1395Fig_10.ps} \end{figure}$	Figure 10: MIDI 8.7 $\mu$ m acquisition image. The north points towards the upper-left side and east the lower-left and the position of the slit is indicated. The slit is 0 $\hbox{$.\!\!^{\prime\prime}$ }$ 6 wide and 3 $\hbox {$^{\prime \prime }$ }$ long. The numbers indicate the central positions of the apertures described in Table 4.
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