Astronomy & Astrophysics

All Figures

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi01.eps} } \end{figure}$ Figure 1: Reconstructed image of Mon R2 IRS3 in the K band. A Gaussian window of FWHM = $5.3\ {\rm \:arcsec^{-1}}$ was applied to the visibility to achieve a resolution of 0 $.\!\!^{\prime\prime}$ 19. The contours are at 5, 10, 15, 30 and 50% of the peak. The noise level is $\sim$ 0.4%. The sources are labelled using the notation by Koresko et al. (1993). The arrows indicate faint stars used to align the H and K images. In this and in the following reconstructed images the intensity scale is normalised to the brightest peak with the brighter regions represented by the darker greys.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi02.eps} } \end{figure}$ Figure 2: Reconstructed image of Mon R2 IRS3 in the H band. The resolution is 0 $.\!\!^{\prime\prime}$ 19. The contours are at 5, 10, 15, 30 and 50% of the peak and the noise level is $\sim$ 1%. The labels used are the same as for the K band image. The star symbols indicate the position of the stars IRS3 N and IRS3 S in the K band image. The small arrows indicate the position of the two stars used to align this image and the K band image.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi03.eps} } \end{figure}$ Figure 3: Colour-coded image of Mon R2 IRS3. The emission at H and K are represented by the blue and red colours respectively. The blue colour of the nebulae indicates the scattered nature of the light.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi06.eps} } \end{figure}$ Figure 6: Speckle reconstructed image of GL 437-S in the K band. The resolution attained is 0 $.\!\!^{\prime\prime}$ 22. The colour scale varies from $-1\%$ (white) to 5% (black) of the brightness peak. The contours are at 15%, 20%, 25%, 30% and 50% of the peak, and the noise is at the 4% level.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi10.eps} } \end{figure}$ Figure 10: Reconstructed image of GL 961 at H. A Gaussian window with a FWHM = $3.1\ {\rm \:arcsec^{-1}}$ was applied to the visibility function in order to filter out the noise associated with the high spatial frequencies. The image has a resolution of 0 $.\!\!^{\prime\prime}$ 32. The contour levels are at 1%, 3%, 5%, 10%, 30% and 50% of the brightness peak. The background noise is $\sim$ 0.1%.
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In the text

$\begin{figure} \par {\includegraphics[width=17.6cm,clip]{0438fi11.eps} } \end{figure}$ Figure 11: a) Reconstructed image of S235 IRS1 in the K band taken with MAGIC during the Calar Alto campaign. The resolution achieved is 0 $.\!\!^{\prime\prime}$ 27. In addition to IRS1, which is near the centre of the FOV, two other stars can be seen towards the NW and SW. The contours represent 0.5%, 1%, 1.5%, 2%, 3% and 5% of the peak. The noise level is ${\sim } 0.1\%$ although negative artifacts at a level of $-2.5\%$ (white in the grey-scale) appear close to the brightness (central) peak. b) The same as on panel a) but using the data taken during the campaign at UKIRT. In this case, the negative artifacts are at a $-1\%$ level.
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In the text

$\begin{figure} \par {\includegraphics[width=8.3cm,clip]{0438fi16.eps} } \end{figure}$ Figure 16: Colour-colour diagram for the massive YSOs observed in our speckle campaigns. The filled circles represent the sources in which a sub-arcsecond conical nebula was detected. The open circles represent sources in which no clear extended emission associated with the outflow was detected. Note that our typical detection limit is at 1% of the brightness peak. The main sequence is plotted as a grey line. The dashed lines indicate the extincted main sequence using the extinction law of He et al. (1995). The arrow represents a visual extinction of 10 mag.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi04.eps} } \end{figure}$ Figure 4: Speckle reconstructed image of S140 IRS1 in the K band at a resolution of 0 $.\!\!^{\prime\prime}$ 19. The contour levels are at 1%, 2.5%, 4%, 5.5%, 7%, 8.5% and 50% of the peak. The noise level is <1%. The grey-scale varies from $-2\%$ (white) to 8% (black).
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi05.eps} } \end{figure}$ Figure 5: Speckle reconstructed image of S255 IRS1 in the K band at a resolution of 0 $.\!\!^{\prime\prime}$ 29. The contour levels are at 0.5%, 1%, 1.5% and 2% of the peak. The noise level is <1%. The grey-scale varies from $-1\%$ (white) to 4% (black). The negative feature (-3.5%) west of IRS1 is a "ghost'' of IRS3.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi07.eps} } \end{figure}$ Figure 7: Reconstructed image of LkH $\alpha$ 101 in the J band with a resolution of 0 $.\!\!^{\prime\prime}$ 11. A Gaussian window of FWHM = $9.1\ {\rm \:arcsec^{-1}}$ was applied to the visibility to reduce the noise associated with the high spatial frequencies. The faint component is located 0 $.\!\!^{\prime\prime}$ 17 away ( ${\sim} 130$ AU at a distance of 800 pc) and it is $\sim$ 5 times fainter than the primary. The background noise is $\la$ 1% of the peak.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi08.eps} } \end{figure}$ Figure 8: H band speckle reconstructed image of GL 490 from data taken at Calar Alto in 1994 The resolution is 0 $.\!\!^{\prime\prime}$ 23. The grey-scale varies between $-2.5\%$ (white) and 9.4% (black) of the peak. The contours are at 1.5, 3, 4.0 and 50% of the peak. The noise level is $0.2\%$ away from the source.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi09.eps} } \end{figure}$ Figure 9: H band speckle image of GL 490 taken at UKIRT in 1997. The resolution achieved was 0 $.\!\!^{\prime\prime}$ 18. The visibility was multiplied by a Gaussian window with a FWHM of $5.5\ {\rm \:arcsec^{-1}}$ . The grey-scale varies from $-1\%$ to 3%. The contours are at 1.5, 3, 4.5 and 30% of the peak. The most negative feature is at a $-1.5\%$ level. The noise is $\sim$ 0.2% away from the source.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi12.eps} } \end{figure}$ Figure 12: Speckle reconstructed image of GL 2591 IRS1 in the K band at a resolution of 0 $.\!\!^{\prime\prime}$ 21. There appears to be a faint extension to the west, at a distance of $0\hbox{$.\!\!^{\prime\prime}$ }6 \pm 0\hbox{$.\!\!^{\prime\prime}$ }1$ from the brightness peak. The contour levels are at 1.5%, 2%, 5%, 30% and 50% of the peak. The noise level is <1% but the negative artifacts (white in the grey-scale) seen to the E of the brightness peak are at a $-1.7\%$ level.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi13.eps} } \end{figure}$ Figure 13: Speckle reconstructed image of GL 4029 IRS1 in the K band at a resolution of 0 $.\!\!^{\prime\prime}$ 19. The contour levels are at 1%, 5%, 10% and 50% of the peak. The noise level is $\protect\la$ 1%. The grey-scale varies from $-0.8\%$ (white) to 2% (black).
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi14.eps} } \end{figure}$ Figure 14: Speckle reconstructed image of NGC 7538 IRS1 in the K band at a resolution of $0\hbox{$.\!\!^{\prime\prime}$ }33$ . The contour levels are at 0.3%, 0.5%, 1%, 2%, 25% and 50% of the peak. The noise level is ${\sim } 0.2\%$ . The grey-scale varies from $-0.1\%$ (white) to 1% (black). In this case, the full FOV of MAGIC was used, and therefore the field of view is $17\hbox{$.\!\!^{\prime\prime}$ }9 \times 17\hbox{$.\!\!^{\prime\prime}$ }9$ . The two parallel horizontal stripes that cross the image at the positions of IRS1 and IRS2 are artifacts from the reconstruction.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi15.eps} } \end{figure}$ Figure 15: Speckle reconstructed image of GL 5180 IRS1 in the K band at a resolution of 0 $.\!\!^{\prime\prime}$ 07. The noise level is $\sim$ 0.5% although near IRS1 there are noise features with a value of $-15\%$ . The grey-scale varies from $-1\%$ (white) to 8% (black). In this case the full array was used, and therefore the field of view is $18'' \times 18''$ . The image shows several artifacts produced during the reconstruction. These appear on the row through IRS1 and as positive and negative artifacts of the binary images.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi03.eps} } \end{figure}$	Figure 3: Colour-coded image of Mon R2 IRS3. The emission at H and K are represented by the blue and red colours respectively. The blue colour of the nebulae indicates the scattered nature of the light.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi06.eps} } \end{figure}$	Figure 6: Speckle reconstructed image of GL 437-S in the K band. The resolution attained is 0 $.\!\!^{\prime\prime}$ 22. The colour scale varies from $-1\%$ (white) to 5% (black) of the brightness peak. The contours are at 15%, 20%, 25%, 30% and 50% of the peak, and the noise is at the 4% level.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi04.eps} } \end{figure}$	Figure 4: Speckle reconstructed image of S140 IRS1 in the K band at a resolution of 0 $.\!\!^{\prime\prime}$ 19. The contour levels are at 1%, 2.5%, 4%, 5.5%, 7%, 8.5% and 50% of the peak. The noise level is <1%. The grey-scale varies from $-2\%$ (white) to 8% (black).
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi05.eps} } \end{figure}$	Figure 5: Speckle reconstructed image of S255 IRS1 in the K band at a resolution of 0 $.\!\!^{\prime\prime}$ 29. The contour levels are at 0.5%, 1%, 1.5% and 2% of the peak. The noise level is <1%. The grey-scale varies from $-1\%$ (white) to 4% (black). The negative feature (-3.5%) west of IRS1 is a "ghost'' of IRS3.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi08.eps} } \end{figure}$	Figure 8: H band speckle reconstructed image of GL 490 from data taken at Calar Alto in 1994 The resolution is 0 $.\!\!^{\prime\prime}$ 23. The grey-scale varies between $-2.5\%$ (white) and 9.4% (black) of the peak. The contours are at 1.5, 3, 4.0 and 50% of the peak. The noise level is $0.2\%$ away from the source.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0438fi13.eps} } \end{figure}$	Figure 13: Speckle reconstructed image of GL 4029 IRS1 in the K band at a resolution of 0 $.\!\!^{\prime\prime}$ 19. The contour levels are at 1%, 5%, 10% and 50% of the peak. The noise level is $\protect\la$ 1%. The grey-scale varies from $-0.8\%$ (white) to 2% (black).
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