Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=18cm,clip]{0954fig1.eps} \end{figure}$ Figure 1: The environment of DENIS-P J185950.9-370632 in the CrA molecular cloud complex. The cross marks the position of the DENIS objects on this DSS1/STSci J plate. The field of view is $50\hbox {$^\prime $ }\times 35\hbox {$^\prime $ }$ . North is up and East is left.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{0954fig2.eps} \end{figure}$ Figure 2: Finding charts of DENIS-P J185950.9-370632 in the I and J filters (DENIS images). The field of view is $3.5\hbox {$^\prime $ }\times 3.5\hbox {$^\prime $ }$ , North is up and East is left.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{0954fig3.eps} \end{figure}$ Figure 3: HST-WFPC2/PC image obtained in the F675W and F814W filters (composite image) on 2000 September 12th. The over-plotted circles represent the position of DENIS-P J185950.9-370632 at different epochs and with different instruments. The radius of each circle corresponds to the uncertainty of that measurement. Although the different measurements are not fully consistent, no source other than DENIS-P J185950.9-370632 can be associated in the image.
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,clip]{0954fig4.eps} \end{figure}$ Figure 4: Contour plots of the ACS/HRC ( F625W) and WFPC2/PC ( F814W) images. The WFPC2/PC and ACS/HRC image have identical scales for easier comparison. The object is clearly elongated on both images, but is better resolved on the higher resolution and better sampled ACS image.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{0954fig5.eps} \end{figure}$ Figure 5: Surface plots showing the results of the non-linear PSF fitting on the ACS/HRC ( F625W filter) and WFPC2/PC ( F814W) images. Amplitudes are normalised. The sky background has been subtracted. The figure shows the images obtained with HST/HRC and WFPC2/PC, one of the PSF stars, the companion appearing after PSF subtraction, and the residuals after subtracting the modelled binary system. The pixel scale of the ACS/HRC is almost two times finer than that of the WFPC2/PC.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0954fig6.eps} \end{figure}$ Figure 6: Comparison of DENIS-P J185950.9-370632 FORS2 spectrum (smoothed via a boxcar with a width of 5 pixels) with the spectrum of the Upper Scorpius member M 8 dwarf DENIS-P J161916.5-234722.9 artificially reddened with $A_{\rm V}=0.5$ mag. The match is very good. The inset box shows a zoom of DENIS-P J185950.9-370632 spectrum around the Li I absorption. Spectrum of DENIS-P J161916.5-234722.9 from Martín et al. (2004). Fluxes have been normalized at the pseudocontinuum level at 840.0 nm.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0954fig7.eps} \end{figure}$ Figure 7: Comparison of DENIS-P J185950.9-370632 FORS2 spectrum (smoothed via a boxcar with a width of 5 pixels) with the spectrum of the field M 8 dwarf VB 10, artificially reddened with $A_{\rm V}=0.5$ mag. The match is very good. The inset boxes show zooms of the two spectra around the K I and Na I doublet. It shows clearly that these two doublets are stronger in VB 10, as expected because of its higher gravity. Spectrum of VB 10 from Martín et al. (1999). Fluxes have been normalized at the pseudocontinuum level at 840.0 nm.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{0954fig8.eps} \end{figure}$ Figure 8: Extinction map of the R-CrA Region around DENIS-P J185950.9-370632 (indicated by white cross). Isocontours of $A_{\rm V}=0.0$ , 1.0, 2.0, 3.0 and 4.0 mag indicate the scale.
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In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{0954fig9.eps} \end{figure}$ Figure 9: HIRES spectra of DENIS 1859-37 (solid line) and Gl 406 (dotted line) in the H $_\alpha$ region. Gl 406 is a typical chromospherically active M 6 dwarf. DENIS 1859-37 has a much broader and asymmetric emission line, indicating that it is probably an accretor.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0954fig10.eps} \end{figure}$ Figure 10: STIS and FORS2 spectra compared with models. Top panel: STIS spectrum of DENIS-P J185950.9-370632 compared with a synthetic spectrum. Bottom panel: FORS2 spectrum of DENIS-P J185950.9-370632 compared with a synthetic spectrum. The best fit is obtained for the same surface gravity (log g=3.5) but slightly different effective temperatures (2600 K and 2700 K). The two results therefore agree within the 100 K temperature step of the model atmosphere grid.
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In the text

$\begin{figure} \par\includegraphics[width=14.2cm,clip]{0954fig11.eps} \end{figure}$ Figure 11: Spectral energy distribution of DENIS-P J185950.9-370632 compared with DUSTY and NextGen models (5 Myr) and field late M-dwarfs distributions: LHS 3003 (M 7), LHS 292 (M 6.5), and LHS 2924 (M 9). The values for DENIS-P J185950.9-370632 have been corrected for an extinction of $A_{\rm V}=0.5$ mag. All fluxes have been normalized to their integrated luminosity between 0 and 1.65 $\mu$ m. (values for the field dwarfs from Leggett 1992; Leggett et al. 2002).
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{0954fig1.eps} \end{figure}$	Figure 1: The environment of DENIS-P J185950.9-370632 in the CrA molecular cloud complex. The cross marks the position of the DENIS objects on this DSS1/STSci J plate. The field of view is $50\hbox {$^\prime $ }\times 35\hbox {$^\prime $ }$ . North is up and East is left.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{0954fig2.eps} \end{figure}$	Figure 2: Finding charts of DENIS-P J185950.9-370632 in the I and J filters (DENIS images). The field of view is $3.5\hbox {$^\prime $ }\times 3.5\hbox {$^\prime $ }$ , North is up and East is left.
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$\begin{figure} \par\includegraphics[width=14.5cm,clip]{0954fig4.eps} \end{figure}$	Figure 4: Contour plots of the ACS/HRC ( F625W) and WFPC2/PC ( F814W) images. The WFPC2/PC and ACS/HRC image have identical scales for easier comparison. The object is clearly elongated on both images, but is better resolved on the higher resolution and better sampled ACS image.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{0954fig8.eps} \end{figure}$	Figure 8: Extinction map of the R-CrA Region around DENIS-P J185950.9-370632 (indicated by white cross). Isocontours of $A_{\rm V}=0.0$ , 1.0, 2.0, 3.0 and 4.0 mag indicate the scale.
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$\begin{figure} \par\includegraphics[width=10cm,clip]{0954fig9.eps} \end{figure}$	Figure 9: HIRES spectra of DENIS 1859-37 (solid line) and Gl 406 (dotted line) in the H $_\alpha$ region. Gl 406 is a typical chromospherically active M 6 dwarf. DENIS 1859-37 has a much broader and asymmetric emission line, indicating that it is probably an accretor.
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