All Figures

$\begin{figure} \par\includegraphics[width=7cm,height=7cm,clip]{Gj061_f1.ps}\end{figure}$ Figure 1: VLT-NACO $K_{\rm s}$ -band image of GQ Lup and its 6 mag fainter companion candidate $0.7325 \pm 0.0034^{\prime \prime }$ west.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Gj061_f2.eps}\end{figure}$ Figure 2: Observed separation between primary star GQ Lup A and companion candidate with HST/PC ( left), Subaru/CIAO ( middle) and VLT/NACO ( right, first the June 2004 image, then the Aug. and Sep. 2004 aquisition images, all consistent within $1\sigma$ ) compared to the expectation when bound (no change in separation as straight full line $\pm$ 5 mas/yr for orbital motion as straight dotted lines) or when background (motion of GQ Lup A alone to the SW due to its proper motion $\pm$ its error with wobble due to expected parallactic motion of 7.1 mas). We can reject the background hypothesis by 4.9 $\sigma$ (NACO-CIAO) plus 7.2 $\sigma$ (NACO-HST).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,height=7.4cm,clip]{Gj061_f3.ps}\end{figure}$ Figure 3: Our flux-calibrated K-band NACO spectrum of the companion of GQ Lup ( bottom) compared to the young M8 brown dwarfs in Cha I ( top) from Comerón et al. (2000), L2 (2MASSW J0829066+145622, 2nd from top) from Reid et al. (2001), and a GAIA-Dusty template spectrum for 2000 K and $\log~g=2$ , which compares well with the companion.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,height=7.5cm,clip]{Gj061_f4.ps}\end{figure}$ Figure 4: H-R diagram with tracks from Wuchterl & Tscharnuter (2003) plus more tracks calculated by us ( from top to bottom) for 1 and $0.7~M_{\odot}$ as well as 13, 5, 2, 1, and 0.5 $M_{\rm jup}$ . The isochrones (dashed) for 1.10 and 1.65 Myr connect the end of the $0.7~M_{\odot}$ track (star A) with the planetary tracks. Components A and B (1 $\sigma$ errors) are co-eval at $\sim$ 1.1 Ma.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,height=7cm,clip]{Gj061_f1.ps}\end{figure}$	Figure 1: VLT-NACO $K_{\rm s}$ -band image of GQ Lup and its 6 mag fainter companion candidate $0.7325 \pm 0.0034^{\prime \prime }$ west.
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$\begin{figure} \par\includegraphics[width=8.2cm,height=7.4cm,clip]{Gj061_f3.ps}\end{figure}$	Figure 3: Our flux-calibrated K-band NACO spectrum of the companion of GQ Lup ( bottom) compared to the young M8 brown dwarfs in Cha I ( top) from Comerón et al. (2000), L2 (2MASSW J0829066+145622, 2nd from top) from Reid et al. (2001), and a GAIA-Dusty template spectrum for 2000 K and $\log~g=2$ , which compares well with the companion.
Open with DEXTER