Astronomy & Astrophysics

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$\begin{figure} \par\mbox{\hspace*{3.4cm}\subfigure[]{\includegraphics[width=6.3c... ...} \subfigure[]{\includegraphics[width=6.4cm,clip]{0486fig1c.eps} }} \end{figure}$ Figure 1: Radio emission contours with the following multiples of the rms noise (Table 1): (-3, -2.1, 2.1, 3, 4.2, 6, 8.4, 12, 16.8, 24). The size of the restoring beam in milliarcseconds, observing epoch, integration time in minutes, and frequency in GHz are given in parentheses after each object name (see Table 1). a) NGC 524 ( $4.5 \times 2.0$ ; 2001 Sep. 01; 180; 5); b) NGC 5354 ( $7.6 \times 3.8$ ; 2001 Sep. 17; 40; 2.3); c) NGC 5354 ( $2.3 \times 1.6$ ; 200 June 22; 105; 5).
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In the text

$\begin{figure} \par\subfigure[]{\includegraphics[width=6.3cm,clip]{0486fig2a.eps... ...par\subfigure[]{\includegraphics[width=6.3cm,clip]{0486fig2c.eps} } \end{figure}$ Figure 2: Same as Fig. 1. a) NGC 5846 (9.2 $\times$ 3.7; 2001 Oct. 06; 48; 2.3); b) NGC 5846 (3.1 $\times$ 1.4; 2000 June 22; 112; 5); c) NGC 5846 ( $1.7 \times 0.7$ ; 2001 Oct. 06; 48; 15).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0486fig3.eps}\end{figure}$ Figure 3: The radio to X-ray ratio ( $R_{\rm x}$ ) versus radio to optical ( $R_{\rm o}$ ) relation in logarithmic units. Upper limits in X-ray and radio luminosity are illustrated by arrows. The solid lines define the radio-loud/radio-quiet boundary for the optical and X-ray diagnostic.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0486fig4.eps}\end{figure}$ Figure 4: The relation between hard X-ray core and H $\alpha$ emission line luminosity. Upper limits in X-ray luminosity are illustrated by arrows. The shaded area corresponds to typical values for LLAGN - ${\log \left(\frac{L_{\rm X}}{L_{\rm H\alpha}}\right) \sim 1 {-} 2}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0486fig5.eps}\end{figure}$ Figure 5: The relation between the mas-scale radio core and hard X-ray core luminosity. Upper limits in radio and X-ray luminosity are illustrated by arrows. The solid line defines the radio-loud/radio-quiet boundary for the X-ray diagnostic.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0486fig6.eps}\end{figure}$ Figure 6: The relation between the mas-scale radio core/hard X-ray core luminosity ratio ( $L_{\rm 5~GHz}$ / $L_{\rm 2{-}10~keV}$ ) and the hard X-ray core luminosity. Upper limits in radio and X-ray luminosity are illustrated by arrows. Numbers in parentheses refer to the logarithm of the black hole masses and the respective error, considering an error in log $\sigma _{\rm c}=0.06$ , 0.02 and 0.01 plus a 10% error in the conversion of $\sigma _{\rm e}$ to $\sigma _{\rm c}$ . The solid lines refer to the ADAF model prediction - ${L_{\rm R} \propto M_{\rm BH}~ L_{\rm X}^{0.1}}$ - for several black hole masses - ${\log ~ M_{\rm BH}=7.0, 8.0, 9.0}$ - in logarithmic units of solar mass.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0486fig7.eps}\end{figure}$ Figure 7: The relation between the mas-scale radio core luminosity and the black hole mass. Upper limits in radio luminosity are illustrated by arrows. We give typical error bars for the black hole mass, considering an error in log $\sigma _{\rm c}=0.06$ , 0.02 and 0.01 plus a 10% error in the conversion of $\sigma _{\rm e}$ to $\sigma _{\rm c}$ . The solid lines refer to the ADAF model prediction - ${L_{\rm R} \propto m_{\rm acc}^{1.2}~M_{\rm BH}^{1.6}}$ - for different mass accretion rates - ${m_{\rm acc}=10^{-2}, 10^{-3}, 10^{-4}}$ - given in dimensionless units of Eddington accretion rate.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0486fig8.eps}\end{figure}$ Figure 8: The relation between the hard X-ray core luminosity and black hole mass. Upper limits in X-ray luminosity are illustrated by arrows. We give typical error bars for the black hole mass, considering an error in log $\sigma _{\rm c}=0.06$ , 0.02 and 0.01 plus a 10% error in the conversion of $\sigma _{\rm e}$ to $\sigma _{\rm c}$ . The solid lines refer to the ADAF model prediction - ${L_{\rm X} \propto M_{\rm BH} m_{\rm acc}^{2}}$ - for various accretion rates - ${m_{\rm acc}=10^{-2}, 10^{-3}, 10^{-4}}$ - given in dimensionless units of Eddington accretion rate.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0486fig9.eps}\end{figure}$ Figure 9: The relation between radio and "black hole mass-corrected'' X-ray luminosity, scaled to the $6~M_{\odot}$ black hole in XRB GX 339-4. The solid line is the predicted radio/X-ray correlation from the jet model and the ellipse details the broadband observations of GX 339-4 (Corbel et al. 2003; Markoff et al. 2003).
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In the text

$\begin{figure} \par\subfigure[]{\includegraphics[width=6.3cm,clip]{0486fig2a.eps... ...par\subfigure[]{\includegraphics[width=6.3cm,clip]{0486fig2c.eps} } \end{figure}$	Figure 2: Same as Fig. 1. a) NGC 5846 (9.2 $\times$ 3.7; 2001 Oct. 06; 48; 2.3); b) NGC 5846 (3.1 $\times$ 1.4; 2000 June 22; 112; 5); c) NGC 5846 ( $1.7 \times 0.7$ ; 2001 Oct. 06; 48; 15).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0486fig3.eps}\end{figure}$	Figure 3: The radio to X-ray ratio ( $R_{\rm x}$ ) versus radio to optical ( $R_{\rm o}$ ) relation in logarithmic units. Upper limits in X-ray and radio luminosity are illustrated by arrows. The solid lines define the radio-loud/radio-quiet boundary for the optical and X-ray diagnostic.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0486fig4.eps}\end{figure}$	Figure 4: The relation between hard X-ray core and H $\alpha$ emission line luminosity. Upper limits in X-ray luminosity are illustrated by arrows. The shaded area corresponds to typical values for LLAGN - ${\log \left(\frac{L_{\rm X}}{L_{\rm H\alpha}}\right) \sim 1 {-} 2}$ .
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0486fig5.eps}\end{figure}$	Figure 5: The relation between the mas-scale radio core and hard X-ray core luminosity. Upper limits in radio and X-ray luminosity are illustrated by arrows. The solid line defines the radio-loud/radio-quiet boundary for the X-ray diagnostic.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0486fig9.eps}\end{figure}$	Figure 9: The relation between radio and "black hole mass-corrected'' X-ray luminosity, scaled to the $6~M_{\odot}$ black hole in XRB GX 339-4. The solid line is the predicted radio/X-ray correlation from the jet model and the ellipse details the broadband observations of GX 339-4 (Corbel et al. 2003; Markoff et al. 2003).
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