All Figures

$\begin{figure} {\hbox{\psfig{figure=h4543f1.ps,width=8cm,angle=0,bbllx=150pt,bblly=287pt,bburx=706pt,bbury=671pt} }}\end{figure}$ Figure 1: A proposed unification scheme for accreting black holes in the mass and accretion rate plane. Above a few percent of the Eddington accretion rate, the systems are proposed to be dominated by disk emission, while below they are inherently dominated by jet emission (RG = radio galaxy). Standard inclination-based unified schemes (Antonucci 1993; Urry & Padovani 1995) are still assumed to be valid but are not explicitly shown here. Given a correlation between bulge mass and black hole mass, the AGN with the most massive black holes are supposed to reside in elliptical galaxies, while less massive black holes are predominantly in spirals. This is, of course, not applicable to XRBs.
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In the text

$\begin{figure} {\hbox{\psfig{figure=h4543f2.ps,width=8cm,angle=0,bbllx=107pt,bblly=562pt,bburx=490pt,bbury=775pt} }}\end{figure}$ Figure 2: A schematic jet spectrum and its theoretically expected scaling with mass and accretion rate. The spectrum has a flat-to-inverted, optically thick part below a turn-over frequency $\nu _{\rm t}$ and a steep optically thin spectrum above. For most sources the flat-to-inverted part of the spectrum will be in the radio/infrared while the steep part will be in the optical and X-rays. A change in the absolute accretion rate will shift the spectrum along a diagonal line from the bottom left to the top right. A change in mass will shift the spectrum horizontally only. Lowering mass and accretion rate (e.g., by keeping the accretion rate at a constant fraction of the Eddington accretion rate) will shift the spectrum towards the bottom right, where stellar-mass black holes are found.
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In the text

$\begin{figure} {\psfig{figure=h4543f3.ps,width=8cm,angle=0} }\end{figure}$ Figure 3: Radio/X-ray correlation for XRBs with our AGN sample. We only extrapolate the optical measurements of some AGN (FR I radio galaxies) to a corresponding monochromatic X-ray luminosity without a mass correction. For Sgr A* we show the quiescent and the flare spectrum. The solid line is the analytically predicted non-linear radio/X-ray correlation from the jet model, normalized for GX 339-4. The supermassive black holes fall below the extrapolation from the X-ray binaries.
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In the text

$\begin{figure} {\psfig{figure=h4543f4.ps,width=8cm,angle=0} }\end{figure}$ Figure 4: The same as Fig. 3 but for an equivalent X-ray luminosity, $L'_{\rm X}$ , which has been individually corrected for the mass factor and scaled to the value the X-ray luminosity would have for a central black hole of only 6 $M_{\odot }$ , as in GX 339-4 (see Eq. (7)). Corrections for Doppler factors have not been applied.
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In the text

$\begin{figure} {\psfig{figure=h4543f5.ps,width=8cm,angle=0} }\end{figure}$ Figure 5: The same as Fig. 4 but the radio and X-ray luminosities of BL Lac objects have been corrected for Doppler boosting. As discussed in the text, this mainly moves BL Lacs along the correlation and they now occupy the same region as FR Is - their parent population within the inclination-based unified scheme.
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In the text

$\begin{figure} {\hbox{\psfig{figure=h4543f6.ps,width=8cm,angle=0} }}\end{figure}$ Figure 6: Radio/X-ray correlation for XRBs and AGN, where the X-ray flux of all AGN has been increased by a constant value of 10⁷, corresponding to an average AGN mass of $3\times10^9 ~M_\odot$ .
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In the text

$\begin{figure} {\psfig{figure=h4543f4.ps,width=8cm,angle=0} }\end{figure}$	Figure 4: The same as Fig. 3 but for an equivalent X-ray luminosity, $L'_{\rm X}$ , which has been individually corrected for the mass factor and scaled to the value the X-ray luminosity would have for a central black hole of only 6 $M_{\odot }$ , as in GX 339-4 (see Eq. (7)). Corrections for Doppler factors have not been applied.
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$\begin{figure} {\psfig{figure=h4543f5.ps,width=8cm,angle=0} }\end{figure}$	Figure 5: The same as Fig. 4 but the radio and X-ray luminosities of BL Lac objects have been corrected for Doppler boosting. As discussed in the text, this mainly moves BL Lacs along the correlation and they now occupy the same region as FR Is - their parent population within the inclination-based unified scheme.
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$\begin{figure} {\hbox{\psfig{figure=h4543f6.ps,width=8cm,angle=0} }}\end{figure}$	Figure 6: Radio/X-ray correlation for XRBs and AGN, where the X-ray flux of all AGN has been increased by a constant value of 10⁷, corresponding to an average AGN mass of $3\times10^9 ~M_\odot$ .
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