![\begin{figure}
\par\includegraphics[width=12cm]{0527fig1.eps}\hfill
\parbox[b]{55mm}{
}
\end{figure}](/articles/aa/full/2005/47/aa0527-04/img7.gif) |
Figure 1: Comparison of a) the optical B band lightcurve and b) the 60 keV X-ray lightcurve of 3C 273. Optical data are from the Geneva photometric system (open points) and scaled observations from Kaspi et al. (2000, filled points). X-ray observations are from CGRO/BATSE (averaged into 30-days bins) (open points) and from INTEGRAL/ISGRI (filled points). |
| Open with DEXTER | |
In the text
![\begin{figure}\includegraphics[width=12cm]{0527fig2.eps}\hfill
\parbox[b]{55mm}{
}
\end{figure}](/articles/aa/full/2005/47/aa0527-04/img82.gif) |
Figure 2:
The Jeans mass as a function of the distance to the black hole and the ratio 
of the accretion velocity to free fall. Also shown in grey is the region in which cloud collapse is faster than accretion. Matter accreted from within the grey region of parameter space will be clumpy when arriving in the vicinity of the black hole, matter accreted from the white section of parameter space may be smooth, provided that it is homogeneous to start with. |
| Open with DEXTER | |
In the text