![\begin{figure}
\par\includegraphics[width=8.8cm,clip]{1520fig1.ps}
\end{figure}](/articles/aa/full/2005/21/aa1520/img22.gif) |
Figure 1:
Displacement between optical and X-ray positions for point-like sources in
the total sample. The solid circle refers to thecross-correlation radius of
20
 ;
the dashed one, with 13
radius, contains about 90% of the
identifications. |
| Open with DEXTER | |
In the text
 |
Figure 2:
First page of the figure available in electronic form. It presents
the
X-ray contours from smoothed X-ray images superimposed onto optical images.
Galaxies are generally at the center of the field. Smoothing is done with a
Gaussian function of
for point-like sources and of
for extended sources. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.2cm,clip]{1520fig3.ps}
\end{figure}](/articles/aa/full/2005/21/aa1520/img54.gif) |
Figure 3: X-ray-to-optical ratio distribution for the total sample. Both fluxes are in units of erg cm-2 s-1. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.4cm,clip]{1520fig4.ps}
\end{figure}](/articles/aa/full/2005/21/aa1520/img58.gif) |
Figure 4:
Sky coverage for the fields at galactic latitude 
10
and off-axis angle
  ,
computed by assuming
a thermal bremsstrahlung spectrum with kT = 5 keV and galactic line of sight
absorption. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.6cm,clip]{1520fig5.ps}
\end{figure}](/articles/aa/full/2005/21/aa1520/img61.gif) |
Figure 5:
The integral
distribution for the complete
serendipitous subsample (asterisks).
The solid line represents the -1.1 slope and the dashed line the Euclidean -1.5 slope. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.6cm,clip]{1520fig6.ps}
\end{figure}](/articles/aa/full/2005/21/aa1520/img64.gif) |
Figure 6:
B flux versus X-ray flux for our total sample
(solid triangles), for the Einstein
sample (empty circles), for the Zimmermann et al. (2001) sample galaxies
(asterisks), and for the EMSS galaxies (empty pentagons). Solid lines
correspond to log
 ,
-2, -4, as indicated; the horizontal
dashed line is
the
mB = 15.5 limit. Only detections in the Einstein sample and
only objects with
 erg cm-2 s-1 and log
 in the Zimmermann et al. (2001) sample are plotted (see text). |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.5cm,clip]{1520fig7.ps}
\end{figure}](/articles/aa/full/2005/21/aa1520/img73.gif) |
Figure 7:
Comparison of the
distribution obtained from
the present sample (asterisks) with several other relations for normal
galaxies from the literature. The dashed line represents the Euclidean
relationship of Fig. 5 extrapolated to the full flux range
considered. Symbols refer to:
EMSS galaxies (empty circles); candidate
galaxies in Zimmermann et al. (2001; solid squares); normal galaxies
(crosses), including LLAGN (solid circles, Georgakakis et al. 2004a),
and stacking analysis (solid
triangles, Georgakakis et al. 2003) found in the XMM-Newton/2dF
survey; XMM-Newton/Sloan DSS normal galaxies
from Georgakakis et al. (2004b; empty
squares); Chandra Deep Fields results from Hornschemeier et al. (2003;
empty triangles); optimistic or
pessimistic curves given by Bauer et al. (2004) (upper/lower dotted line);
Bayesian sample of Norman et al. (2004) reported by Ranalli et al. (2004;
dot - dashed line). Open stars and horned-shaped box indicate the
detections and fluctuation analysis predictions of Miyaji & Griffiths
(2002). |
| Open with DEXTER | |
In the text
Full Version
 |
Figure 2:
First page of the figure available in electronic form. It presents
the X-ray contours from smoothed X-ray images superimposed onto optical images.
Galaxies are generally at the center of the field. Smoothing is done with a
Gaussian function of
for point-like sources and of
for extended sources. |
| Open with DEXTER | |
In the text
 |
Figure 2:
X-ray contours from smoothed X-ray images superimposed onto optical images.
Galaxies are generally at the center of the field. Smoothing is done with a
Gaussian function of
for point-like sources and of
for extended sources.
|
| Open with DEXTER | |
In the text
 |
Figure 2: continued. |
| Open with DEXTER | |
In the text
 |
Figure 2: continued. |
| Open with DEXTER | |
In the text
 |
Figure 2: continued. |
| Open with DEXTER | |
In the text
 |
Figure 2: continued. |
| Open with DEXTER | |
In the text
 |
Figure 2: continued. |
| Open with DEXTER | |
In the text
 |
Figure 2: continued. |
| Open with DEXTER | |
In the text
 |
Figure 2: continued. |
| Open with DEXTER | |
In the text
 |
Figure 2: continued. |
| Open with DEXTER | |
In the text
 |
Figure 2: continued. |
| Open with DEXTER | |
In the text
 |
Figure 2: continued. |
| Open with DEXTER | |
In the text