![\begin{figure}
\par\includegraphics[width=8cm,clip]{0126fig1}
\end{figure}](/articles/aa/full/2004/23/aa0126/img9.gif) |
Figure 1: Raw CHANDRA image of NGC 1052 showing the spatial distribution of photon events in the energy range (0.2-1.0) keV. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=12cm,clip]{0126fig2}
\end{figure}](/articles/aa/full/2004/23/aa0126/img14.gif) |
Figure 2:
Three color CHANDRA image of the jet-associated X-ray emission in NGC 1052
with the 1.4 GHz MERLIN radio image overlaid in contours. The CHANDRA
image has been
smoothed to a resolution of 4
to increase sensitivity.
Red represents photons between 0.1 keV and 1 keV, green between 1 keV and 2 keV
and blue (2-3) keV. The clipping level is 3 .
The MERLIN image was
restored with a circular beam of 1.7 arcsec FWHM.
Contours are shown for (0.5, 1.5, 2.5, 3.5, 4.5, 5.5, 6.5)  1 mJy/beam.
The jet-associated emission is dominated by soft X-rays below 1 keV,
whereas the AGN appears white, representing a rather flat X-ray spectrum. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.5cm,clip]{0126fig3}
\end{figure}](/articles/aa/full/2004/23/aa0126/img15.gif) |
Figure 3:
Comparison
between the VLA image of NGC 1052 observed in 1980 (Wrobel 1984) and the MERLIN image from 1995, both at 1.4 GHz. Both maps have been convolved with the same (circular) restoring beam
of 1.7 arcsec FWHM. Contours at (-1, 1, 2, 3, 4, 5, 6, 7, 8, 9, 10, 11, 12, 13, 14, 15,
800) 0.5 mJy are given in both maps (the VLA map also shows negative
contours at (-4, -3, -2)
0.5 mJy). The hot spots (labeled as H1 and H2)
do not show any positional changes.
The emission peak of the eastern knot (A)
is about 0.5 arcsec closer to the core in 1995. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=12cm,clip]{0126fig4}
\end{figure}](/articles/aa/full/2004/23/aa0126/img16.gif) |
Figure 4:
HST structure map of NGC 1052. Dark regions represent dust obscuration while
bright regions are locations of enhanced emission. Overlaid is the pure naturally
weighted MERLIN map showing the core of NGC 1052 with sub-arcsecond resolution. Contours
at (-1, 1, 2, 4, 8, 16, 32, 64, 128, 256, 512, 1024) 0.5 mJy/beam
are shown. The inlaid panel shows an enlarged view of the marked box around the
area of the optical emission cone. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.5cm,clip]{0126fig5}
\end{figure}](/articles/aa/full/2004/23/aa0126/img21.gif) |
Figure 5: Top panel: X-ray spectrum of the extended X-ray jet emission and the Raymond/Smith plasma model folded with the detector response matrix (solid line). Middle panel: X-ray spectrum of the nuclear emission and the best fit of model Ib (solid line, compare Table 4.2). Bottom panel: the unfolded model Ib spectrum representing an absorbed Raymond/Smith plasma whose model parameters have been held fixed at the best fitting values to the extended X-ray emission spectrum (see Table 1) plus a power-law with an additional absorber. |
| Open with DEXTER | |
In the text