![\begin{figure}
\par\includegraphics[angle=-90,width=8.8cm,clip]{Gl231_f1.eps}
\end{figure}](/articles/aa/full/2005/23/aagl231/img44.gif) |
Figure 1:
a) Image of the ring with 0
 5 seeing, b) best configuration
for the lens and the source, with the position of the caustics (cf. text for parameter definitions), c)
best-fitting
image convolved with the seeing, and d) the predicted image at the resolution
of HST/ACS. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[angle=-90,width=8.8cm,clip]{Gl231_f2.eps}
\end{figure}](/articles/aa/full/2005/23/aagl231/img51.gif) |
Figure 2:
Top: the spectrum of the lens (middle black line),
the underlying sky emission (bottom red line), and the
HYPERZ-derived best-fit synthetic spectrum (top blue line).
Bottom: observed
photometry and the
spectral energy distribution of the best-fitting spectrum shown above.
|
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[angle=-90,width=8.8cm,clip]{Gl231_f3.eps}
\end{figure}](/articles/aa/full/2005/23/aagl231/img86.gif) |
Figure 3:
Top: the spectrum of the source galaxy, showing strong lines
from the interstellar medium, yields a redshift of
 .
Bottom: the shape of the continuum and the depth of the lines are
consistent with a population of stars having past a major episode of
star formation, very similar to the post-starburst galaxies shown
in comparison, both distant (cB58) or nearby (NGC 1741). The sky
emission and some telluric lines are also indicated.
|
| Open with DEXTER | |
In the text