![\begin{figure}
\par {\includegraphics[width=8.8cm,clip]{3918.f1.ps} }\end{figure}](/articles/aa/full/2003/37/aa3918/img38.gif) |
Figure 1:
The image shows the coadded V-band image
taken with the 2.5 NOT at 31.067-31.135 March 2001 UT. The FOV
covered by the image corresponds to
 .
North
is to the top and East to the left. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\mbox{\includegraphics[width=8.6cm,clip]{3918.f2a.ps}\includegraphics[width=8.4cm,clip]{3918.f2b.ps} }
\end{figure}](/articles/aa/full/2003/37/aa3918/img50.gif) |
Figure 2:
Left panel: The global mapping of the fitted
SED
when the redshifts of the templates are varied in a
broad range (
0 < z <5). The dotted vertical line indicates the
spectroscopic redshift of the host galaxy (z=1.118). The different
symbols indicated the best fitted template type for each redshift. As
it is shown, the spectroscopic redshift is consistent with the broad
minimum (
0.65 < z < 1.20) centred at z=1.029. This minimum is
governed by Stb galaxies. Other local minima (for instance the one at
achieved with E and Im galaxies) show larger values of
Right panel: The plot shows a blow up around the
absolute minimum with no distinction among templates types. The
evolution of
rejects the photometric redshifts not located
at
0.65 < z < 1.2, specially the ones at z > 1.5 where
 .
General: The plot assumed a Sc86 IMF, a Sea79 extinction
law, and Solar metallicity (SOL-Sc86-Sea79 subfamily of templates). |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=7.4cm,clip]{3918.f3a.ps}\hspace*{1.6cm}
\includegraphics[width=7.4cm,clip]{3918.f3b.ps}
\end{figure}](/articles/aa/full/2003/37/aa3918/img104.gif) |
Figure 3:
The left panel shows a contour
plot of the GRB 000418 host galaxy seen with STIS (CL-band filter).
The observations were carried out 299 days after the gamma-ray event, so
no contribution from the OA is expected. The right panel contours show
the residuals of the host when the host galaxy surface brightness model
is subtracted (see Sect. 4.1 for further information). The
contours of both figures scale linearly with the detection confidence
level (from 
to  ,
with a step of 3 ). As can be
seen in the right plot, the residuals consist of a few pixels
above the background. They are concentrated in the host nucleus, where
the PSF of STIS might affect the surface photometry. Thus, we conclude
that (perhaps with the exception of the central region within a radius of
 )
there are no reliable underlying structures associated to
the host galaxy (like dust lanes, spiral arms or disks) above the
detection threshold of our STIS images. The FOV is
 .
The arrows indicate the orientation of the images. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par {\includegraphics[width=14cm,clip]{3918.f4.ps} }\end{figure}](/articles/aa/full/2003/37/aa3918/img105.gif) |
Figure 4:
The points show the measured flux in the
bands for the GRB 000418 host galaxy, once the
Galactic dereddening is introduced (
E(B-V)=0.033, Schlegel et al.
1998). The solid curve represent the best SED fitted to
the photometric points (
 ), corresponding to a
starburst synthetic template at a redshift of
z = 1.029. The
plots assumes a Sc86 IMF. The derived value of the starburst age
corresponds to 0.053 Gyr. The extinction law used to construct
the plot is given by Sea79. The fit is consistent with a low global
extinction in the host (
 ). The SED
shows an appreciable
 Å break,
approximately at the Z-band filter wavelength. |
| Open with DEXTER | |
In the text