Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{0516fig1}\end{figure}$ Figure 1: Upper 5 panels: photon count rates in two WFC bands and 3 Konus bands. A time interval of 1.48 s was subtracted from the Konus times to account for the delay in light travel time between Wind and BeppoSAX. The extrapolated (Gaussian) last peak is shown in the 2-9 keV light curve. The lowest panel shows the photon index resulting from a power law fit to the WFC spectra only.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{0516fig2}\end{figure}$ Figure 2: Histogram of 2-10/40-700 keV fluence ratio for the BeppoSAX GRBs.
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In the text

$\begin{figure} \par\includegraphics[width=13.4cm,clip]{0516fig3}\end{figure}$ Figure 3: Spectra for the two BeppoSAX-MECS ToOs. The data are fitted with a power law plus a Galactic $N_{\rm H}$ . Note the excess around 3 keV in both ToOs.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0516fig4}\end{figure}$ Figure 4: X-ray (2-10 keV) WFC and MECS light curve including GRB 020410. The flatter fit is obtained using only the MECS data; the steeper one is instead constrained by using the 90% upper limit to the fitted slope.
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In the text

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{0516fig5}\end{figure}$ Figure 5: 600 s co-added R-band image of the GRB 020410 field taken with the MOA 0.6-m telescope 6.25 h after the burst. The larger circle represents the MECS 20'' error box; the smaller one highlights the OT at the HST position. Norh is up and East to the left.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0516fig6}\end{figure}$ Figure 6: R-band magnitudes and possible time evolution of the optical transient of GRB 020410. The first point is the MOA 0.6-m detection. The asterisk is the ESO 3.6-m (see also Levan et al. 2004) upper limit. Filled triangles are the HST measurements converted using $R-V\simeq 0.4$ ( $\check{\rm S}$ imon et al. 2001). The early time decay law marginally agrees with that observed in X-rays.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{0516fig1}\end{figure}$	Figure 1: Upper 5 panels: photon count rates in two WFC bands and 3 Konus bands. A time interval of 1.48 s was subtracted from the Konus times to account for the delay in light travel time between Wind and BeppoSAX. The extrapolated (Gaussian) last peak is shown in the 2-9 keV light curve. The lowest panel shows the photon index resulting from a power law fit to the WFC spectra only.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{0516fig2}\end{figure}$	Figure 2: Histogram of 2-10/40-700 keV fluence ratio for the BeppoSAX GRBs.
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$\begin{figure} \par\includegraphics[width=13.4cm,clip]{0516fig3}\end{figure}$	Figure 3: Spectra for the two BeppoSAX-MECS ToOs. The data are fitted with a power law plus a Galactic $N_{\rm H}$ . Note the excess around 3 keV in both ToOs.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0516fig4}\end{figure}$	Figure 4: X-ray (2-10 keV) WFC and MECS light curve including GRB 020410. The flatter fit is obtained using only the MECS data; the steeper one is instead constrained by using the 90% upper limit to the fitted slope.
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$\begin{figure} \par\includegraphics[width=8.45cm,clip]{0516fig5}\end{figure}$	Figure 5: 600 s co-added R-band image of the GRB 020410 field taken with the MOA 0.6-m telescope 6.25 h after the burst. The larger circle represents the MECS 20'' error box; the smaller one highlights the OT at the HST position. Norh is up and East to the left.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0516fig6}\end{figure}$	Figure 6: R-band magnitudes and possible time evolution of the optical transient of GRB 020410. The first point is the MOA 0.6-m detection. The asterisk is the ESO 3.6-m (see also Levan et al. 2004) upper limit. Filled triangles are the HST measurements converted using $R-V\simeq 0.4$ ( $\check{\rm S}$ imon et al. 2001). The early time decay law marginally agrees with that observed in X-rays.
Open with DEXTER