All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{9863fig1.ps}\end{figure}$ Figure 1: Lightcurves in four energy bands for a 1.25 $M_{\odot }$ ONe-type nova ( left) and for a 1.15 $M_{\odot }$ CO-type nova ( right) based on the most recent available nova models and for a distance of 1 kpc.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9863fig2.ps} \end{figure}$ Figure 2: Histogram of the novae discovered in 5 years intervals from 1901-2005 ( left) and per year from 1995-2005 ( right).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{9863fig3.ps} \end{figure}$ Figure 3: Distribution of the distances from the Sun of the simulated novae. Black, red and green histograms correspond to novae distributed according to models 1-3 respectively (see Table 1).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{9863fig4.ps} \end{figure}$ Figure 4: Distribution of the distances from us of the novae detected in gamma rays in the Monte Carlo simulation. Model 1 was assumed.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{9863fig5.eps} \end{figure}$ Figure 5: Distribution of the magnitude of the novae detected in gamma rays in the Monte Carlo simulation (solid line). The dashed line represents the same distribution weighted for the probability of optical discovery of a nova (see text for details).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip,origin=rb]{9863fig6.ps} \end{figure}$ Figure 6: Average expected flux as a function of integration time for the nova V2362 Cyg. Red and green bars are supposing a CO type and a ONe type nova respectively. Upper limits from BAT are indicated by arrows, for percentage coverage of possible onset times P= 10% (black) and P = 50% (blue). The purple curve represents the ideal 5 $\sigma$ BAT sensitivity if the source were observed continuously in the fully coded FOV. As expected, for long integrations the sensitivity is better, but the average flux lower.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{9863fig1.ps}\end{figure}$	Figure 1: Lightcurves in four energy bands for a 1.25 $M_{\odot }$ ONe-type nova ( left) and for a 1.15 $M_{\odot }$ CO-type nova ( right) based on the most recent available nova models and for a distance of 1 kpc.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9863fig2.ps} \end{figure}$	Figure 2: Histogram of the novae discovered in 5 years intervals from 1901-2005 ( left) and per year from 1995-2005 ( right).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{9863fig3.ps} \end{figure}$	Figure 3: Distribution of the distances from the Sun of the simulated novae. Black, red and green histograms correspond to novae distributed according to models 1-3 respectively (see Table 1).
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{9863fig4.ps} \end{figure}$	Figure 4: Distribution of the distances from us of the novae detected in gamma rays in the Monte Carlo simulation. Model 1 was assumed.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{9863fig5.eps} \end{figure}$	Figure 5: Distribution of the magnitude of the novae detected in gamma rays in the Monte Carlo simulation (solid line). The dashed line represents the same distribution weighted for the probability of optical discovery of a nova (see text for details).
Open with DEXTER