All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4626fig1} \end{figure}$ Figure 1: Maximum-entropy map of the Galactic plane (within latitude $\pm$ 30 $^\circ$ ) in the ⁴⁴Ti energy window (1.066-1.246 MeV) for the combination of CGRO observations from 0.1 to 617.1. Two crosses mark the positions of Cas A and GRO J0852-4642. This figure is adopted from Iyudin (1999).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16.7cm,clip]{4626fig2} \end{figure}$ Figure 2: The expected Ti sky of 10 simulated galaxies of model A where the supernova recurrence time is taken to be 30 years and the supernovae ratio of Ia:Ib:II = 0.10:0.15:0.75. Simulating a 10⁵ galaxy sky, a gamma-ray detector with a detection limit of $10^{-5}~\rm cm^{-2}~s^{-1}$ would have a probability of detecting 0, 1, and 2 ⁴⁴Ti sources of 0.0017, 0.012, and 0.037, respectively. A slightly better instrument than the $10^{-5}\rm ~cm^{-2}~s^{-1}$ detection limit would detect several ⁴⁴Ti sources.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16.7cm,clip]{4626fig3} \end{figure}$ Figure 3: Cumulative ⁴⁴Ti gamma-ray line flux distribution of supernovae with $f_{\gamma }>$ 1 $\times$ 10^-12 cm^-2 s^-1 according to our Model A (see Appendix A.2) with supernovae type ratio of Ia:Ib:II = 0.1:0.15:0.75 ( left). Expected average number of supernovae per sample galaxy with their ⁴⁴Ti gamma-line fluxes above detection limits, for a supernova recurrence time of 30 yr, irrespective of their position in the sky ( right). The detection limit of COMPTEL instrument is shown as a dotted line.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{4626fig4} \end{figure}$ Figure 4: The longitude distribution of supernovae for four ⁴⁴Ti gamma-ray line flux bandwidths in Model A of Appendix A.2 with supernovae type ratio of Ia:Ib:II = 0.1:0.15:0.75. The equal-bin width is 20 degrees in longitude. Only the $f_{\gamma }<1\times 10^{-6}$ cm^-2 s^-1 distribution is normalized and multiplied by a factor of 0.298.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{4626fA1a}\hspace*{3mm} \includegraphics[angle=90,width=8.4cm,clip]{4626fA1b} \end{figure}$ Figure A.1: Same as Fig. 4 but for models B (left) and C (right).

In the text

$\begin{figure} \par\includegraphics[origin=rb,angle=90,width=16cm,clip]{4626fgA2} \end{figure}$ Figure A.2: The distribution of supernovae in model A in Galactic longitude and latitude.

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.2cm,clip]{4626fgA3} \end{figure}$ Figure A.3: The distribution of supernovae distance in model A.

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{4626fgB1} \end{figure}$ Figure B.1: The distribution of the peak absolute magnitudes of supernova in the B-band of model A.

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.2cm,clip]{4626fgB2} \end{figure}$ Figure B.2: The Galactic visual extinction magnitude as a function of distance from the Sun to various direction according to empirical model of (Hakkila et al. 1997).

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{4626fgB3} \end{figure}$ Figure B.3: The apparent magnitude of supernovae in model A according to empirical extinction model of Hakkila et al. (1997).

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4626fgB4} \end{figure}$ Figure B.4: Normalized relative probability of Galactic SNe rate calculated from three different analysis vs. SNe recurrence time for model A. The solid line is the probability of the model in which the number of SNe with $m_V \leq 0$ is 6 in a 1000 year duration. The dashed-line is the probability inferred by maximum likelihood analysis of COMPTEL's 1.157 MeV $\gamma$ -line inner galactic ( $l\leq 90$ , $b\leq 30$ ) image map. The dotted-line is the relative probability from chi-square test that the 1.157 MeV $\gamma$ -line fluxes in the model are consistent with the COMPTEL observed fluxes. The labels of the curves show the optimal, 1 $\sigma$ ranges, or the 1 $\sigma$ lower limits of the SNe recurrence time. The boxes, circles, and diamonds on the curves show the 1 $\sigma$ , 90%, and 95% relative probabilities. The shaded area shows the range of the Galactic SNe recurrence time that is consistent with better than 1 $\sigma$ probability with each of the historical record and the COMPTEL flux dataspace analysis.

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4626fB5a}\hspace*{4mm} \includegraphics[width=8cm,clip]{4626fB5b} \end{figure}$ Figure B.5: Same as Fig. B.4 but for models B ( left) and C ( right).

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4626fig1} \end{figure}$	Figure 1: Maximum-entropy map of the Galactic plane (within latitude $\pm$ 30 $^\circ$ ) in the ⁴⁴Ti energy window (1.066-1.246 MeV) for the combination of CGRO observations from 0.1 to 617.1. Two crosses mark the positions of Cas A and GRO J0852-4642. This figure is adopted from Iyudin (1999).
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$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{4626fig4} \end{figure}$	Figure 4: The longitude distribution of supernovae for four ⁴⁴Ti gamma-ray line flux bandwidths in Model A of Appendix A.2 with supernovae type ratio of Ia:Ib:II = 0.1:0.15:0.75. The equal-bin width is 20 degrees in longitude. Only the $f_{\gamma }<1\times 10^{-6}$ cm^-2 s^-1 distribution is normalized and multiplied by a factor of 0.298.
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