All Figures

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{5346fig1a.ps}\includegraphics[width=7.25cm,clip]{5346fig1b.ps}\end{figure}$ Figure 1: Left: sky map of the GRO J1411-64 region as seen by IBIS/ISGRI in the 20-40 keV range, by combining all data obtained in the observations performed during 2004 December 30 to 2005 January 6. See Table 2 for details of each detected source. Right: sky map of the GRO J1411-64 region as seen by JEMX in 1.6-10 keV range, by combining all data obtained in the observations performed during 2004 December 30 to 2005 January 6. The detected two sources are 1H 1254-690 (122 $\sigma$ ), and 4U 1323-62 (39 $\sigma$ ).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.1cm,clip]{5346fig2a.ps}\in... ...fig2b.ps}\includegraphics[angle=-90,width=5.25cm,clip]{5346fig2c.ps}\end{figure}$ Figure 2: Left: light curve of 1H1254-690 with each bin averaged over 3000 s, observed by JEMX in the 1.6-10 keV range. Middle: light curve of GX 310-2 with each bin averaged over 3000 s, observed by IBIS/ISGRI in the 20-40 keV range. Right: light curve of the Circinus Galaxy with each bin averaged over half day, observed by IBIS/ISGRI in the 20-40 keV range.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.65cm,clip]{5346fig3a.ps}\i... ...fig3b.ps}\includegraphics[angle=-90,width=5.65cm,clip]{5346fig3c.ps}\end{figure}$ Figure 3: Left: spectrum of 1H1254-690 from the JEMX combined data. The fit model is cutoffpl in XSPEC. Middle: spectrum of GX 301-2 from IBSI/ISGRI combined data. The fit model is cutoffpl in XSPEC. Right: spectrum of the Circinus Galaxy from IBIS/ISGRI combined data. The fit model is cutoffpl plus wabs in XSPEC.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{5346fig4.ps}\end{figure}$ Figure 4: Light curve of GRO J1411-64 as observed by COMPTEL at 0.75-1 MeV band. The error bar is 1 $\sigma$ and upper limit 2 $\sigma$ . These data points include the 7 viewing periods when the source was flaring.
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In the text

$\begin{figure} \par\includegraphics[width=7.05cm,clip]{5346fig5.ps}\end{figure}$ Figure 5: The skymap of GRO J1411-64 as observed by COMPTEL in 0.75-1 MeV during 1991-1996, not including the flare period of 4 months in 1995. The star represents the best-guessed source location. The contour lines start at a detection significance level of 3 $\sigma$ with steps of 0.5 $\sigma$ .
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In the text

$\begin{figure} \par\includegraphics[width=4.6cm,clip]{5346fig6.eps}\end{figure}$ Figure 6: Combined energy spectrum of GRO J1411-64. Filled (open) circles represent flare (low) states of GRO J1411-64 as observed by COMPTEL at MeV energies. The corresponding power law shapes (solid line for the flare state, dashed line for the low state), are compared to 2 $\sigma$ upper limits obtained from IBIS/ISGRI (triangles) and SPI (squares). The solid curve at low energies is the energy spectrum of Circinus Galaxy derived from the IBIS/ISGRI data. The error bar is 1 $\sigma$ and upper limit 2 $\sigma$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5346fig7.ps}\end{figure}$ Figure 7: XMM-Newton EPIC image (combining all 3 cameras), where detected sources and previously catalogued sources have been labeled. The centroid of the COMPTEL source GRO 1411-64 is marked with a square box, the error contour being larger than the image itself.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.6cm,clip]{5346fig8.ps}\end{figure}$ Figure 8: EPIC pn hardness ratio HR₂ (see text for details) versus source counts in that detector.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.8cm,clip]{5346fig9.ps}\end{figure}$ Figure 9: XMM-Newton unfolded spectrum of the X-ray source XMMU J141255.6-635932. The model shown is only the thermal component in the X-ray spectrum. The COMPTEL detections and the INTEGRAL upper limits are also shown at high energies, with horizontal bars denoting 2 $\sigma$ upper limits.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{5346fig10.ps}\end{figure}$ Figure 10: A microquasar model in the light of observational constraints. See text for details.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{5346fig11.ps}\end{figure}$ Figure 11: The original observations of GRO J1411-64 as reported in Zhang et al. (2002), see Table 1. The dependence from the individual measurements from the underlaying exposure is easily seen, as is the different character in the phase 4 vs. phase 5 measurements, which exhibit the largest flux values, but missing a 1-3 MeV flux in case of the phase 5 measurement.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.1cm,clip]{5346fig2a.ps}\in... ...fig2b.ps}\includegraphics[angle=-90,width=5.25cm,clip]{5346fig2c.ps}\end{figure}$	Figure 2: Left: light curve of 1H1254-690 with each bin averaged over 3000 s, observed by JEMX in the 1.6-10 keV range. Middle: light curve of GX 310-2 with each bin averaged over 3000 s, observed by IBIS/ISGRI in the 20-40 keV range. Right: light curve of the Circinus Galaxy with each bin averaged over half day, observed by IBIS/ISGRI in the 20-40 keV range.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.65cm,clip]{5346fig3a.ps}\i... ...fig3b.ps}\includegraphics[angle=-90,width=5.65cm,clip]{5346fig3c.ps}\end{figure}$	Figure 3: Left: spectrum of 1H1254-690 from the JEMX combined data. The fit model is cutoffpl in XSPEC. Middle: spectrum of GX 301-2 from IBSI/ISGRI combined data. The fit model is cutoffpl in XSPEC. Right: spectrum of the Circinus Galaxy from IBIS/ISGRI combined data. The fit model is cutoffpl plus wabs in XSPEC.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{5346fig4.ps}\end{figure}$	Figure 4: Light curve of GRO J1411-64 as observed by COMPTEL at 0.75-1 MeV band. The error bar is 1 $\sigma$ and upper limit 2 $\sigma$ . These data points include the 7 viewing periods when the source was flaring.
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$\begin{figure} \par\includegraphics[width=7.05cm,clip]{5346fig5.ps}\end{figure}$	Figure 5: The skymap of GRO J1411-64 as observed by COMPTEL in 0.75-1 MeV during 1991-1996, not including the flare period of 4 months in 1995. The star represents the best-guessed source location. The contour lines start at a detection significance level of 3 $\sigma$ with steps of 0.5 $\sigma$ .
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5346fig7.ps}\end{figure}$	Figure 7: XMM-Newton EPIC image (combining all 3 cameras), where detected sources and previously catalogued sources have been labeled. The centroid of the COMPTEL source GRO 1411-64 is marked with a square box, the error contour being larger than the image itself.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.6cm,clip]{5346fig8.ps}\end{figure}$	Figure 8: EPIC pn hardness ratio HR₂ (see text for details) versus source counts in that detector.
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$\begin{figure} \par\includegraphics[angle=270,width=6.8cm,clip]{5346fig9.ps}\end{figure}$	Figure 9: XMM-Newton unfolded spectrum of the X-ray source XMMU J141255.6-635932. The model shown is only the thermal component in the X-ray spectrum. The COMPTEL detections and the INTEGRAL upper limits are also shown at high energies, with horizontal bars denoting 2 $\sigma$ upper limits.
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$\begin{figure} \par\includegraphics[width=6.2cm,clip]{5346fig10.ps}\end{figure}$	Figure 10: A microquasar model in the light of observational constraints. See text for details.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{5346fig11.ps}\end{figure}$	Figure 11: The original observations of GRO J1411-64 as reported in Zhang et al. (2002), see Table 1. The dependence from the individual measurements from the underlaying exposure is easily seen, as is the different character in the phase 4 vs. phase 5 measurements, which exhibit the largest flux values, but missing a 1-3 MeV flux in case of the phase 5 measurement.
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