All Figures

$\begin{figure} \par\includegraphics[angle=+90,width=8cm,clip]{5247fig1.ps} \end{figure}$ Figure 1: Galactic distribution of the unidentified $\gamma$ -ray sources from the third EGRET catalogue (Hartman et al. 1999): the two black circles show the positions of 3EG J0616-3310 and 3EG J1249-8330.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5247fig2.ps} \end{figure}$ Figure 2: Processed XMM-Newton EPIC/MOS image of field 4 (see Table 1. Photons selected from three different energy bands are colour-coded: red (0.3-1 keV); green (1-3 keV); blue (3-10 keV).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.3cm,clip]{5247f3a.ps}\hspace*{4mm} \includegraphics[angle=-90,width=6.3cm,clip]{5247f3b.ps} \end{figure}$ Figure 3: Histograms of the source count-rate distributions for each EPIC pointing of the error box of 3EG J0616-3310 (left, N1-N4) and 3EG J1249-8330 (right, N5-N8), in the energy ranges 0.5-2 keV (red line) and 2-10 keV (blue line). For observation 7 the distribution peaks at higher count rate ( $\log CR = -2.35$ ) due to the shorter effective exposure time.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.3cm,clip]{5247f4a.ps}\hspace*{4mm} \includegraphics[angle=-90,width=6.3cm,clip]{5247f4b.ps} \end{figure}$ Figure 4: Histogram of the source S/N distribution for the 3EG J0616-3310 (left, N1-N4) and 3EG J1249-8330 (right, N5-N8) fields.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.3cm,clip]{5247f5a.ps}\hspace*{4mm} \includegraphics[angle=-90,width=6.3cm,clip]{5247f5b.ps} \end{figure}$ Figure 5: Histograms of the HR distributions for sources in the 3EG J0616-3310 (left) and 3EG J1249-8330 (right) error boxes. Green bars indicate the expected HRs computed for thermal bremsstrahlung spectra with kT = 0.5, 1, 2 and 5 keV ( from left to right). Magenta bars indicate the expected HRs computed for power-law spectra with $\Gamma = 1$ , 1.5, 2 and 2.5 ( from right to left).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.1cm,clip]{5247f6a.ps}\hspace*{4mm} \includegraphics[angle=-90,width=6.1cm,clip]{5247f6b.ps}\end{figure}$ Figure 6: The total sky coverage of the EPIC observations of the 3EG J0616-3310 (left) and 3EG J1249-8330 (right) error boxes, in the energy bands 0.5-2 keV (red line) and 2-10 keV (blue line).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.1cm,clip]{5247f7a.ps}\hspace*{4mm} \includegraphics[angle=-90,width=6.1cm,clip]{5247f7b.ps}\end{figure}$ Figure 7: Cumulative log N-log S distribution of the sources detected in the EPIC observations of the 3EG J0616-3310 (left) and 3EG J1249-8330 (right) error boxes, in the energy bands 0.5-2 keV (red squares) and 2-10 keV (blue dots). For comparison, in both diagrams we also show the lower and upper limits of the high latitude log N-log S in the energy ranges 0.5-2 keV (red solid lines) and 2-10 keV (blue dashed lines).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5247fig8CMJN.eps}\end{figure}$ Figure 8: Composite BVR image (B = blue; V = green; R = red) of field 4 taken with WFI at the ESO/MPG 2.2 m telescope.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,angle=-90,clip]{5247f9a.ps}\hspace*{4mm} \includegraphics[width=6.2cm,angle=-90,clip]{5247f9b.ps} \end{figure}$ Figure 9: X-ray-to-optical flux ratios $f_{\rm X}/f_{\rm opt}$ for the X-ray sources detected in the 3EG J0616-3310 (left) and 3EG J1249-8330 (right) fields plotted as a function of the X-ray flux. Different colours refer to magnitudes computed in different bands i.e. V (green), B,B_j (blue), R,R_F (red). In case of multiple optical counterparts for a single X-ray source, the $f_{\rm X}/f_{\rm opt}$ value of each candidate counterpart is shown. Vertical arrows indicate the lower limit on $f_{\rm X}/f_{\rm opt}$ for sources with no candidate optical counterpart down to B_J = 23, V = 24.7 (left) and V = 24.3 (right). The dashed lines at $\log(f_{\rm X}/f_{\rm opt}) = 2$ represent the threshold level for a source to be considered as a possible INS candidate.
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In the text

$\begin{figure} \includegraphics[width=18cm]{5247f10.ps}\end{figure}$ Figure 10: Finding charts of the X-ray sources listed in Table 7. For each source the 5'' radius error circle is superimposed on the corresponding V-band WFI image.
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In the text

$\begin{figure} \par\includegraphics[angle=+90,width=8cm,clip]{5247fig1.ps} \end{figure}$	Figure 1: Galactic distribution of the unidentified $\gamma$ -ray sources from the third EGRET catalogue (Hartman et al. 1999): the two black circles show the positions of 3EG J0616-3310 and 3EG J1249-8330.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5247fig2.ps} \end{figure}$	Figure 2: Processed XMM-Newton EPIC/MOS image of field 4 (see Table 1. Photons selected from three different energy bands are colour-coded: red (0.3-1 keV); green (1-3 keV); blue (3-10 keV).
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$\begin{figure} \par\includegraphics[angle=-90,width=6.3cm,clip]{5247f3a.ps}\hspace*{4mm} \includegraphics[angle=-90,width=6.3cm,clip]{5247f3b.ps} \end{figure}$	Figure 3: Histograms of the source count-rate distributions for each EPIC pointing of the error box of 3EG J0616-3310 (left, N1-N4) and 3EG J1249-8330 (right, N5-N8), in the energy ranges 0.5-2 keV (red line) and 2-10 keV (blue line). For observation 7 the distribution peaks at higher count rate ( $\log CR = -2.35$ ) due to the shorter effective exposure time.
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$\begin{figure} \par\includegraphics[angle=-90,width=6.3cm,clip]{5247f4a.ps}\hspace*{4mm} \includegraphics[angle=-90,width=6.3cm,clip]{5247f4b.ps} \end{figure}$	Figure 4: Histogram of the source S/N distribution for the 3EG J0616-3310 (left, N1-N4) and 3EG J1249-8330 (right, N5-N8) fields.
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$\begin{figure} \par\includegraphics[angle=-90,width=6.1cm,clip]{5247f6a.ps}\hspace*{4mm} \includegraphics[angle=-90,width=6.1cm,clip]{5247f6b.ps}\end{figure}$	Figure 6: The total sky coverage of the EPIC observations of the 3EG J0616-3310 (left) and 3EG J1249-8330 (right) error boxes, in the energy bands 0.5-2 keV (red line) and 2-10 keV (blue line).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5247fig8CMJN.eps}\end{figure}$	Figure 8: Composite BVR image (B = blue; V = green; R = red) of field 4 taken with WFI at the ESO/MPG 2.2 m telescope.
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$\begin{figure} \includegraphics[width=18cm]{5247f10.ps}\end{figure}$	Figure 10: Finding charts of the X-ray sources listed in Table 7. For each source the 5'' radius error circle is superimposed on the corresponding V-band WFI image.
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