All Figures

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{9685fig1.eps}\end{figure}$ Figure 1: The top figure is the longitude profile of all photon counts observed by EGRET above 100 MeV at all latitudes (black error bars), compared with the diffuse counts predicted by the 3EG model (blue curve) and the Ring model (red curve). The bottom figure is the residual expressed in number of standard deviation, colors are the same as above, we added the Galprop residuals in purple. Counts from bright sources have been added to the diffuse component. For more visibility the plot are presented with a binning of 4 $^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig2.eps} . \end{figure}$ Figure 2: Map in Galactic coordinates of the residuals (expressed in $\sigma = \sqrt {N_{\rm pred}}$ values) between the E > 100 MeV photon counts (in 0.5 $^{\circ }$ bin) and the best-fit Ring model solution given by Eq. (1).
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig3.eps}\end{figure}$ Figure 3: An example of the iterative source detection with the 2D binned likelihood around Geminga at energies above 100 MeV. 4 consecutive TS maps are shown. Sources are detected, then are included in the background for the next step until no significant one is left. The colourbar gives TS.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig4.eps}\end{figure}$ Figure 4: Spatial distribution, in Galactic coordinates, of the EGR sources. The confused sources are marked as open circles.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig5.eps}\end{figure}$ Figure 5: Spatial distribution, in Galactic coordinates, of the 3EG sources.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig6.eps}\end{figure}$ Figure 6: Spatial distribution, in Galactic coordinates, of the 3EG sources with no counterpart in EGR: the unidentified sources as circles and the identified AGN as stars. The filled circles and stars mark the sources that were flagged as extended or confused in the 3EG catalogue.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig7.eps}\end{figure}$ Figure 7: Spatial distribution, in Galactic coordinates, of the new EGR sources with no 3EG counterpart. The confused sources are marked as open circles.
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In the text

$\begin{figure} \includegraphics[width=9cm,clip]{9685fi15.ps}\end{figure}$ Figure 8: Second stage of the iterative source detection around Geminga (see Fig. 3) obtained using the 3EG model ( left) and map of the Ring model intensity divided by the 3EG one ( right). The excess in the TS map assigned in 3EG to the 3EG J0556+0409 point source corresponds to a local underestimation of the diffuse emission in the 3EG model. Maps are given in 0.5 $^{\circ }$ bins and galactic coordinates.
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In the text

$\begin{figure} \par\resizebox{7cm}{5cm}{\includegraphics{9685fig8.eps}}\end{figure}$ Figure 9: Histogram of the relative flux differences $\vert F_{\rm EGR} - F_{\rm 3EG}\vert / \sigma _{F_{\rm EGR}}$ measured between the EGR and 3EG counterparts in units of the statistical error on flux for each source. All fluxes are measured above 100 MeV.
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In the text

$\begin{figure} \par\resizebox{7cm}{5cm}{\includegraphics{9685fig9.eps}}\end{figure}$ Figure 10: Histogram of the relative angular separation between the positions found for the EGR and 3EG counterparts in units of the 95% confidence angle for each source.
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In the text

$\begin{figure} \par\resizebox{7cm}{5cm}{ \includegraphics{9685fi10.eps}}\end{figure}$ Figure 11: Histogram of the relative flux differences $\vert F_{\rm EGR}-F_{\rm sys}\vert/ \sigma _{F_{\rm EGR}}$ measured with the Ring and Galprop models in units of the statistical error in flux for each source. All fluxes are measured above 100 MeV.
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In the text

$\begin{figure} \resizebox{7cm}{5cm}{\includegraphics{9685fi11.eps}} \end{figure}$ Figure 12: Histogram of the relative angular separation between the positions found with the Ring and Galprop models in units of the 95% confidence angle for each source.
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In the text

$\begin{figure} \includegraphics[width=14cm,clip]{9685fi12.eps} \end{figure}$ Figure 13: The revised EGRET source catalog, shown in Galactic coordinates. The symbols indicate the counterpart types found in the error box: identified pulsars as black squares; other ATNF pulsars as open squares; LSI +61 303, LMC, and solar flare as black triangles; ASDC and CGRaBS blazar candidates as black diamonds; other flat-spectrum radiosources from CRATES as open diamonds; supernova remnants from the Green catalogue as stars; no counterpart as crosses.
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In the text

$\begin{figure} \resizebox{6.8cm}{4.8cm}{\includegraphics{9685fi13.eps}} \end{figure}$ Figure 14: Latitude distribution of the EGR sources with young Galactic sources at $\vert b\vert <3^{\circ }$ , nearly isotropically distributed sources far from the plane, as expected from the black curve, and a flattening at mid-latitude because of the rapid increase in the interstellar background flux.
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In the text

$\begin{figure} \resizebox{7.8cm}{5.8cm}{\includegraphics{9685fi14.eps}} \end{figure}$ Figure 15: TS-map obtained at energies above 1 GeV toward the Galactic centre above the 3EG a) and Ring b) interstellar model
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In the text

$\begin{figure} \resizebox{7.2cm}{5.2cm}{\includegraphics{0028.eps}} \end{figure}$ Figure 16: Likelihood TS contours for energies above 100 MeV and periods incompassing PSR J0030+0451. The cross, the plus sign and the black dot respectively mark the EGR catalog position, the position with maximum likelihood and the pulsar location.
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In the text

$\begin{figure} \resizebox{7.2cm}{5.2cm}{\includegraphics{3c345.eps}} \end{figure}$ Figure 17: Likelihood TS contours (50%, 68%, 95% and 99% confidence) for energies above 100 MeV and period 5190. The cross is the EGR catalog position, the plus sign the position with maximum likelihood and the black dots mark the radio positions of 3C345, Mrk 501, and 4C+38.41.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig2.eps} . \end{figure}$	Figure 2: Map in Galactic coordinates of the residuals (expressed in $\sigma = \sqrt {N_{\rm pred}}$ values) between the E > 100 MeV photon counts (in 0.5 $^{\circ }$ bin) and the best-fit Ring model solution given by Eq. (1).
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig3.eps}\end{figure}$	Figure 3: An example of the iterative source detection with the 2D binned likelihood around Geminga at energies above 100 MeV. 4 consecutive TS maps are shown. Sources are detected, then are included in the background for the next step until no significant one is left. The colourbar gives TS.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig4.eps}\end{figure}$	Figure 4: Spatial distribution, in Galactic coordinates, of the EGR sources. The confused sources are marked as open circles.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig5.eps}\end{figure}$	Figure 5: Spatial distribution, in Galactic coordinates, of the 3EG sources.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig6.eps}\end{figure}$	Figure 6: Spatial distribution, in Galactic coordinates, of the 3EG sources with no counterpart in EGR: the unidentified sources as circles and the identified AGN as stars. The filled circles and stars mark the sources that were flagged as extended or confused in the 3EG catalogue.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9685fig7.eps}\end{figure}$	Figure 7: Spatial distribution, in Galactic coordinates, of the new EGR sources with no 3EG counterpart. The confused sources are marked as open circles.
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$\begin{figure} \par\resizebox{7cm}{5cm}{\includegraphics{9685fig8.eps}}\end{figure}$	Figure 9: Histogram of the relative flux differences $\vert F_{\rm EGR} - F_{\rm 3EG}\vert / \sigma _{F_{\rm EGR}}$ measured between the EGR and 3EG counterparts in units of the statistical error on flux for each source. All fluxes are measured above 100 MeV.
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$\begin{figure} \par\resizebox{7cm}{5cm}{\includegraphics{9685fig9.eps}}\end{figure}$	Figure 10: Histogram of the relative angular separation between the positions found for the EGR and 3EG counterparts in units of the 95% confidence angle for each source.
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$\begin{figure} \par\resizebox{7cm}{5cm}{ \includegraphics{9685fi10.eps}}\end{figure}$	Figure 11: Histogram of the relative flux differences $\vert F_{\rm EGR}-F_{\rm sys}\vert/ \sigma _{F_{\rm EGR}}$ measured with the Ring and Galprop models in units of the statistical error in flux for each source. All fluxes are measured above 100 MeV.
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$\begin{figure} \resizebox{7cm}{5cm}{\includegraphics{9685fi11.eps}} \end{figure}$	Figure 12: Histogram of the relative angular separation between the positions found with the Ring and Galprop models in units of the 95% confidence angle for each source.
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$\begin{figure} \resizebox{6.8cm}{4.8cm}{\includegraphics{9685fi13.eps}} \end{figure}$	Figure 14: Latitude distribution of the EGR sources with young Galactic sources at $\vert b\vert <3^{\circ }$ , nearly isotropically distributed sources far from the plane, as expected from the black curve, and a flattening at mid-latitude because of the rapid increase in the interstellar background flux.
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$\begin{figure} \resizebox{7.8cm}{5.8cm}{\includegraphics{9685fi14.eps}} \end{figure}$	Figure 15: TS-map obtained at energies above 1 GeV toward the Galactic centre above the 3EG a) and Ring b) interstellar model
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$\begin{figure} \resizebox{7.2cm}{5.2cm}{\includegraphics{0028.eps}} \end{figure}$	Figure 16: Likelihood TS contours for energies above 100 MeV and periods incompassing PSR J0030+0451. The cross, the plus sign and the black dot respectively mark the EGR catalog position, the position with maximum likelihood and the pulsar location.
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$\begin{figure} \resizebox{7.2cm}{5.2cm}{\includegraphics{3c345.eps}} \end{figure}$	Figure 17: Likelihood TS contours (50%, 68%, 95% and 99% confidence) for energies above 100 MeV and period 5190. The cross is the EGR catalog position, the plus sign the position with maximum likelihood and the black dots mark the radio positions of 3C345, Mrk 501, and 4C+38.41.
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