Fig. 6
Top panels: luminosity/sr radiated in our direction from the stellar GRXE and the scattered GRXE component (including stellar and XBs contributions) in the 3−20 keV range integrated over the longitude range (l< | 180°|) and latitude range − b to b. The difference in the scale height of the scattered component compared with a GRXE of stellar origin is clearly visible. Bottom panels: ratio of the two profiles. The peak in the ratio profile is caused by the elevation of the Sun above the Galactic plane by 15 pc.
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