Fig. A.5
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Distribution of the average count rates of sources in the SEP field, in eRASS1, 2, and 3. The average count rates were determined by Eq. A.3. Due to the high exposures in the SEP field, eROSITA could detect sources at much lower count rates than in the rest of the sky. This figure does not show the six sources with a slightly negative average count rate.
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