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Fig. A.3

image

PSF fitting test with a variable PSF, complex, extended emission from gas/dust, and diffuse emission from a population of unresolved faint stars. Left: point-source subtracted image after use of a variable PSF. The grey scale is expressed in terms of σ deviations from the noise image. Middle: residual image, after subtracting the input distribution of diffuse emission. Right: background as function of distance from Sgr A* as measured in the residual image. The dashed red line is the power-law cusp used as input. The grey scales are expressed in terms of σ deviations from the noise image. We note that the scales are different from the ones used in in Fig. A.2.

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