Table 3: Residual intensities $I_{\rm res}$ in the artificial diffraction-limiteda and the SOT observationsb.
$I_{\rm res}$ [%]   450 nm 555 nm 668 nm
Mercury disc-centre (r = 5  $^{\prime \prime }$)
r = 5  $^{\prime \prime }$ observed $7.0 \pm 0.7$ $10.3 \pm 0.2$ $11.3 \pm 0.5$
  theoret. 1.8 2.2 2.6
  difference $5.2 \pm 0.7$ $8.1 \pm 0.2$ $8.7 \pm 0.5$
Total eclipse, different distances r from lunar limb
r = 5  $^{\prime \prime }$ observed $2.9 \pm 0.4$ $4.7 \pm 1.5$ $5.3 \pm 1.5$
  theoret. 0.6 0.7 0.8
  difference $2.3 \pm 0.4$ $4.0 \pm 1.5$ $4.5 \pm 1.5$
r = 10  $^{\prime \prime }$ observed $2.3 \pm 0.3$ $4.2 \pm 1.5$ $4.7 \pm 1.5$
  theoret. 0.3 0.3 0.4
  difference $2.0 \pm 0.3$ $3.9 \pm 1.5$ $4.3 \pm 1.5$
r = 20  $^{\prime \prime }$ observed $1.9 \pm 0.2$ $3.8 \pm 1.4$ $4.4 \pm 1.4$
  theoret. 0.2 0.2 0.3
  difference $1.7 \pm 0.2$ $3.6 \pm 1.4$ $4.1 \pm 1.4$
a All theoretical values are corrected for the influence of the far PSF wings at different distances from the terminator (see Sect. 4.1.1). b The difference between both is due to contributions not included in the ideal PSFs, e.g., stray-light inside the telescope.

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