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Table 3:

The results of decomposing the $I_{\rm sh}$ AARP data into shell brightness distributions.
Filter Shell $I_{{\rm peak}}$ $F_{{\rm tot}}$a ${S_{{\rm av}}}$ ${F_{{\rm sc}}} / {F_{\star}}$b
    [ $10^{-16}~{\rm erg~s^{-1}~cm^{-2}~\hbox{$^{\prime\prime}$ }^{-2}}$] [ $10^{-13}~{\rm erg~s^{-1}~cm^{-2}}$] [ $10^{-14}~{\rm erg~s^{-1}~cm^{-2}~\AA^{-1} }$] [10-4]
Str y 3 5.7 16.1 0.9 4.1
  4 14.2 80.1 4.4 20.1
  total   144.4 7.9 36.3
F59 3 8.7 20.5 (19%) 3.9 20.5
  4 4.0 24.2 (83%) 4.6 24.2
  total   84.7 (43%) 16.3 84.7
H$\alpha $ 3 2.4 6.6 0.5 1.6
  4 6.1 34.9 2.8 8.3
  total   68.2 5.5 16.3
F77 3   14.0 (3%) 2.8 3.3
  4   3.3 (100%) 0.7 0.8
  total   30.0 (50%) 6.0 7.1

Notes. The columns give the peak intensity, total flux, and average flux density of the shell brightness distribution fits ( $I_{{\rm peak}}$, $F_{{\rm tot}}$, and  ${S_{{\rm av}}}$, respectively), and the ratio between the circumstellar and stellar fluxes ( ${F_{{\rm sc}}} / {F_{\star}}$).
(a) The values for the total of all shells are obtained by integrating the observed brightness distributions. The numbers within brackets in the F59 and F77 filters give the percentage of flux that may come from dust, based on a linear inter- and extrapolation between the Str-y and H$\alpha $ filters.
(b) The fluxes of the star in the filters are: 4.0 $\times$ $10^{-9}~{\rm erg~s^{-1}~cm^{-2}}$ (Str y), 1.1 $\times$ $10^{-9}~{\rm erg~s^{-1}~cm^{-2}}$ (F59), 4.2 $\times$ $10^{-9}~{\rm erg~s^{-1}~cm^{-2}}$ (H$\alpha $), and 4.2 $\times$ $10^{-9}~{\rm erg~s^{-1}~cm^{-2}}$ (F77).


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