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Table 3:

Erratum for Table 3 in Gielen et al. (2009a): best-fit parameters deduced from our full spectral fitting.

$\chi^2$ $T_{\rm\rm dust1}$ $T_{\rm\rm dust2}$ Fraction $T_{\rm\rm cont1}$ $T_{\rm\rm cont2}$ Fraction
    (K) (K) $T_{\rm\rm dust1}{-}T_{\rm\rm dust2}$ (K) (K) $T_{\rm\rm cont1}-T_{\rm\rm cont2}$

EP Lyr
5.4 $ 100_{\rm 50}^{ 50}$ $ 200_{\rm 50}^{ 50}$ $ 0.90_{\rm0.05}^{0.10}{-}0.10_{\rm0.10}^{0.05}$ $ 100_{\rm 50}^{ 50}$ $ 643_{\rm 50}^{302}$ $ 0.98_{\rm0.04}^{0.01}{-}0.02_{\rm0.01}^{0.04}$
HD 52961 50.0 $ 200_{\rm 50}^{ 50}$ $ 700_{\rm 50}^{50}$ $ 0.90_{\rm0.05}^{ 0.05}{-}0.10_{\rm0.05}^{ 0.05}$ $ 100_{\rm 50}^{ 50}$ $1000_{\rm 50}^{ 50}$ $ 0.99_{\rm0.01}^{ 0.01}{-}0.01_{\rm0.01}^{ 0.01}$

Olivine Pyroxene Forsterite Enstatite Continuum
  small-large small-large small-large small-large  

EP Lyr
$ 0.24_{\rm0.24}^{16.83}{-}8.74_{\rm 7.64}^{7.92}$ $7.17_{\rm 4.79}^{13.69}{-}8.09_{\rm 7.24}^{12.67}$ $35.18_{\rm 2.78}^{3.04}{-}2.08_{\rm 1.89}^{2.61}$ $ 0.00_{\rm0.00}^{0.00}{-}38.50_{\rm 3.46}^{4.30}$ $57.99_{\rm 3.60}^{2.53}$

HD 52961

$ 0.00_{\rm0.00}^{ 0.00}{-}0.00_{\rm0.00}^{ 0.00}$ $59.17_{\rm0.69}^{0.72}{-}0.00_{\rm0.00}^{0.00}$ $0.77_{\rm0.69}^{1.46} {-} 40.06_{\rm 1.62}^{1.02}$ $ 0.00_{\rm0.00}^{ 0.00}{-}0.00_{\rm0.00}^{ 0.00}$ $68.88_{\rm0.46}^{0.42}$

Notes. Listed are the $\chi^2$, dust, and continuum temperatures and their relative fractions. Best-fit parameters deduced from our full spectral fitting. The abundances of small and large grains of the various dust species are given as fractions of the total mass, excluding the dust responsible for the continuum emission. The last column gives the continuum flux contribution, listed as a percentage of the total integrated flux over the full wavelength range.

Source LaTeX | All tables | In the text

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