Analysis of the infrared spectra of the peculiar post-AGB stars EP Lyrae and HD 52961

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This article has an erratum: [https://doi.org/10.1051/0004-6361/200912982e]

Table 2:

$\chi ^2$ values for different models used in our full spectral fitting.
	EP Lyr	HD 52961	model description
	$\chi ^2$	$\chi ^2$
model1	21.7	129.4	Mie - 0.1-2.0 $\mu$ m - x=0.5
model2	6.2	67.5	DHS - 0.1-1.5 $\mu$ m - x=0.5
model3	6.2	63.8	DHS - 0.1-1.5 $\mu$ m - x=1.0
model4	8.4	101.4	DHS - 1.5-3.0 $\mu$ m - x=0.5
model5	8.6	140.8	DHS - 1.5-3.0 $\mu$ m - x=1.0
model6	5.9	64.2	GRF - 0.1-2.0 $\mu$ m - x=0.5
model7	6.3	50.0	GRF - 0.1-2.0 $\mu$ m - x=1.0
model8	5.8	96.5	GRF - 2.0-4.0 $\mu$ m - x=0.5
model9	5.4	72.2	GRF - 2.0-4.0 $\mu$ m - x=1.0

Note: For each model we give the used dust approximation, grain size and Mg-Fe content in the amorphous grains. x=1.0 denotes pure Mg-rich amorphous dust, x=0.5 the more standard Mg-Fe amorphous silicates.

Source LaTeX | All tables | In the text

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