Silicate features in Galactic and extragalactic post-AGB discs

C. Gielen; J. Bouwman; H. Van Winckel; T. Lloyd Evans; P. M. Woods; F. Kemper; M. Marengo; M. Meixner; G. C. Sloan; A. G. G. M.  Tielens

doi:doi:10.1051/0004-6361/201117364

Issue		A&A Volume 533, September 2011


Article Number		A99
Number of page(s)		26
Section		Interstellar and circumstellar matter
DOI		http://dx.doi.org/10.1051/0004-6361/201117364
Published online		07 September 2011

Online material

Appendix A: Figures and Tables

	Fig. A.1 Left: the 14 μm complex for the Galactic sources, continuum subtracted and normalised. Overplotted in red the mean spectrum. The mass absorption coefficients of forsterite and enstatite are plotted in green and blue. The high noise level on the LMC sources did not allow for a mean spectrum determination. Right: same as on the left, but for the 16 μm complex.
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	Fig. A.2 Left: the 19 μm complex for the Galactic sources, continuum subtracted and normalised. Overplotted in red the mean spectrum. The mass absorption coefficients of forsterite and enstatite are plotted in green and blue. Right: same as on the left, but for the LMC sources. The top panel shows the comparison between the calculated mean for the LMC and Galactic sources.
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	Fig. A.3 Same as Fig. A.2, but for the 23 μm complex.
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	Fig. A.4 Same as Fig. A.2, but for the 27 μm complex.
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	Fig. A.5 Same as Fig. A.2, but for the 33 μm complex.
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Fig. A.6

Best model fits for our Galactic sample stars, showing the contribution of the different dust species. Top: the observed spectrum (black curve) is plotted together with the best model fit (red curve) and the continuum (black solid line). Forsterite is plotted in green, enstatite in blue, silica in cyan and amorphous olivine and pyroxene in magenta. Small grains (0.1 μm) are plotted as dashed lines and larger grains (2 and 4 μm) as dotted lines. Bottom: the normalised residuals after subtraction of our best model of the observed spectra.

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	Fig. A.6 continued.
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	Fig. A.6 continued.
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Fig. A.7

Best model fits for our LMC sample stars, showing the contribution of the different dust species. Top: the observed spectrum (black curve) is plotted together with the best model fit (red curve) and the continuum (black solid line). Forsterite is plotted in green, enstatite in blue, silica in cyan and amorphous olivine and pyroxene in magenta. Small grains (0.1 μm) are plotted as dashed lines and larger grains (2 and 4 μm) as dotted lines. Bottom: the normalised residuals after subtraction of our best model of the observed spectra.

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	Fig. A.7 continued.
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Fig. A.8

Left: the mass fraction in crystalline grains versus the forsterite fraction in the crystalline material. Right: the mean size of crystalline grains versus the enstatite fraction in the crystalline material. Galactic sources are given in red plus signs and LMC sources in blue diamonds. The magenta symbols depict Galactic sources for which the infrared spectra only start from 9.9 μm. The numbers correspond to numbers given in Tables 1 and 2.

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Fig. A.9

Left: the mean size of crystalline grains versus the mean size of amorphous grains. Right: the mean size of the crystalline grains versus crystallinity fraction. Galactic sources are given in red plus signs and LMC sources in blue diamonds. The magenta symbols depict Galactic sources for which the infrared spectra only start from 9.9 μm. The numbers correspond to numbers given in Tables 1 and 2.

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	Fig. A.10 The mean size of the amorphous grains versus the disc flaring, determined by the F₂₄/F₈ flux ratio. Galactic sources are given in red plus signs and LMC sources in blue diamonds. The magenta symbols depict Galactic sources for which the infrared spectra only start from 9.9 μm. The numbers correspond to numbers given in Tables 1 and 2.
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Table A.1

Best fit parameters deduced from our full spectral fitting.

Table A.2

Best fit parameters deduced from our full spectral fitting.

Table A.3

Best fit parameters deduced from our full spectral fitting.

© ESO, 2011

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