Why circumstellar disks are so faint in scattered light: the case of HD 100546

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Table 1

Fitting parameters to the geometric albedo of the disk, used to derive the disk albedo (Fig. 6).


Grains	Filter
	F435W	F814W	F160W	F222M

Large	0.0059 [1.1]	0.011 [1.3]	0.020 [1.1]	0.037 [1.0]
Medium	0.075 [2.0]	0.084 [1.0]	0.079 [0.7]	0.048 [0.6]
Small	0.052 [0.8]	0.025 [0.5]	0.0067 [0.7]	0.0024 [0.5]

Observed	0.0062 [1.0]	0.009 [0.7]	0.024 [1.2]	0.033 [1.3]

Notes. Displayed is ω_filt [q] , calculated by fitting a power law of the form ω_filt·(r)^−q to ω_disk(r) (Eq. (3)). The values given are for models with the same grain sizes and wavelengths as in Fig. 5, and for the observed images.

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