Issue 
A&A
Volume 584, December 2015



Article Number  L10  
Number of page(s)  5  
Section  Letters  
DOI  https://doi.org/10.1051/00046361/201527563  
Published online  02 December 2015 
Online material
Appendix A: Grain size fitting
In order to calculate the maximum likelihood grainsize distribution, we compute the scattering and polarising properties of a grid of dust models under the assumption of Mie scattering (Mie 1908) by bare, compact spheres, which allows us to fit the observations under the assumption of single scattering. We assume a grain size distribution of the form , where a is the grain radius and is the number density of grains with radius a. The lower (a_{min}) and upper (a_{max}) size limits are free parameters, and the exponent of the grain size distribution is fixed to q = 3.5. For each size distribution, we calculate the scattering and absorbtion crosssections, and the components of the Müller matrix at one degree intervals, for each wavelength for which we wish to fit observations.
The polarisation fraction at each wavelength is completely determined by the elements of the Müller matrix, such that p(λ,θ) = S_{12}(λ,θ)/S_{11}(λ,θ), where p is the polarisation fraction, λ is the wavelength of interest, θ is the scattering angle, and S_{ij} are the elements of the Müller matrix.
The ratio of the scattered intensities at any pair of wavelengths is determined by the scattering phase function, contained within S_{11}, and the ratio of the scattering efficiencies, i.e. (A.1)where F_{∗} is the flux emitted by the star and Q_{sca} are the scattering efficiencies. For each grainsize distribution, we calculate the likelihood where Δ is a vector of observations such that Δ_{i} is the ith observation and σ_{Δi} its associated uncertainty, M_{i} is the output of the model associated with the ith observation, and Θ is a vector of model parameters (in our case ). The maximumlikelihood model is then defined to be the model with parameters Θ that maximises the value of , and Θ contains the information in which we are interested.
For the sake of efficiency, it is common to compute the loglikelihood by taking only the exponent.
By calculating a grid of grainsize distributions with 5 nm <a_{min} ≤ 1μm and 100 nm <a_{max} ≤ 50 μm we cover the full range of grain sizes observed in the interstellar medium and in the circumstellar environments of evolved stars. The resulting likelihood space for the S Knot is shown in Fig. A.1, zoomed to show the region of interest.
Fig. A.1
Likelihood space for scattering angle of 63°, corresponding to the S Knot, zoomed to show grain sizes in the range 0.1−3 μm. 

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The average size of the maximumlikelihood distribution is calculated simply from which can be solved analytically.
Because the scattering properties are determined by the real part of the complex refractive index of the grain material, which is similar for all of the plausible choices, the optical properties are dominated by the grain size for a ~ λ, rather than the choice of silicate material.
© ESO, 2015
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