The near-infrared degree of polarization in debris disks - Toward a self-consistent approach to model scattered light observations

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Table B.1

Results of the geometric modeling of the observations, ordered by increasing distance from earth.

Star	d_* [pc]	a₀ [″]	i [°]	ϕ [°]	α_in	α_out	ψ [10⁻³ rad]	γ	$χ_{r}^{2}$ $\[\chi_{\mathrm{r}}^2\]$
HD 191089	50.11 ± 0.05	0.88 ± 0.02	61.3 ± 0.3	−108.0 ± 0.3	8.7 ± 0.7	−3.4 ± 0.2	46 ± 19	5.21 ± 2.74	0.23
HD 157587	99.87 ± 0.23	0.79 ± 0.03	70.1 ± 0.3	−50.7 ± 0.3	9.7 ± 0.3	−2.9 ± 0.1	15 ± 11	5.79 ± 2.93	0.25
HD115600	109.04 ± 0.25	0.45 ± 0.02	76.6 ± 0.3	−156.0 ± 0.2	2.2 ± 0.2	−6.0 ± 0.2	132 ± 4	8.32 ± 1.52	1.04
HD129590	136.32 ± 0.44	0.35 ± 0.02	82.0 ± 0.2	−60.6 ± 0.3	32.4 ± 2.5	−1.8 ± 0.1	1 ± 1	9.70 ± 0.23	1.27

Notes. The columns show the stellar names, the distance, the reference radius a₀, the inclination i, position angle ϕ, inner and outer slopes of the density distribution (α_in and α_out, respectively), opening angle ψ, the exponential fall-off γ, and the reduced χ².

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