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

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Table 2

Best-fitting parameters to model the total intensity phase function and degree of polarization as a function of the scattering angle.

Star	Region	s_min (μm)	s_max (μm)	n	log₁₀(k)
HD 157587	0.70″ ≤ r < 1.10″	${0.03}_{- 0.02}^{+ 0.06}$ $\[0.03_{-0.02}^{+0.06}\]$	$97_{- 84}^{+ 375}$ $\[97_{-84}^{+375}\]$	${3.1}_{- 0.8}^{+ 0.5}$ $\[3.1_{-0.8}^{+0.5}\]$	${0.69}_{- 0.10}^{+ 0.07}$ $\[0.69_{-0.10}^{+0.07}\]$
HD 115600	0.35″ ≤ r < 0.50″	${0.11}_{- 0.07}^{+ 0.06}$ $\[0.11_{-0.07}^{+0.06}\]$	${0.49}_{- 0.13}^{+ 0.14}$ $\[0.49_{-0.13}^{+0.14}\]$	${2.0}_{- 0.7}^{+ 1.1}$ $\[2.0_{-0.7}^{+1.1}\]$	${1.6}_{- 0.3}^{+ 0.2}$ $\[1.6_{-0.3}^{+0.2}\]$
HD 129590	0.30″ ≤ r < 0.50″	${0.36}_{- 0.01}^{+ 0.01}$ $\[0.36_{-0.01}^{+0.01}\]$	$110_{- 52}^{+ 75}$ $\[110_{-52}^{+75}\]$	${4.3}_{- 0.0}^{+ 0.1}$ $\[4.3_{-0.0}^{+0.1}\]$	$- {2.69}_{- 2.28}^{+ 0.40}$ $\[-2.69_{-2.28}^{+0.40}\]$
HD 129590	0.50″ ≤ r < 0.70″	${0.16}_{- 0.03}^{+ 0.02}$ $\[0.16_{-0.03}^{+0.02}\]$	${1.9}_{- 0.3}^{+ 0.4}$ $\[1.9_{-0.3}^{+0.4}\]$	${3.4}_{- 0.1}^{+ 0.1}$ $\[3.4_{-0.1}^{+0.1}\]$	$- {0.04}_{- 0.03}^{+ 0.03}$ $\[-0.04_{-0.03}^{+0.03}\]$
HD 129590	0.70″ ≤ r < 0.90″	${0.48}_{- 0.01}^{+ 0.01}$ $\[0.48_{-0.01}^{+0.01}\]$	${0.96}_{- 0.03}^{+ 0.03}$ $\[0.96_{-0.03}^{+0.03}\]$	${3.2}_{- 0.1}^{+ 0.1}$ $\[3.2_{-0.1}^{+0.1}\]$	${0.03}_{- 0.02}^{+ 0.02}$ $\[0.03_{-0.02}^{+0.02}\]$
HD 129590	0.90″ ≤ r < 1.10″	${0.25}_{- 0.04}^{+ 0.21}$ $\[0.25_{-0.04}^{+0.21}\]$	${1.2}_{- 0.4}^{+ 0.2}$ $\[1.2_{-0.4}^{+0.2}\]$	${2.4}_{- 0.1}^{+ 0.1}$ $\[2.4_{-0.1}^{+0.1}\]$	$- {0.11}_{- 0.04}^{+ 0.07}$ $\[-0.11_{-0.04}^{+0.07}\]$

Notes. The second column shows the results for different annuli for HD 129590 (see text for details).

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