Revealing the sub-AU asymmetries of the inner dust rim in the disk around the Herbig Ae star R Coronae Austrinae

Table 2:

Model-fitting results.
	Compact component									Extended component		Goodness-of-fit
Model	$\theta_{1}$	f	$\rho$	$\phi^{(a)}$	i	s	R	H/R	$\epsilon$	$\theta_{\rm 2}$	$I_{\rm 2}/I_{\rm 1}$	$\chi^{2}_{r,V}$	$\chi^{2}_{r,\Phi}$	$\chi^{2}_{r}$
	[mas]		[mas]	[ $\ifmmode^\circ\else^\circ\fi$ ]	[ $\ifmmode^\circ\else^\circ\fi$ ]		[AU]			[mas]
	Point-symmetric models:
UD	13.86											24.82	29.32^(c)	25.92
RING	8.92	0.25^(b)										26.38	29.32^(c)	25.21
GAUSS	8.55											18.16	29.32^(c)	20.88
2-GAUSS	5.77									25.78	0.59	2.35	29.32^(c)	8.92
	Asymmetric models:
BINARY	4.8		6.2	34						14.8	1.04	3.47	5.32	3.93
SKEWED RING		0.8		190	14	0.64	0.44			27	0.58	1.58	3.13	1.96
VERTICAL RIM				132	16		0.60	0.35		27	0.68	2.30	6.16	3.25
CURVED RIM				180	35				$\epsilon_{\rm cr}$	32	0.50	1.77	3.28	2.14

Notes. ^(a) This column gives the model orientation, measured East of North. For the BINARY model, $\phi$ gives the PA of the separation vector, while for the SKEWED RING, VERTICAL RIM, and CURVED RIM models, the orientation of the ellipse/rim major axis is given. Due to a lack of closure phase calibration observations on the E0-G0-H0 array configuration, we are unfortunately not able to unambiguously define the CP sign, resulting in a 180 $\ifmmode^\circ\else^\circ\fi$ -ambiguity in the derived position angles. ^(b) In the fitting process, this parameter was fixed. ^(c) This model is point-symmetric, resulting in a CP which is identical zero.

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