Table 4: Preliminary orbital solutions, dynamical parallaxes, and system masses for $\theta ^1$ Ori C.
Orbit #1 Orbit #2

P [yrs] 10.98 10.85

T 1996.52 1996.64

e 0.909 0.925

a [mas] 41.3 45.0

i [ $^\circ$ ] 105.2 103.7

$\Omega$ [ $^\circ$ ] 56.5 56.9

$\omega$ [ $^\circ$ ] 65.7 68.2

$\chi^2/\textnormal{dof}$ 1.61 1.59

$\pi_{\rm dyn}^{a)}$ [mas] $2.304 \pm 0.066$ $2.585 \pm 0.074$

$d_{\rm dyn}^{a)}$ [pc] $434 \pm 12$ $387 \pm 11$

$(M_{\rm C1}+M_{\rm C2})^{a)}$ [ $M_{\odot}$ ] $47.8 \pm 4.2$ $44.8 \pm 3.9$

^a The errors on the dynamical parallaxes and corresponding distances were estimated by varying the measured binary flux ratio within the observational uncertainties, the assumed spectral types for the bolometric correction by one sub-class, the extinction by ${\pm} 0.2$ mag, and by using three different MLRs (by Demircan & Kahraman 1991; Heintz 1978; Baize & Romani 1946). However, the given errors do not reflect the uncertainties on the orbital elements a and P. Due to the presence of the multiple orbital solutions, it is currently not possible to quantify these errors reliably.

**Table 4:** Preliminary orbital solutions, dynamical parallaxes, and system masses for $\theta ^1$ Ori C.
		Orbit #1	Orbit #2
P	[yrs]	10.98	10.85
T		1996.52	1996.64
e		0.909	0.925
a	[mas]	41.3	45.0
i	[ $^\circ$ ]	105.2	103.7
$\Omega$	[ $^\circ$ ]	56.5	56.9
$\omega$	[ $^\circ$ ]	65.7	68.2
$\chi^2/\textnormal{dof}$		1.61	1.59
$\pi_{\rm dyn}^{a)}$	[mas]	$2.304 \pm 0.066$	$2.585 \pm 0.074$
$d_{\rm dyn}^{a)}$	[pc]	$434 \pm 12$	$387 \pm 11$
$(M_{\rm C1}+M_{\rm C2})^{a)}$	[ $M_{\odot}$ ]	$47.8 \pm 4.2$	$44.8 \pm 3.9$

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