The Araucaria project: High-precision orbital parallaxes and masses of binary stars - I. VLTI/GRAVITY observations of ten double-lined spectroscopic binaries

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Table 8.

Additional information about the systems and their detection with Gaia.

Star	RUWE	a_phot	S/N
		(mas)
TZ For	1.3	0.257	7.5	−4.1
AI Phe	1.1	0.035	1.0	−0.6
AL Dor	1.0	0.005	0.1	0.6
KW Hya	1.3	0.306	8.9	−3.2
NN Del	1.2	0.338	9.9	1.7
ψ Cen	3.1	1.153	33.7	−0.6
AK For	1.1	0.257	7.5	−0.6
HD 9312	2.7	1.488	43.5	−1.8
HD 41255	1.0	−0.007	−0.2	2.1
HD 70937	1.2	0.361	10.6	−0.7
HD 210763	1.0	0.539	15.8	2.3
HD 224974	1.1	0.095	2.8	2.1
HD 188088	1.2	−0.545	−15.9	3.0
LL Aqr	1.1	0.189	5.5	0.9
o Leo	3.2	0.655	19.2	0.7
V963 Cen	1.0	0.011	0.3	0.8

Notes. #2: RUWE parameter as estimated by the Gaia team. #3: estimated photocentre semi-major axis (Eq. (3)). #4: signal-to-noise ratio to detect the astrometric signature (Eq. (4)). #5: relative difference with our measured orbital parallax.

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