High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP) - I. Lucky imaging observations of 101 systems in the southern hemisphere

D. F. Evans; J. Southworth; P. F. L. Maxted; J. Skottfelt; M. Hundertmark; U. G. Jørgensen; M. Dominik; K. A. Alsubai; M. I. Andersen; V. Bozza; D. M. Bramich; M. J. Burgdorf; S. Ciceri; G. D’Ago; R. Figuera Jaimes; S.-H. Gu; T. Haugbølle; T. C. Hinse; D. Juncher; N. Kains; E. Kerins; H. Korhonen; M. Kuffmeier; L. Mancini; N. Peixinho; A. Popovas; M. Rabus; S. Rahvar; R. W. Schmidt; C. Snodgrass; D. Starkey; J. Surdej; R. Tronsgaard; C. von Essen; Yi-Bo Wang; O. Wertz

doi:10.1051/0004-6361/201527970

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A&A, 589 (2016) A58

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Table 9

The preferred models of relative motions for candidate companions with previous astrometric measurements.

Target	Comp.	Preferred Model	Significance

CoRoT-2	1	CPM	0.4σ
CoRoT-3	1	CPM¹	0.7σ
CoRoT-3	2	CPM²	0.1σ
CoRoT-11	1	CPM	0.8σ
HAT-P-30	Near	CPM	>5.0σ
HAT-P-30	Far	BG	0.6σ
HAT-P-41	1	CPM	2.0σ
WASP-2	1	CPM	>5.0σ
WASP-8	1	CPM	>5.0σ
WASP-36	1	CPM	0.1σ
WASP-70	1	CPM	>5.0σ
WASP-77	1	CPM	>5.0σ

Notes. The Common Proper Motion model (CPM) assumes that the two stars have the same proper motion and parallax; the Background model (BG) is based on the candidate companion being a distant background star with negligible proper motion and parallax. Results significant by more than 1.0σ are highlighted in the table.

⁽¹⁾

NOMAD and PPMXL give significantly different proper motions to UCAC4 for CoRoT-3; the CPM model is preferred at 4.3σ using NOMAD, and at 2.3σ PPMXL proper motions. The results for companion 2 are unchanged.

⁽²⁾

NOMAD gives a significantly different proper motion to UCAC4 for CoRoT-11; the CPM model is preferred at 3.5σ using NOMAD.

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