A near-infrared interferometric survey of debris-disc stars - VI. Extending the exozodiacal light survey with CHARA/JouFLU

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Volume 608 (December 2017)

A&A, 608 (2017) A113

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Table 3

Circumstellar emission level for the exozodi survey.

HD	Name	Type	K	Baseline	f_cse(%)

5015	HR 244	F9V	3.54	S1-S2	0.61 ± 0.83	1.79	1.68
5448	37 And	A5V	3.5	S1-S2	2.64 ± 0.53	0.716	5.24
6961	θ Cas	A7V	3.97	S1-S2	0.64 ± 0.67	3.4	2.91
10780	V987 Cas	K0V	3.84	S1-S2	2.34 ± 0.89	3.42	3.47
14055	γ Tri	A1Vnn	3.96	E1-E2	−1.39 ± 1.08	0.891	1.67
15335	13 Tri	G0V	4.48	E1-E2	0.60 ± 1.41	0.651	0.51
19373	ι Per	F9.5V	2.68	S1-S2	−0.36 ± 0.28	2.267	2.12
20630	κ1 Cet	G5Vv	3.34	E1-E2	1.39 ± 1.03	0.83	1.08
23249	δ Eri	K1III-IV	1.43	E1-E2	1.40 ± 0.77	0.092	1.75
26965	40 Eri	K0.5V	2.498	S1-S2	0.01 ± 0.76	1.94	1.39
28355	79 Tau	A7V	4.55	E1-E2	−0.86 ± 1.23	4.157	3.16
33111	β Eri	A3IV	2.38	S1-S2	3.21 ± 0.37	6.35	17.67
34411	λ Aur	G1.5IV-V	3.27	E1-E2	0.25 ± 0.56	0.525	0.48
50635	38 Gem	F0Vp	3.89	E1-E2	2.0 ± 1.0	3.93	3.55
87901	α Leo	B8IVn	1.60	S1-S2	−0.12 ± 0.79	0.539	0.37
162003A	HR 6636	F5IV-V	3.43	E1-E2	7.44 ± 0.52	1.431	29.02
164259	ζ Ser	F2IV	3.67	E1-E2	0.76 ± 0.88	2.748	2.48
165777	72 Oph	A4IVs	3.42	E1-E2	3.27 ± 1.46	1.46	1.68
168151	LTT 15404	F5V	3.85	E1-E2	1.84 ± 0.76	3.30	3.89
182572	31 Aql	G8IV	3.53	E1-E2	0.03 ± 0.6	2.34	2.05
182640	δ Aql	F0IV	2.52	S1-S2	7.2 ± 0.41	1.91	51.24
184006	ι Cyg	A5V	3.598	E1-E2	−0.54 ± 0.875	1.581	1.32
187691	LTT 15798	F8V	3.902	E1-E2	1.17 ± 1.87	0.48	0.84
190360	LHS 3510	G7IV-V	4.05	E1-E2	0.05 ± 0.52	1.55	1.32
192640	V1644 Cyg	A2V	4.47	E1-E2	2.16 ± 1.35	1.667	1.95
202444	τ Cyg	F0IV	2.69	S1-S2	2.83 ± 1.35	3.44	3.58
210418	θ Peg	A1Va	3.33	E1-E2	1.69 ± 0.54	1.67	2.80
213558	α Lac	A1V	3.75	E1-E2	−1.17 ± 0.86	0.43	0.71
215648	LHS 3851	F7V	2.92	S1-S2	0.51 ± 0.42	1.08	1.17
217014	51 Peg	G2.5IVa	3.99	E1-E2	−0.03 ± 0.76	0.62	0.51
219080	7 And	F0V	3.77	S1-S2	−0.2 ± 0.54	0.98	0.87
219134	HR 8832	K3V	3.12	S1-S2	0.58 ± 0.54	1.61	1.55
222368	ι Psc	F7V	2.82	E1-E2	1.58 ± 0.36	1.41	4.82

Notes. For each target, the table shows the identifiers, K-band magnitude, interferometric baselines used (S1-S2 ~ 33 m, E1-E2 ~ 60 m), circumstellar emission level, reduced for the star + pole-on-disk model (Eq. (1)), and reduced for the photosphere model. The highlighted boxes correspond to statistically significant excesses: red boxes indicate that there is no evidence of binarity, while yellow boxes indicate that there is separate evidence of binarity.

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