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Table 1

NIR interferometric detections of hot exozodiacal dust, together with associated outer debris belt locations.

Object Sp. type Band Excess FOVa Instrument Refs. Outer belt distanceb Refs.
[%] [AU] [AU]
Vega A0V H 1.23 ± 0.53 6 IOTA/IONIC D11 10–14, 80 D00, S13
Vega A0V K 1.26 ± 0.27 3 CHARA/FLUOR A06, A13 10–14, 80 D00, S13
Vega A0V K 4 PTI C01 10–14, 80 D00, S13
ζ Aql A0V K 1.69 ± 0.27 10 CHARA/FLUOR A08, A13 no detectable outer belt A08, P09
β Leo A3V K 0.94 ± 0.26 4 CHARA/FLUOR Ak09, A13 19 C06
λ Gem A3V K 0.74 ± 0.17 12 CHARA/FLUOR A13 no detectable outer belt M09, G13
Fomalhaut A4V K 0.88 ± 0.12 6 VLTI/VINCI Ab09 2, 8–11, 133 K05, L13, S13
β Picc A6V H 1.37 ± 0.16 4 VLTI/PIONIER D12 10–40d L94, P97
β Picc A6V K 0.76 ± 0.49 1.3 VLTI/VINCI D04, D12 10–40d L94, P97
α Aql A7V K 3.07 ± 0.24 2 CHARA/FLUOR A13 no detectable outer belt A13
α Cep A7IV K 0.87 ± 0.18 6 CHARA/FLUOR A13 no detectable outer belt C05
η Lepe F1V K 0.89 ± 0.21 6 CHARA/FLUOR A13 1–16, 18 L09, E13
110 Here F6V K 0.94 ± 0.25 8 CHARA/FLUOR A13 70–500 M13
10 Taue F9V K 1.21 ± 0.11 6 CHARA/FLUOR A13 >5.8 T08
ξ Booe G8V K 0.74 ± 0.20 3 CHARA/FLUOR A13 no detectable outer belt A13
τ Cet G8V K 0.98 ± 0.18 1.5 CHARA/FLUOR D07, A13 10–55 G04
κ CrBe K1IV K 1.18 ± 0.20 12 CHARA/FLUOR A13 20, 41 B13

Notes.

(a)

FOV denotes the approximate linear field-of-view radius at half maximum.

(b)

For the outer belt distance (r0 in our models) we list literature estimates of the radial distance to (the inner edge of) “cold” and “warm” outer belts, derived from SED fitting and/or resolved imaging.

(c)

The NIR excess of β Pic contains a significant contribution from stellar light scattered by the outer belt (Defrère et al. 2012).

(d)

The debris disk around β Pic is seen edge-on, making it hard to determine the parent belt location. The values given mark the radial range in which the particle density is derived to decrease.

(e)

For η Lep, 110 Her, 10 Tau, ξ Boo, and κ CrB, the possibility that the observed NIR excess is due to a low-mass companion within the field-of-view cannot be excluded (Absil et al. 2013).

Reference. (A06) Absil et al. (2006); (A08) Absil et al. (2008); (Ab09) Absil et al. (2009); (Ak09) Akeson et al. (2009); (A13) Absil et al. (2013); (B13) Bonsor et al. (2013); (C01) Ciardi et al. (2001); (C05) Chen et al. (2005); (C06) Chen et al. (2006); (D00) Dent et al. (2000); (D04) di Folco et al. (2004); (D07) di Folco et al. (2007); (D11) Defrère et al. (2011); (D12) Defrère et al. (2012); (E13) Eiroa et al. (2013); (G04) Greaves et al. (2004); (G13) Gáspár et al. (2013); (K05) Kalas et al. (2005); (L94) Lagage & Pantin (1994); (L09) Lawler et al. (2009); (L13) Lebreton et al. (2013); (M09) Morales et al. (2009); (M13) Marshall et al. (2013); (P97) Pantin et al. (1997); (P09) Plavchan et al. (2009); (S13) Su et al. (2013); (T08) Trilling et al. (2008).

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