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Table 5

Comparison of RCO,10% to the location of the inner dust disk as calculated from the dust sublimation radius and, where available, as measured with IR interferometry.

Name R CO,10% /L

Group I [au] [au] [au] [au]

HD 100546 6.8±1.6 0.45 0.25 0.26e 1.30 ± 0.13 (–3)
HD 97048 10.1±1.8 0.36 0.20 1.29 ± 0.01 (–3)
HD 179218 9.2±1.5 0.61 0.34 >3.1a 1.65 ± 0.17 (–3)

Group II

HD 101412 0.6±0.1 0.35 0.20 2.57 ± 0.05 (–4)
HD 190073 1.9±2.8,† 0.64 0.36 0.62b 9.61 ± 2.80 (–5)
HD 98922 4.2±2.2,‡ 2.09 1.18 1.25c n.s.
HD 95881 1.9±0.6,‡ 0.33 0.18 0.37d 9.53 ± 0.08 (–4)
HD 150193 0.5±0.2 0.28 0.15 0.71a <5.3 (–5)
HD 104237 0.3±0.5,† 0.41 0.23 0.29c <5.3 (–6)

Not classified

HD 141569 10.4±1.9,† 0.25 0.14 8.70 ± 0.10 (–5)
HD 135344B 0.4±0.2 0.22 0.13 0.2f 2.74 ± 0.12 (–4)

Notes. The references for the 2 μm inner rim sizes in the fifth column are:

(a)

Monnier et al. (2006), IOTA, H band.

(b)

Eisner et al. (2009) (Keck, K band).

(c)

Kraus et al. (2008), VLTI/AMBER, K band.

(d)

Verhoeff et al. (2010), VLTI/AMBER, K band.

(e)

Benisty et al. (2010), VLTI/AMBER, K band,

(f)

Carmona et al. (2014), VLTI/PIONIER H band. PAH to luminosity ratios in the last column are adapted from Acke et al. (2010) and Acke & van den Ancker (2004). The upper limits are 3σ, a(b) represents a × 10b, and n.s. means no spectrum is available. To calculate the error on RCO,10% for sources with missing error estimates we adopt a 10% error for the values of the stellar mass (†) and the inclination (‡).

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