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.
|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)|
|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 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)|
|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:
Monnier et al. (2006), IOTA, H band.
Eisner et al. (2009) (Keck, K band).
Kraus et al. (2008), VLTI/AMBER, K band.
Verhoeff et al. (2010), VLTI/AMBER, K band.
Benisty et al. (2010), VLTI/AMBER, K band,
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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