Table 5
Gaussian fit to our sample.
| Star | d | FWHM | R/U | λ |
| (pc) | (′′) | (μm) | ||
|
|
||||
| AB Aur | 139.3 ± 19.0 | 6.7 ± 0.2 | R | 70 |
| HD 31648 | 137.0 ± 26.2 | 6.1 ± 0.2 | U | 70 |
| HD 35187 | 114.2 ± 32.4 | 6.1 ± 0.2 | U | 70 |
| HD 36112 | 279.3 ± 75.0 | 6.1 ± 0.2 | U | 70 |
| CQ Tau | 113.0 ± 24.0 | 6.1 ± 0.2 | U | 70 |
| HD 97048 | 159.5 ± 15.7 | 6.1 ± 0.2 | U | 70 |
| HD 98922 | 200 | 6.1 ± 0.2 | U | 70 |
| HD 100453 | 121.5 ± 9.7 | 6.1 ± 0.2 | U | 70 |
| HD 100546 | 96.9 ± 4.0 | 6.5 ± 0.2 | R | 70 |
| HD 104237 | 114.7 ± 4.7 | 6.4 ± 0.3 | R | 70 |
| HD 135344B | 142.0 ± 27.0 | 6.1 ± 0.2 | U | 70 |
| HD 139614 | 140.0 ± 42 | 6.1 ± 0.2 | U | 70 |
| HD 141569 | 116.1 ± 8.1 | 7.2 ± 0.2 | R | 100 |
| HD 142527 | 233.1 ± 56.2 | 6.5 ± 0.2 | R | 70 |
| HD 142666 | 145.0 ± 43 | 6.1 ± 0.2 | U | 70 |
| HD 144668 | 162.9 ± 15.3 | 6.1 ± 0.2 | U | 70 |
| HD 150193 | 216.5 ± 76.0 | 6.3 ± 0.1 | U | 100 |
| KK Oph | 260 | 6.1 ± 0.2 | U | 70 |
| 51 Oph | 124.4 ± 3.7 | 6.1 ± 0.2 | U | 70 |
| HD 163296 | 118.6 ± 11.1 | 6.1 ± 0.2 | U | 70 |
| HD 169142 | 145.0 ± 43 | 6.1 ± 0.2 | U | 70 |
| HD 179218 | 253.8 ± 44.7 | 6.1 ± 0.2 | U | 70 |
|
|
||||
| 49 Ceta | 59.4 ± 1.0 | 7.8 ± 0.6 | R | 70 |
| HD 32297b | 112.4 ± 10.8 | 6.1 ± 0.2 | U | 70 |
| HR 1998 | 21.6 ± 0.1 | 6.1 ± 0.1 | U | 70 |
| HR 4796A | 72.8 ± 1.8 | 7.0 ± 0.4 | U | 70 |
| HD 158352 | 59.6 ± 0.9 | 6.1 ± 0.2 | U | 70 |
Notes. R/U column indicates whether the object is resolved (R) or unresolved (U) compared to point source α Boo. Last column states wavelength at which the FWHM was measured. Distances are from the revised parallaxes by van Leeuwen (2007), except for HD 135344B (Müller et al. 2011), HD 98922 (Manoj et al. 2006), HD 139614, HD 142666, and HD 169142 (van Boekel et al. 2005), HD 89822 and (Blondel & Djie 2006). and
Has been resolved in Roberge et al. (2013), with a disc size of 200 au
in Donaldson et al. (2013), with a disc size of 110 au.
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