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Table 1:

Characteristics of the source in the considered sample
Object log ( $T_{\rm stellar}$) Sp. type Disk evolution Age (Myr) Ref.
HD 135 344 3.810 F4Ve Transition $8 \pm 4$ 1, 3, 11
HD 169 142 3.914 A5Ve Transition $\rm 6^{+6}_{-3}$ 1, 4, 12
HD 34 282 3.941 A3Vne Thin 5 1, 5, 13
HD 97 048 4.000 A0/B9Ve+sh Thick $4\pm 1$ 1, 6
HD 34 700 3.774 G0IVe Thick $\rm 3 ^{+6}_{-3}$ 1, 7
RR Tau 3.927 A4e Transition $\rm 3^{+1}_{-2.6}$ 1, 8, 9
HD 141 569 3.979 A0Ve Thin 5 1, 5
BD +40$^{\circ }$ 4124 4.291 B2Ve Thick+Env. $\rm 1^{+2}_{-0.9}$ 1, 8, 14
CD -42$^{\circ }$ 11 721 4.470 B0IVep Thick+Env. $\rm0.5^{+2}_{-0.4}$ 1, 10
LkH$\alpha$ 215 4.114 B7 Thick+Env. 1 14
IRS 48 ? ? Thin $4\pm 1$ 2
Gomez Hamburger ? ? Thick ? 15, 16
1: Acke & van den Ancker (2004), 2: Geers et al. (2007), 3: Doucet et al. (2006), 4: Raman et al. (2006), 5: Merín et al. (2004), 6: Lagage et al. (2006), 7: Torres (2004), 8: Natta et al. (1997), 9: Rostopchina (1999), 10: Wang & Looney (2007), 11: Brown et al. (2007), 12: Grady et al. (2007), 13: Piétu et al. (2003), 14: Hillenbrand et al. (1995), 15: Ruiz et al. (1987), 16: Bujarrabal et al. (2008).


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