– 49 – Table 3—Continued $^{a}$The disk mass upper limits for targets #12 and 27 come from Cieza et al. (2008). $^{b}$Source # 12 is a binary identified by VLBA observations (Loinard et al. 2008). Source # 24 is a triple system. The tight components are consistent with two equal-brightness objects with a separation of ∼ 7 AU and a ∼ 30 deg position angle (see § 4.4 and Figure 4). Source # 27 is a triple system. The “primary” star in the VLT observations is itself a spectroscopic binary with a 35.9 d period and estimated separation of 0.27 AU (Mathieu et al. 1994). # LOG(Acc. rate) Mass Disk a r$_{proj.}$ b λ$_{tun}$$_{−}$$_{off}$ α$_{excess}$ LOG(L$_{D}$/L$_{∗}$) A$_{J}$ Object Type (M$_{⊙}$/yr) (M$_{JUP}$ ) (AU) µ m (mag) 32 -9.9 11.1 · · · 8.00 0.72 -2.70 1.3 giant planet forming disk 33 · · · · · · · · · 8.00 -2.21 < -3.86 1.6 AGB star 34 · · · · · · · · · 8.00 -1.83 < -3.58 1.4 AGB star