Notes. The full table is available at the CDS. This table lists all observed objects, their Li and Hα EW, and membership criteria. The objects IDs are based on the spectrograph (optical) coordinates. If Hα appears in absorption, we label it as “Abs.” in the corresponding column. If Lithium absorption can be excluded for EW larger than 0.1, we label it as “N” in the corresponding column. Membership and presence of disks are marked as “Y” (yes), “N” (no), “P” (probable), and “pN” (probably not). In case the disk excess was observed only at one wavelength, we label it (e.g. P(24) indicates that the object has probably an excess, but only at 24 μm). Undetermined values of the spectral type, uncertain membership, and uncertain IR fluxes are marked by “X”, objects with spectral types earlier than G are marked with “E”. The errors in the spectral type are of 0.5 subtypes for objects K5 or later, 1 subtype for early K stars, and 2–3 subtypes for G-type objects. The best spectral types (in case of multiple values due to different observations with different S/N) are marked with ^(b). Objects previously identified by Sicilia-Aguilar et al. (2005, 2006a,b) are marked with ⁽¹⁾ (and their previous names are given in the comments), those identified by Barentsen et al. (2011) are marked with ⁽²⁾, those in common with Morales-Calderón et al. (2009) are marked with ⁽³⁾, objects with X-ray counterparts in Getman et al. (2012) are marked with ⁽⁴⁾, and further IR-excess sources in the same paper are marked with ⁽⁵⁾. In the comments field, we mention if there is any problem due to IR nebular emission (Neb.), nearby objects (Nobj.), if the SED suggest that the object is variable (Var.), if the object appears older than 10 Myr in the V vs. V − I diagram (oVVI), or any other observation regarding the star/disk.