1 Apparently below the main sequence 2 Merin et al. (2008, Cat. ) fit a spectral type corresponding 2 to a cooler temperature, with no extinction, and derive a lower luminosity 2 that yields an unusually high disk-to-star luminosity ratio, L_disk_/L_*_ 2 ratio. Our results, involving moderate extinction, imply L_disk_/L_*_=0.36, 2 closer to typical values among the Lupus 3 population. 3 Unreliable fit probably due to veiling. See Table 6. 4 Important K excess in addition to veiling. No fit in Merin et al. 4 (2008, Cat. ). 5 Well known to apparently lie below the main sequence despite its M5 spectral 5 type. Variability reported by Comeron et al. (2003A&A...406.1001C). 7 Fit as M5 in Merin et al. (2008, Cat. ); close companion 7 at 2.4", probably contaminating the photometry confusion. 8 No fit in Merin et al. (2008, Cat. ). 9 Fit much later than in Merin et al. (2008, Cat. ) 10 Highly variable. 11 Candidate member in Nakajima et al. (2000AJ....119..873N). Variability 11 suspected. A comparison with 2MASS photometry shows it to be fainter in J, H 11 by 0.12 and 0.16mag respectively, and brighter in Ks by 0.15mag, in the 11 observations of Nakajima et al. (2000AJ....119..873N). 14 Variability suspected. A comparison with 2MASS photometry shows it to be 14 brighter in J by 0.26mag, and slightly fainter in HKs by 0.07mag. 15 Fitted by Merin et al. (2008, Cat. ) as A0 with very high 15 extinction, which seems unlikely because it sits in a low extinction region. 15 It may be a background red giant instead. 16 Strong K excess. No fit in Merin et al. (2008, Cat. ). 17 Relatively blue spectral energy distribution, the fit seems reasonable. Hints 17 of elongation; perhaps having a disk close to edge-on orientation. 19 Sz 102 is a peculiar object with strong emission lines, veiling and 19 underluminous. 20 Very strong H{alpha} emission reported by Hughes et al. 20 (1994AJ....108.1071H), possibly veiled. 21 Our measured I_C_ is fainter than that in Hughes et al. 21 (1994AJ....108.1071H), whereas the 2MASS JHK_S_ magnitudes are brighter than 21 those listed in that work by 0.4mag. The source thus seems to be highly 21 variable and our fit is likely to be affected by non-simultaneity of 21 observations. 22 Selected as possible member by Nak00 because of near-infrared excess. 24 Variability at the ~0.2mag level in JHK_S_ reported by Hughes et al. 24 (1994AJ....108.1071H). Our I_C_ measurement is very similar to that of 24 Hughes et al. (1994AJ....108.1071H). Probably variable. 25 Possibly variable: 2MASS J magnitude brighter than in Hughes et al. 25 (1994AJ....108.1071H) by ~0.2mag, but H and K_S_ almost identical. Our I_C_ 25 measurement is ~0.2mag brighter than in Hughes et al. (1994AJ....108.1071H). 26 K2 in Hughes et al. (1994AJ....108.1071H). The 2MASS HK_S_ magnitudes are 26 fainter than in Hughes et al. (1994AJ....108.1071H) by ~0.2mag, but J is 26 very similar. Our measurement in I_C_ is 0.5mag fainter than in Hughes et 26 al. (1994AJ....108.1071H). Probably variable, affecting our fit. 27 Moderately variable: the R_C_ and I_C_ in Comeron et al. 27 (2003A&A...406.1001C) are 0.17mag fainter than in the new WFI measurements, 27 and the 2MASS H and K_S_ magnitudes are ~0.1mag brighter than the 27 measurements in those bands given in Comeron et al. (2003A&A...406.1001C). 28 Photometry in R_C_ contaminated by a much bluer companion at 1.7", clearly 28 detected in R_C_, much fainter in I_C_ and undetected in z_WFI_. 29 Extended in the NE-SW direction in the R_C_ image. Hints of elongation in 29 I_C_, point source in z_WFI_. It might possess an outflow. 30 Very uncertain WFI photometry:marginal detection in R_C_ and z_WFI_, and very 30 faint in I_C_. 31 Slightly fainter companion at 2". 32 Undetected in R_C_ and faint in I_C_; uncertain fit at the WFI wavelengths. 33 Close companion at 1.5" contaminating our photometry. 34 Clearly elongated in the NW-SE direction in R_C_, hints of elongation also in 34 I_C_ and z_WFI_. It might be scattered light by a close-to-edge-on disk. 35 Slightly elongated in R_C_ and I_C_ in the NW-SE direction. 36 High residual fit (over 0.2mag rms).