A new population of cool stars and brown dwarfs in the Lupus clouds

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Table 6:

Fits to $I_{\rm C}z_{\rm WFI}JHK_S$ photometry of stars with suspected veiling.
Object (SSTc2dJ)	$T_{\rm eff}$	L ( $L_\odot$ )	A_V	M ( $M_\odot$ )	Age (Myr)	Notes
160708.6-391407	4000	0.086	8.1	0.62	80
160754.7-391545	3200	0.0037	5.0	0.13	101
160829.7-390311	4000	0.020	1.7	-	-	2, 4
160837.3-392311	2300	0.0061	1.5	-	<1	1, 2
160851.4-390530	4000	0.020	5.9	-	-	2, 3
160927.0-383628	3300	0.11	2.5	0.25	2.8
161204.5-380959	3400	0.0033	2.6	-	-	2

Notes - 1: the fit excluding $R_{\rm C}$ leads to a good agreement with the very late spectral type (L0) assigned by López Martí et al. (2005); 2 apparently below the main sequence; 3 par-Lup3-4. Best-fitting temperature is still higher than corresponding to its M 5 type (Comerón et al. 2003), possibly due to a combination of veiling, emission lines, the known infrared excess, and variability of this object; 4 Sz 102. The temperature is consistent with the poorly constrained spectral type (K:) proposed by Hughes et al. (1994). The object is well known to be underluminous, perhaps due to blocking due to a disk close to edge-on.

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