Top: 70 μm flux density shown as a function of spectral type for the Taurus Class II population, with spectral types spanning early K to late M. The vertical dotted lines mark the boundaries of the TBOSS sample (targets of spectral types M4+) and the stellar/substellar limit (M6.25). Flux densities measured from PACS and MIPS are represented by the black and gray points respectively. Additionally, for the detected TBOSS targets, the large blue points correspond to best-fit stellar radii of >1.5 times that of the evolutionary model values, and the small red points correspond to best-fit stellar radii of <0.5 times that of the evolutionary model values. Downwards arrows represent the 3σ upper limits. The dashed lines represent the 70 μm flux densities extracted from a test grid of model SEDs, generated with the radiative transfer code MCFOST and represent the flux densities for disk inclinations of face-on (0°; purple dashed-line), 60° (blue dashed-line) and edge-on (90°; red dashed-line). Bottom: bolometric luminosities of the Taurus Class II population, with spectral types spanning early K to late M. The luminosities of the TBOSS sample are derived from the best-fit stellar radii. The luminosities for targets of spectral type <M4 are from those reported in Andrews et al. (2013). The 1 Myr isochrone from Baraffe et al. (1998) is represented with the blue solid line and the corresponding isochrones are shown for values of 2 and 0.4 times that of the model stellar radii (purple and red solid lines respectively).