Checking of wavelength coverage when calculating bolometric fluxes

In the colors module, when an SED is integrated to calculate a bolometric flux, is there any check done to see if the SED spans a sufficient wavelength range for the flux to be accurate? What happens if a user calculates bolometric fluxes from SEDs that only extend from the near-UV to longer wavelengths -- is there any warning that this will give wrong values for hot stars that emit much of their energy in the mid-UV?

A related question -- has there been any comparison of the bolometric fluxes evaluated by the colors module, and F_bol = sigma Teff^4? In principle, the two should agree if the stellar atmosphere is consistent with the photospheric boundary condition applied in MESA.