UV excess measures of accretion onto young very low mass stars and brown dwarfs

Low-resolution spectra from 3000 to 9000 angstrom of young low-mass stars and brown dwarfs were obtained with LRIS on Keck I. The excess UV and optical emission arising in the Balmer and Paschen continua yields mass accretion rates ranging from 2 x 10(-12) to 10(-8) M-circle dot yr(-1). These results are compared with HST STIS spectra of roughly solar-mass accretors with accretion rates that range from 2 x 10(-10) to 5 x 10(-8) M-circle dot yr(-1). The weak photospheric emission from M dwarfs at < 4000 angstrom leads to a higher contrast between the accretion and photospheric emission relative to higher mass counterparts. The mass accretion rates measured here are systematically similar to 4-7 times larger than those from H alpha emission line profiles, with a difference that is consistent with but unlikely to be explained by the uncertainty in both methods. The accretion luminosity correlates well with many line luminosities, including high Balmer and many He I lines. Correlations of the accretion rate with H alpha 10% width and line fluxes show a large amount of scatter. Our results and previous accretion rate measurements suggest that. (M) over circle alpha M-1.87 +/- 0.26 for accretors in the Taurus molecular cloud.