We have identified four brown dwarfs in the Taurus star-forming region .
They were first selected from R and I CCD photometry of 2.29 square degrees obtained at the Canada-France-Hawaii Telescope .
Subsequently , they were recovered in the 2MASS second incremental data release point source catalog .
Low-resolution optical spectra obtained at the William Herschel telescope allow us to derive spectral types in the range M7–M9 .
One of the brown dwarfs has very strong H \alpha emission ( EW=-340 Å ) .
It also displays Br \gamma emission in an infrared spectrum obtained with IRCS on the Subaru telescope , suggesting that it is accreting matter from a disk .
The K i resonance doublet and the Na i subordinate doublet at 818.3 and 819.5 nm in these Taurus objects are weaker than in field dwarfs of similar spectral type , consistent with low surface gravities as expected for young brown dwarfs .
Two of the objects are cooler and fainter than GG Tau Bb , the lowest mass known member of the Taurus association .
We estimate masses of only 0.03 M _ { \odot } for them .
The spatial distribution of brown dwarfs in Taurus hints to a possible anticorrelation between the density of stars and the density of brown dwarfs .