Measuring the properties of protoplanetary disks around brown dwarfs is central to understanding the formation of brown dwarfs and their planetary companions .
We present modeling of CFHT Tau 4 and 2M0444 , two brown dwarfs with protoplanetary disks in the Taurus Molecular Cloud .
By combining modeling of the spectral energy distributions and ALMA images , we obtain disk radii and masses for these objects ; these parameters can be used to constrain brown dwarf formation and planet formation , respectively .
We find that the disk around CFHT Tau 4 has a total mass of 0.42 M _ { Jup } and a radius of 80 au ; we find 2M0444 ’ s disk to have a mass of 2.05 M _ { Jup } and a radius of 100 au .
These radii are more consistent with those predicted by theoretical simulations of brown dwarf formation via undisturbed condensation from a mass reservoir than those predicted by ejection from the formation region .
Furthermore , the disk mass of 2M0444 suggests that planet formation may be possible in this disk , although the disk of CFHT Tau 4 is likely not massive enough to form planets .
The disk properties measured here provide constraints to theoretical models of brown dwarf formation and the formation of their planetary companions .