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While brown dwarfs show similarities with stars in their early life, theirspin evolution is much more akin to that of planets. We have used lightcurvesfrom the K2 mission to measure new rotation periods for 18 young brown dwarfsin the Taurus star-forming region. Our sample spans masses from 0.02 to 0.08Msol and has been characterised extensively in the past. To search for periods,we utilize three different methods (autocorrelation, periodogram, GaussianProcesses). The median period for brown dwarfs with disks is twice as long asfor those without (3.1 vs. 1.6 d), a signature of rotational braking by thedisk, albeit with small numbers. With an overall median period of 1.9 d, browndwarfs in Taurus rotate slower than their counterparts in somewhat older (3-10Myr) star-forming regions, consistent with spin-up of the latter due tocontraction and angular momentum conservation, a clear sign that disk brakingoverall is inefficient and/or temporary in this mass domain. We confirm thepresence of a linear increase of the typical rotation period as a function ofmass in the sub-stellar regime. The rotational velocities, when calculatedforward to the age of the solar system assuming angular momentum conservation,fit the known spin-mass relation for solar system planets and extra-solarplanetary-mass objects. This spin-mass trend holds over six orders of magnitudein mass, including objects from several different formation paths. Our resultimplies that brown dwarfs by and large retain their primordial angular momentumthrough the first few Myr of their evolution.

A universal spin-mass relation for brown dwarfs and planets