BAF-type main-sequence stars rotation velocities

We rely on high-precision model-independent internal rotation frequencies, as well as on masses and radii from asteroseismology to deduce Veq, Veq/Vcrit, and J/M for 2937 gravity-mode pulsators in the Milky Way. The sample stars have rotation frequencies between almost zero and 33uHz, corresponding to rotation periods above 0.35d. We find that intermediate-mass stars experience a break in their J/M occurring {in the mass interval [2.3,2.7]M_{sun}_.} We establish unimodal Veq and Veq/Vcrit distributions for the mass range [1.3,2.5[M_{sun}_ while stars with M in [2.5,8.8]M_{sun}_ reveal some structure in their distributions.

We find {that the near-core rotation slows down as stars evolve,} pointing to very efficient angular momentum transport. The kernel density estimators of the asteroseismic internal rotation frequency, equatorial rotation velocity, and specific angular momentum of this large sample of intermediate-mass field stars can conveniently be used for population synthesis studies and to fine-tune the theory of stellar rotation across the main sequence evolution.