  We have discovered rotationally split core g-mode triplets and surface p-mode
triplets and quintuplets in a terminal age main sequence A star, KIC 11145123,
that shows both $\delta$ Sct p-mode pulsations and $\gamma$ Dor g-mode
pulsations. This gives the first robust determination of the rotation of the
deep core and surface of a main sequence star, essentially model-independently.
We find its rotation to be nearly uniform with a period near 100 d, but we show
with high confidence that the surface rotates slightly faster than the core. A
strong angular momentum transfer mechanism must be operating to produce the
nearly rigid rotation, and a mechanism other than viscosity must be operating
to produce a more rapidly rotating surface than core. Our asteroseismic result,
along with previous asteroseismic constraints on internal rotation in some B
stars, and measurements of internal rotation in some subgiant, giant and white
dwarf stars, has made angular momentum transport in stars throughout their
lifetimes an observational science.
