  Few dozens of young high mass stars orbit Sgr A* at distances as short as 0.1
parsec, where star formation should be quenched by the strong tidal shear from
Sgr A*. The puzzling young stellar population is believed to come into
existence in one of the two ways:
  (i) "normal" star formation at several tens of parsec in a very massive star
cluster that then spiraled in, or (ii) star formation in situ in a massive
self-gravitating disk. We propose to constrain these two scenarios via the
expected X-ray emission from young low mass stars that should have formed
alongside the massive stars. To this end we compare the recent Chandra
observations of X-ray emission from young stars in the Orion Nebula, and the
Chandra observations of Sgr A* field. We show that the cluster inspiral model
is ruled out irrespectively of the initial mass function (IMF) of the young
stars. In addition, for the in situ model, we find that no more than few
thousand low-mass stars could have formed alongside the massive stars. This is
more than a factor of ten fewer than expected if these stars were formed with
the standard IMF as elsewhere in the Galaxy. The young stars in the GC are thus
the first solid observational evidence for star formation in AGN disks and also
require the IMF of these stars to be top-heavy. We briefly consider implication
of these results for AGN in general.
