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Recent evidence based on APOGEE data for stars within a few kpc of theGalactic centre suggests that dissolved globular clusters (GCs) contributesignificantly to the stellar mass budget of the inner halo. In this paper weenquire into the origins of tracers of GC dissolution, N-rich stars, that arelocated in the inner 4 kpc of the Milky Way. From an analysis of the chemicalcompositions of these stars we establish that about 30% of the N-rich starspreviously identified in the inner Galaxy may have an accreted origin. Thisresult is confirmed by an analysis of the kinematic properties of our sample.The specific frequency of N-rich stars is quite large in the accretedpopulation, exceeding that of its in situ counterparts by near an order ofmagnitude, in disagreement with predictions from numerical simulations. We hopethat our numbers provide a useful test to models of GC formation anddestruction.

An enquiry on the origins of N-rich stars in the inner Galaxy basedon APOGEE chemical compositions