Aluminum Enhanced Metal-Poor Stars buried in the Inner Galaxy
  Stars with higher aluminum and nitrogen enrichment are often the key pieces
for the chemical makeup of multiple populations in almost all globular clusters
(GCs). There is also compelling observational evidence that some Galactic
components could be partially built from dissipated GCs. Thus, the
identification of such kinds of stars among metal-poor field stars may provide
insights on the composite nature of the Milky Way (MW) bulge and inner stellar
halo, as well as reveal other chemical peculiarities. Here, based on APOGEE
spectra, we report the discovery of 29 mildly metal-poor ([Fe/H]$\lesssim-0.7$)
stars with stellar atmospheres strongly enriched in aluminum (Al-rich stars:
[Al/Fe]$\gtrsim+0.5$), well above the typical Galactic levels, located within
the Solar radius toward the bulge region, which lies in highly eccentric orbits
($e\gtrsim0.6$). We find many similarities for almost all of the chemical
species measured in this work with the chemical patterns of GCs, so we
conjecture that they have likely been dynamically ejected into the bulge and
inner halo from GCs formed in situ and/or GC formed in different progenitors of
known merger events experienced by the MW, such as the
\textit{Gaia}-Sausage-Enceladus and/or Sequoia.
