The Chemical Compositions of Accreted and {\it in situ} Galactic
  Globular Clusters According to SDSS/APOGEE
  Studies of the kinematics and chemical compositions of Galactic globular
clusters (GCs) enable the reconstruction of the history of star formation,
chemical evolution, and mass assembly of the Galaxy. Using the latest data
release (DR16) of the SDSS/APOGEE survey, we identify 3,090 stars associated
with 46 GCs. Using a previously defined kinematic association, we break the
sample down into eight separate groups and examine how the kinematics-based
classification maps into chemical composition space, considering only $\alpha$
(mostly Si and Mg) elements and Fe. Our results show that: (i) The loci of both
in situ and accreted subgroups in chemical space match those of their field
counterparts; (ii) GCs from different individual accreted subgroups occupy the
same locus in chemical space. This could either mean that they share a similar
origin or that they are associated with distinct satellites which underwent
similar chemical enrichment histories; (iii) The chemical compositions of the
GCs associated with the low orbital energy subgroup defined by Massari and
collaborators is broadly consistent with an in situ origin. However, at the low
metallicity end, the distinction between accreted and in situ populations is
blurred; (iv) Regarding the status of GCs whose origin is ambiguous, we
conclude the following: the position in Si-Fe plane suggests an in situ}origin
for Liller 1 and a likely accreted origin for NGC 5904 and NGC 6388. The case
of NGC 288 is unclear, as its orbital properties suggest an accretion origin,
its chemical composition suggests it may have formed in situ.
