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We combine spectroscopic, photometric, and astrometric information fromAPOGEE data release 17 and $Gaia$ early data release 3 to perform aself-consistent characterization of $Gaia$-Sausage/Enceladus (GSE), the remnantof the last major merger experienced by the Milky Way, considering stars andglobular clusters (GCs) altogether. Our novel set of chemodynamical criteria toselect genuine stars of GSE yields a metallicity distribution function with amedian [Fe/H] of $-1.22$ dex and $0.23$ dex dispersion. Stars from GSE presentan excess of [Al/Fe] and [Mg/Mn] (also [Mg/Fe]) in comparison to survivingMilky Way dwarf satellites, which can be explained by differences instar-formation efficiencies and timescales between these systems. However,stars from Sequoia, another proposed accreted halo substructure, essentiallyoverlap the GSE footprint in all analyzed chemical-abundance spaces, butpresent lower metallicities. Among probable GCs of GSE with APOGEE observationsavailable, we find no evidence for atypical [Fe/H] spreads with the exceptionof $\omega$ Centauri ($\omega$Cen). Under the assumption that $\omega$Cen is astripped nuclear star cluster, we estimate the stellar mass of its progenitorto be $M_\star \approx 1.3 \times 10^9 M_\odot$, well-within literatureexpectations for GSE. This leads us to envision GSE as the best availablecandidate for the original host galaxy of $\omega$Cen. We also take advantageof $Gaia$'s photometry and APOGEE metallicities as priors to determinefundamental parameters for eight high-probability ($>$70%) GC members of GSEvia statistical isochrone fitting. Finally, the newly determined ages andAPOGEE [Fe/H] values are utilized to model the age-metallicity relation of GSE.

Reconstructing the Disrupted Dwarf Galaxy $Gaia$-Sausage/Enceladus Using its Stars and Globular Clusters