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Since the chemical abundances of stars are the fossil records of the physicalconditions in galaxies, they provide the key information for recovering theassembly history of galaxies. In this work, we explore thechemo-chrono-kinematics of accreted and in-situ stars, by analyzing six M31/MWanalogues from the HESTIA suite of cosmological hydrodynamics zoom-insimulations of the Local Group. We found that the merger debris are chemicallydistinct from the survived dwarf galaxies. The mergers debris have abundancesexpected for stars originating from dwarfs that had their star formationactivity quenched at early times. Accreted stellar haloes, including individualdebris, reveal abundance gradients in the ELz, where the most metal-rich starshave formed in the inner parts of the disrupted systems before the merger andmainly contribute to the central regions of the hosts. Therefore, we suggestthat abundance measurements in the inner MW will allow constraining better theparameters of building blocks of the MW stellar halo. The MDFs of theindividual debris show several peaks and the majority of debris have lowermetallicity than the in-situ stars for Lz>0, while non-rotating and retrogradeaccreted stars are similar to the in-situ. Prograde accreted stars show aprominent knee in the [Fe/H]-[Mg/Fe] plane while the retrograde stars typicallydeposit to a high-[Mg/Fe] sequence. We found that the metal-poor stars([Fe/H]<-1) of the HESTIA galaxies exhibit between zero to 80 km/s net rotationwhich is consistent with the Aurora population. At higher metallicities, wedetect a sharp transition (spin-up) from the turbulent phase to a disk-likerotation. Mergers debris are similar in the [Fe/H]-[Mg/Fe] plane. However,combining a set of abundances allows to capture chemical patterns correspondingto different debris, which are the most prominent as a function of stellar age.

The stellar halo in Local Group Hestia simulations III. Chemical abundance relations for accreted and in-situ stars