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Using Gaia DR2, we trace the Anticenter Stream (ACS) in various stellarpopulations across the sky and find that it is kinematically and spatiallydecoupled from the Monoceros Ring. Using stars from {\sc lamost} and {\scsegue}, we show that the ACS is systematically more metal-poor than Monocerosby $0.1$ dex with indications of a narrower metallicity spread. Furthermore,the ACS is predominantly populated of old stars ($\sim 10\,\rm{Gyr}$), whereasMonoceros has a pronounced tail of younger stars ($6-10\, \rm{Gyr}$) asrevealed by their cumulative age distributions. Put togehter, all of thisevidence support predictions from simulations of the interaction of theSagittarius dwarf with the Milky Way, which argue that the Anticenter Stream(ACS) is the remains of a tidal tail of the Galaxy excited during Sgr's firstpericentric passage after it crossed the virial radius, whereas Monocerosconsists of the composite stellar populations excited during the more extendedphases of the interaction. We suggest that the ACS can be used to constrain theGalactic potential, particularly its flattening, setting strong limits on theexistence of a dark disc. Importantly, the ACS can be viewed as a stand-alonefossil of the chemical enrichment history of the Galactic disc.

Chemo-dynamical properties of the Anticenter Stream: a surviving disc fossil from a past satellite interaction