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We have for the first time identified the early stellar disk in the Milky Wayby using a combination of elemental abundances and kinematics. Using data fromAPOGEE DR17 and Gaia we select stars in the Mg-Mn-Al-Fe plane with elementalabundances indicative of accreted origin and find stars with both halo-like anddisk-like kinematics. The stars with halo-like kinematics lie along a lowersequence in [Mg/Fe], while the stars with disk-like kinematics lie along ahigher sequence. Through with asteroseismic observations, we determine thestars with halo-like kinematics are old, 9-11 Gyr and that the more evolvedstellar disk is about 1-2 Gyr younger. We show that the in situ fraction ofstars on deeply bound orbits is not small, in fact the inner Galaxy likelyharbours a genuine in-situ population together with an accreted one. Inaddition, we show that the selection of Gaia-Sausage-Enceladus in the En-Lzplane is not very robust. In fact, radically different selection criteria givealmost identical elemental abundance signatures for the accreted stars.

The metal-weak Milky Way stellar disk hidden in the Gaia-Sausage-Enceladus debris: the APOGEE DR17 view