| Summary: | The search for accreted satellites in the Galactic disk is a challenging task, to which Gaia plays a crucial role in synergy with ground-based spectroscopic surveys. In 2021, P. Re Fiorentin et al. discovered five substructures with disk kinematics including Icarus. To gain more insight into the origin of Icarus as a remnant of a dwarf galaxy rather than a signature of secular processes of disk formation, we complement astrometric Gaia DR3 data with spectroscopy from APOGEE DR17 and GALAH DR3, and explore the chemodynamical distributions within 3 kpc of the Sun. We select 622 stars in the accreted/unevolved regions of [Mg/Mn]–[Al/Fe] and [Mg/Fe]–[Fe/H], where we identify 81 and 376 stars with −2 < [Fe/H] < −0.7 belonging to Icarus and Gaia-Sausage-Enceladus (GSE), respectively. The revised properties of Icarus are: 〈 V + V _LSR 〉 ≃ 171 km s ^−1 , σ _V ≃ 37 km s ^−1 , 〈 e 〉 ≃ 0.36, 〈[Fe/H]〉 ≃ −1.35, 〈[Mg/Fe]〉 ≃ +0.27, 〈[Al/Fe]〉 ≃ −0.13, and 〈[Mn/Fe]〉 ≃ −0.39. From the color–magnitude diagram of its members, Icarus appears older than 12 Gyr. Such age and dynamical properties are reminiscent of the metal-weak thick disk. However, detailed chemical analysis in the diagnostic spaces [Ni/Fe]–[(C+N)/O], [Y/Eu]–[Fe/H], [Eu/Mg]–[Fe/H], [Ba/Y]–[Fe/H], and [Ba/Mg]–[Mg/H] evidences that Icarus and GSE occupy the accreted region, well separated from the bulk of in situ disk stars. Updated comparisons with N -body simulations confirm that Icarus’s stars are consistent with the debris of a dwarf galaxy with a stellar mass of ∼10 ^9 M _☉ accreted onto a primordial disk on an initial prograde low-inclination orbit.
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