An Inward-moving and Asymmetric Velocity Wave Detected in LAMOST-Gaia

Abstract

The phase space, as coded by kinematic parameters and chemical abundances, is crucial for understanding the formation of the Galactic disk. Using red giant stars from the Galactic thin disk with [Fe/H] > − 0.8 and low-α ratios identified in LAMOST-Gaia, we detect numerous ridges and undulations in the R–V ϕ diagram coded by median V R . Strikingly, the slope of these features changes from −22 km s−1 kpc−1 to −8 km s−1 kpc−1 at R ∼ 11.5 kpc. Accordingly, the R g–V ϕ plane, also coded by median V R , reveals wave-like structures that propagate outwards in the inner disk but reverse direction and move inwards beyond R g = 11.5 kpc. The most prominent feature is the G1 group, distinguished by its wider spread and negative median V R at R g ∼ 15 kpc, contrasting with the narrower G0 group that exhibits positive median V R at R g < 11.5 kpc. Furthermore, the [C/N] versus [Fe/H] relationship for the G1 group mirrors the opposite trend compared to the G0 group. Since [C/N] serves as a proxy for age, this contrasting behavior suggests an inverse age–metallicity relation for the G1 group. Comparison with the Sagittarius dwarf galaxy reveals that the G1 group possesses distinct [Mg/Fe] and [Al/Fe] ratios, yet its [C/N] versus [Fe/H] pattern is similar to that of the Sgr dwarf galaxy. Based on these observations, we proposed that the inward-moving and asymmetric velocity wave G1 might be linked to the minor merge of the Sagittarius galaxy.