Insights into the Galactic Bulge Chemodynamical Properties from Gaia Data Release 3

• Published in: The Astrophysical journal Vol. 967; no. 1; pp. 5 - 19
• Main Authors: Liao, Xiaojie, Li, Zhao-Yu, Simion, Iulia, Shen, Juntai, Grand, Robert, Fragkoudi, Francesca, Marinacci, Federico
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.05.2024; IOP Publishing
• Subjects: Galactic bulge; Galaxies; Galaxy bulges; Giant stars; Iron; Kinematics; Metallicity; Milky Way evolution; Red giant stars; Rotation
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad38ba

Abstract We explore the chemodynamical properties of the Galaxy in the azimuthal velocity V ϕ and metallicity [Fe/H] space using red giant stars from Gaia Data Release 3. The row-normalized V ϕ –[Fe/H] maps form a coherent sequence from the bulge to the outer disk, clearly revealing the thin/thick disk and the Splash. The metal-rich stars display bar-like kinematics, while the metal-poor stars show dispersion-dominated kinematics. The intermediate-metallicity population (−1 < [Fe/H]< − 0.4) can be separated into two populations, one that is bar-like, i.e., dynamically cold ( σ V R ∼ 80 km s −1 ) and fast-rotating ( V ϕ ≳ 100 km s −1 ), and the Splash, which is dynamically hot ( σ V R ∼ 110 km s −1 ) and slow-rotating ( V ϕ ≲ 100 km s −1 ). We compare the observations in the bulge region with an Auriga simulation where the last major merger event occurred ∼10 Gyr ago: only stars born around the time of the merger reveal a Splash-like feature in the V ϕ –[Fe/H] space, suggesting that the Splash is likely merger-induced, predominantly made up of heated disk stars and the starburst associated with the last major merger. Since the Splash formed from the proto-disk, its lower metallicity limit coincides with that of the thick disk. The bar formed later from the dynamically hot disk with [Fe/H] > − 1 dex, with the Splash not participating in the bar formation and growth. Moreover, with a set of isolated evolving N -body disk simulations, we confirm that a nonrotating classical bulge can be spun up by the bar and develop cylindrical rotation, consistent with the observations for the metal-poor stars.