Browsing by Author "Jing, Yingjie"

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    Bar-driven Gas Dynamics of M31
    (2024) Feng, Zi-Xuan; Li, Zhi; Shen, Juntai; Gerhard, Ortwin; Saglia, R. P.; Blana, Matias; Li, Hui; Jing, Yingjie
    The large-scale gaseous shocks in the bulge of M31 can be naturally explained by a rotating stellar bar. We use gas dynamical models to provide an independent measurement of the bar pattern speed in M31. The gravitational potentials of our simulations are from a set of made-to-measure models constrained by stellar photometry and kinematics. If the inclination of the gas disk is fixed at i = 77 degrees, we find that a low pattern speed of 16-20 km s-1 kpc-1 is needed to match the observed position and amplitude of the shock features, as shock positions are too close to the bar major axis in high omega b models. The pattern speed can increase to 20-30 km s-1 kpc-1 if the inner gas disk has a slightly smaller inclination angle compared with the outer one. Including subgrid physics such as star formation and stellar feedback has minor effects on the shock amplitude, and does not change the shock position significantly. If the inner gas disk is allowed to follow a varying inclination similar to the H i and ionized gas observations, the gas models with a pattern speed of 38 km s-1 kpc-1, which is consistent with stellar-dynamical models, can match both the shock features and the central gas features.
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    SDSS-IV MaNGA: a distinct mass distribution explored in slow-rotating early-type galaxies
    (OXFORD UNIV PRESS, 2018) Rong, Yu; Li, Hongyu; Wang, Jie; Gao, Liang; Li, Ran; Ge, Junqiang; Jing, Yingjie; Pan, Jun; Fernandez Trincado, J. G.; Valenzuela, Octavio; Aquino Ortiz, Erik
    We study the radial acceleration relation (RAR) for early-type galaxies (ETGs) in the SDSS MaNGA MPL5 data set. The complete ETG sample show a slightly offset RAR from the relation reported by McGaugh et al. (2016) at the low-acceleration end; we find that the deviation is due to the fact that the slow rotators show a systematically higher acceleration relation than the McGaugh's RAR, while the fast rotators show a consistent acceleration relation to McGaugh's RAR. There is a 1 sigma significant difference between the acceleration relations of the fast and slow rotators, suggesting that the acceleration relation correlates with the galactic spins, and that the slow rotators may have a different mass distribution compared with fast rotators and late-type galaxies. We suspect that the acceleration relation deviation of slow rotators may be attributed to more galaxy merger events, which would disrupt the original spins and correlated distributions of baryons and dark matter orbits in galaxies.