Mapping the Milky Way Disk Population Structures and Galactoseismology with large sky surveys (MWDPSG)

Abstract: In the Gaia era, with the help of Large sky surveys such as current RAVE, LAMOST, APOGEE, GALAH, TESS, DESI catalog and future plans such as WEAVE, 4MOST, PFS, MSE, CSST, etc. There is no doubt that we are entering into the golden era to investigate the formation history and structure of our home galaxy in multiple stellar populations of six-phase space by chemical tagging, time tagging, kinematics and dynamics. Our home galaxy is a typical dynamic systems that are perturbed by bars, spiral arms, warp, giant molecular clouds, dark matter subhalos, Gaia-Sausage-Enceladus, Sagittarius, LMC&SMC, tidally disrupt satellite galaxies and so on. These processes will leave behind some imprints on stars, demonstrating abundant population structures dominated by dynamics and Galactoseismology signals. We plan to Mapping the Milky Way Disk Population Structures and Galactoseismology with large sky surveys. We will try our best to figure out: what about the population morphology of the outskirts ? Where is the truncation and how about disk stability? What are the mechanisms for so many asymmetric substructures and Galactoseismology? How do the dark matter halo, bars, spiral arms, satellites interact with the stellar, gas and dust disk? etc. Thus then, We could establish a possible theoretical framework in the future to unify or partly unify the global picture of the disk structures and origins with a possible comprehensive distribution function. There is still a long way for us to go with this project, in this talk, I will share some recent new progress about the Galactic disk with LAMOST and Gaia data, and some preliminary simulation results.


Hai-Feng Wang (王海峰)
Meeting ID: 822 8287 7472 Passcode: astroPKU
Monday, September 20, 2021 - 1:30PM to Monday, September 20, 2021 - 3:30PM