GravPot16: A novel dynamical model to rediscovery our Milky Way

主讲人 (Speaker): Jose Fernandez-Trincado

主讲人单位 (Speaker's Institute): 智利康塞普西翁大学

邀请人 (Invited by): 汤柏添

时间 (Time): 星期四, 2018/12/20 - 15:00 to 16:00

地点 (Location): 珠海校区海滨红楼17栋107会议室

摘要 (Abstract):

In this contribution talk, I will introduce the novel galaxy modelling algorithm called GravPot16 (https://fernandez-trincado.github.io/GravPot16/), a dynamical tool originally developed in Besancon under support of the CNES and continuously improved under support of the Chilean Fondecyt. The algorithm was build-up to make a new dynamical model of the Milky Way complemented with the Besancon Galaxy model. GravPot16 is a state-of-the art orbital integration model with an (as far as possible) realistic gravitational potential, with an emphasis on the use of data from the Gaia mission along with other complimentary spectroscopic survey data, like APOGEE-2/SDSS-IV. Here, I will present the more relevant researches using GravPot16.

主讲人简介 (Speaker's CV):

Galactic dynamics: I developed the galaxy modelling algorithm called GravPot16 (web service: https://gravpot.utinam.cnrs.fr), which is designed to make a new dynamical model of the Milky Way for the orbital interpretation of future releases of the Gaia data. Numerical simulations: I have built particle simulations (~100 million particles) of multiple disk components evolved in a 3-D steady-state potential model of the Milky Way in order to infer the kinematics and orbital properties of the barred Milky Way galaxy, as well as constraining the structural parameters of the rotating-Galactic bar and spiral arms, with an emphasis on the interpretation of data from the European Space Agency’s Gaia mission along with other complimentary spectroscopic survey data like APOGEE. Data mining: Applying statistical methods on large astronomical datasets, creating mock surveys with GravPot16+Besancon galaxy model; Model comparison and structure finding. Stellar abundances: Characterization and discovery of absorptions lines associated with s-process elements (Ce II and Nd II) in H -band spectra (1.51 - 1.69 μm); line-by-line spectrum synthesis calculations for the full set of (atomic and molecular) lines of APOGEE spectra using the Brussels Automatic Stellar Parameter (BACCHUS) code and iSpec (for optical spectra). Further interests: constraints of the astrophysical sources that led to the unusual abundance patterns in the Milky Way field; multiple stellar population in metal-rich stellar clusters; integral- field spectroscopy; chemo-dynamics models of the Milky Way; variable stars as tracers of halo-substructures around globular clusters; understand the origin of the moving groups from dynamical models.