The core-halo structure of the scalar field dark matter model

Hei Yin Jowett Chan^1*, Elisa. G. M. Ferreira^2,3, Masashi Chiba⁴, Kohei Hayashi⁵, Simon May⁷

¹Physics Division, National Center for Theoretical Sciences,, National Taiwan University, Taipei, Taiwan
²Kavli IPMU, Kashiwa, Toyko, Japan
³Institute of Physics, University of São Paulo, São Paulo, Brazil
⁴Astronomical Institute, Tohoku University, Sendai, Miyagi, Japan
⁵National Institute of Technology, Ichinoseki College, Ichinoseki,Iwate, Japan
⁶Max Planck Institute for Astrophysics, Garching, Germany
⁷Theoretical Physics, Perimeter Institute, Waterloo, Ontario, Canada

* Presenter:Hei Yin Jowett Chan, email:jchan@phys.ncts.ntu.edu.tw

The scalar field dark matter (SFDM) model was suggested to be a promising candidate that could be as equally competitive as the traditional cold dark matter (CDM) model. Since the non-linear evolution of the SFDM is governed by the coupled Schroedinger-Poisson equations, the structure formation on galactic scale are often suppressed by quantum pressure, and therefore, different from the non-linear structure of CDM model. We will recap some of the recent observational constraints on the SFDM model, and the numerical simulations performed by different groups. In this talk, we will focus on our recent finding obtained from cosmological simulations, the diversity of the core-halo structure of the SFDM model, which is closely related to the observed inner structure of faint dwarf galaxies within the Milky Way. I will conclude with a prospect on the future direction for SFDM simulations.

Keywords: Dark Matter, Simulation, Local Universe