A Fully Self-Consistent Cosmological Simulation Pipeline for Interacting
  Dark Energy Models
  We devise a fully self-consistent simulation pipeline for the first time to
study the interaction between dark matter and dark energy. We perform
convergence tests and show that our code is accurate on different scales. Using
the parameters constrained by Planck, Type Ia Supernovae, Baryon Acoustic
Oscillations (BAO) and Hubble constant observations, we perform cosmological
N-body simulations. We calculate the resulting matter power spectra and halo
mass functions for four different interacting dark energy models. In addition
to the dark matter density distribution, we also show the inhomogeneous density
distribution of dark energy. With this new simulation pipeline, we can further
refine and constrain interacting dark energy models.
