Dark matter accounts for roughly 85 percent of all the matter in the universe.
"The numerical challenge for studies focusing on fuzzy dark matter is that its distinguishing features, the granular density fluctuations in collapsed halos and filaments, are orders of magnitude smaller than any cosmological simulation box large enough to accurately capture the dynamics of the cosmic web," Bodo Schwabe, one of the researchers who carried out the study, explained to Phys.org.
Schwabe and Niemeyer combined both the n-body and the finite difference methods, both of which are widely used but rarely combined to perform cosmological simulations. This promoted the n-body particles to the state of coherent wave packages known as"Gaussian beams", leading to a fuzzy dark matter wave function that allowed them to perform their simulations. The researchers believe their method will help the global scientific community to better understand dark matter as a whole.
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Deep Zoom-In Simulation of a Fuzzy Dark Matter Galactic HaloFuzzy dark matter (FDM) made of ultralight bosonic particles is a viable alternative to cold dark matter with clearly distinguishable small-scale features in collapsed structures. On large scales, it behaves gravitationally like cold dark matter deviating only by a cutoff in the initial power spectrum and can be studied using $N$-body methods. In contrast, wave interference effects near the de Broglie scale result in new phenomena unique to FDM. Interfering modes in filaments and halos yield a stochastically oscillating granular structure which condenses into solitonic cores during halo formation. Investigating these highly nonlinear wave phenomena requires the spatially resolved numerical integration of the Schr\'odinger equation. In previous papers we introduced a hybrid zoom-in scheme that combines $N$-body methods to model the large-scale gravitational potential around and the mass accretion onto pre-selected halos with simulations of the Schr\'odinger-Poisson equation to capture wave-like effects inside these halos. In this work, we present a new, substantially improved reconstruction method for the wave function inside of previously collapsed structures. We demonstrate its capabilities with a deep zoom-in simulation of a well-studied sub-${L}_{*}$-sized galactic halo from cosmological initial conditions. With a particle mass of $m=2.5\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}22}\text{ }\text{ }\mathrm{eV}$ and halo mass ${M}_{\mathrm{vir}}=1.7\ifmmode\times\else\texttimes\fi{}{10}^{11}\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ in a $(60\text{ }\text{ }{\mathrm{h}}^{\ensuremath{-}1}\text{ }\text{comoving Mpc}{)}^{3}$ cosmological box, it reaches an effective resolution of 20 comoving pc. This pushes the values of $m$ and $M$ accessible to simulations significantly closer to those relevant for studying galaxy evolution in the allowed range of FDM masses.
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