Non-linear clustering during the BEC dark matter phase transition

Abstract

Spherical collapse of the Bose-Einstein Condensate (BEC) dark matter model is studied in the Thomas Fermi approximation. The evolution of the overdensity of the collapsed region and its expansion rate are calculated for two scenarios. We consider the case of a sharp phase transition (which happens when the critical temperature is reached) from the normal dark matter state to the condensate one and the case of a smooth first order phase transition where there is a continuous conversion of "normal" dark matter to the BEC phase. We present numerical results for the physics of the collapse for a wide range of the model's space parameter, i.e. the mass of the scalar particle $m_{\chi }$ and the scattering length $l_s$. We show the dependence of the transition redshift on $m_{\chi }$ and $l_s$. Since small scales collapse earlier and eventually before the BEC phase transition the evolution of collapsing halos in this limit is indeed the same in both the CDM and the BEC models. Differences are expected to appear only on the largest astrophysical scales. However, we argue that the BEC model is almost indistinguishable from the usual dark matter scenario concerning the evolution of nonlinear perturbations above typical clusters scales, i.e., $\gtrsim 10^{14}{M}_{\odot }$. This provides an analytical confirmation for recent results from cosmological numerical simulations [H.-Y. Schive {\it et al.}, Nature Physics, {\bf10}, 496 (2014)].

11 pages. Final version to appear in EPJC

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• Constraints on self-interacting Bose-Einstein condensate dark matter using large-scale observables
• Cosmological simulations of self-interacting Bose-Einstein condensate dark matter
• Quantum tunneling rate of dilute axion stars close to the maximum mass
• Spherical collapse of fuzzy dark matter
• Primordial Universe with radiation and Bose-Einstein condensate