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Improved constraints on the primordial power spectrum at small scales from ultracompact minihalos

Torsten Bringmann*

Pat Scott†

Yashar Akrami‡

  • II. Institute for Theoretical Physics, University of Hamburg, Luruper Chausse 149, DE-22761 Hamburg, Germany

  • Department of Physics, McGill University, 3600 rue University, Montréal, QC, H3A 2T8, Canada

  • The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden; Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, N-0315 Oslo, Norway

  • *torsten.bringmann@desy.de
  • †patscott@physics.mcgill.ca
  • ‡yashar.akrami@astro.uio.no
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Phys. Rev. D 85, 125027 – Published 19 June, 2012

DOI: https://doi.org/10.1103/PhysRevD.85.125027

Abstract

For a Gaussian spectrum of primordial density fluctuations, ultracompact minihalos (UCMHs) of dark matter are expected to be produced in much greater abundance than, e.g., primordial black holes. Forming shortly after matter-radiation equality, these objects would develop very dense and spiky dark matter profiles. In the standard scenario where dark matter consists of thermally produced, weakly interacting massive particles, UCMHs could thus appear as highly luminous gamma-ray sources or leave an imprint in the cosmic microwave background by changing the reionization history of the Universe. We derive corresponding limits on the cosmic abundance of UCMHs at different epochs and translate them into constraints on the primordial power spectrum. We find the resulting constraints to be quite severe, especially at length scales much smaller than what can be directly probed by the cosmic microwave background or large-scale structure observations. We use our results to provide an updated compilation of the best available constraints on the power of density fluctuations on all scales, ranging from the present-day horizon to scales more than 20 orders of magnitude smaller.

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Phys. Rev. D 85, 125027– Published 19 June, 2012
  • Received 27 October 2011

© 2012 American Physical Society

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