Gamma-rays from ultracompact minihalos: potential constraints on the primordial curvature perturbation

Details Gamma-rays from ultracompact minihalos: potential constraints on the primordial curvature perturbation Gamma-rays from ultracompact minihalos: potential constraints on the primordial curvature perturbation

2010-06-25

arxiv.org/abs/1006.4970v2

Phys.Rev.D82:083527,2010

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

5 pages, 2 figures, version to appear in Phys. Rev. D, minor changes

Scientific paper

10.1103/PhysRevD.82.083527

Ultracompact minihalos (UCMHs) are dense dark matter structures which can form from large density perturbations shortly after matter-radiation equality. If dark matter is in the form of Weakly Interacting Massive Particles (WIMPs), then UCMHs may be detected via their gamma-ray emission. We investigate how the {\em{Fermi}} satellite could constrain the abundance of UCMHs and place limits on the power spectrum of the primordial curvature perturbation. Detection by {\em Fermi} would put a lower limit on the UCMH halo fraction. The smallest detectable halo fraction, $f_{\rm UCMH} \gtrsim 10^{-7}$, is for $M_{\rm UCMH} \sim 10^{3} M_{\odot}$. If gamma-ray emission from UCMHs is not detected, an upper limit can be placed on the halo fraction. The bound is tightest, $f_{\rm UCMH} \lesssim 10^{-5}$, for $M_{\rm UCMH} \sim 10^{5} M_{\odot}$. The resulting upper limit on the power spectrum of the primordial curvature perturbation in the event of non-detection is in the range $\mathcal{P_R} \lesssim 10^{-6.5}- 10^{-6}$ on scales $k \sim 10^{1}-10^{6} \, {\rm Mpc}^{-1}$. This is substantially tighter than the existing constraints from primordial black hole formation on these scales, however it assumes that dark matter is in the form of WIMPs and UCMHs are not disrupted during the formation of the Milky Way halo.

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