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Issue A&A
Volume 502, Number 1, July IV 2009
Page(s) 37 - 43
Section Cosmology (including clusters of galaxies)
DOI http://dx.doi.org/10.1051/0004-6361/200911961
Published online 04 June 2009

A&A 502, 37-43 (2009)
DOI: 10.1051/0004-6361/200911961

New constraints on the primordial black hole number density from Galactic $\gamma$-ray astronomy

R. Lehoucq1, M. Cassé1, 2, J.-M. Casandjian1, and I. Grenier1

1  Laboratoire AIM, CEA-Irfu/CNRS/Université Paris Diderot, Service d'astrophysique, CEA-Saclay, 91191 Gif-sur-Yvette, France
    e-mail: lehoucq@cea.fr
2  Institut d'Astrophysique, 98 bis boulevard Arago, 75014 Paris, France

Received 27 February 2009 / Accepted 18 May 2009

Abstract
Context. Primordial black holes are unique probes of cosmology, general relativity, quantum gravity and non standard particle physics. They open a new window on the very small scales in the early Universe and also can be considered as the ultimate particle accelerator in their last (explosive) moments since they are supposed to reach, very briefly, the Planck temperature.
Aims. Upper limits on the primordial black hole number density of mass $M_{\star}$ = 5$\times$1014 g, the Hawking mass (born in the big-bang terminating their life presently), is determined comparing their predicted cumulative $\gamma$-ray emission, galaxy-wise, to the one observed by the EGRET satellite, once corrected for non thermal $\gamma$-ray background emission induced by cosmic ray protons and electrons interacting with light and matter in the Milky Way.
Methods. A model with free gas emissivities is used to map the Galaxy in the 100 MeV photon range, where the peak of the primordial black hole emission is expected. The best gas emissivities and additional model parameters are obtained by fitting the EGRET data and are used to derive the maximum emission of the primordial black hole of the Hawking mass, assuming that they are distributed like the dark matter in the Galactic halo.
Results. The bounds we obtain, depending on the dark matter distribution, extrapolated to the whole Universe ($\Omega_{\rm PBH}(M_{\star})$ = 2.4$\times$10-10 to 2.6$\times$10-9) are more stringent than the previous ones derived from extragalactic $\gamma$-ray background and antiprotons fluxes, though less model dependent and based on more robust data.
Conclusions. These new limits have interesting consequences on the theory of the formation of small structures in the Universe, since they are the only constraint on very small scale density fluctuations left by inflation. Significant improvements by data gathered by the FERMI $\gamma$-ray satellite are expected in the near future. The interest of a generalisation of this work beyond the standard particle model and in extradimensions is briefly alluded.


Key words: gamma rays: observations -- Galaxy: center -- cosmology: dark matter -- gamma rays: theory -- black hole physics



© ESO 2009

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