Multi-wavelength astronomical searches for primordial black holes. (arXiv:1812.07967v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Manshanden_J/0/1/0/all/0/1">Julien Manshanden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaggero_D/0/1/0/all/0/1">Daniele Gaggero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertone_G/0/1/0/all/0/1">Gianfranco Bertone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Connors_R/0/1/0/all/0/1">Riley M. T. Connors</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricotti_M/0/1/0/all/0/1">Massimo Ricotti</a>
If primordial black holes of $mathcal{O}(1-100) M_{odot}$ constitute a
significant portion of the dark matter in the Universe, they should be very
abundant in our Galaxy. We present here a detailed analysis of the radio and
X-ray emission that these objects are expected to produce due to the accretion
of gas from the interstellar medium. With respect to previous studies, we relax
the assumption of a monochromatic mass function, and introduce an improved
treatment of the physics of gas accretion onto isolated, moving compact
objects, based on a set of state-of-the-art numerical simulations. By comparing
our predictions with known radio and X-ray sources in the Galactic center
region, we show that the maximum relic density of primordial black holes in the
mass range of interest is $sim 10^{-3}$ smaller than that of dark matter. The
new upper bound is two orders of magnitude stronger with respect to previous
results, based on a conservative phenomenological treatment of the accretion
physics. We also provide a comprehensive critical discussion on the reliability
of this bound, and on possible future developments in the field. We argue in
particular that future multi-wavelength searches will soon start to probe the
galactic population of astrophysical black holes.
If primordial black holes of $mathcal{O}(1-100) M_{odot}$ constitute a
significant portion of the dark matter in the Universe, they should be very
abundant in our Galaxy. We present here a detailed analysis of the radio and
X-ray emission that these objects are expected to produce due to the accretion
of gas from the interstellar medium. With respect to previous studies, we relax
the assumption of a monochromatic mass function, and introduce an improved
treatment of the physics of gas accretion onto isolated, moving compact
objects, based on a set of state-of-the-art numerical simulations. By comparing
our predictions with known radio and X-ray sources in the Galactic center
region, we show that the maximum relic density of primordial black holes in the
mass range of interest is $sim 10^{-3}$ smaller than that of dark matter. The
new upper bound is two orders of magnitude stronger with respect to previous
results, based on a conservative phenomenological treatment of the accretion
physics. We also provide a comprehensive critical discussion on the reliability
of this bound, and on possible future developments in the field. We argue in
particular that future multi-wavelength searches will soon start to probe the
galactic population of astrophysical black holes.
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