Constraining primordial black holes in dark matter with kinematics of dwarf galaxies. (arXiv:1906.10463v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lu_B/0/1/0/all/0/1">Bo-Qiang Lu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_Y/0/1/0/all/0/1">Yue-Liang Wu</a>
We propose that the kinematical observations of dwarf galaxies can be used to
constrain the primordial black hole’s (PBH) abundance in dark matter since the
presence of primordial black holes in star clusters will lead to the radial
velocity dispersion of the system. For instance, using the velocity dispersion
observations from Leo I we show that the primordial black hole fraction $f_{rm
PBH}gtrsim 2.0times(1~M_{odot}/m_{rm PBH})^2$ is ruled out at a 99.99%
confidence level. This method yields the most stringent limits on the PBH
abundance at the mass scales $sim (1-10^3)~M_{odot}$ and tightly constrains
the primordial origin of gravitational wave events observed by the LIGO
experiments.
We propose that the kinematical observations of dwarf galaxies can be used to
constrain the primordial black hole’s (PBH) abundance in dark matter since the
presence of primordial black holes in star clusters will lead to the radial
velocity dispersion of the system. For instance, using the velocity dispersion
observations from Leo I we show that the primordial black hole fraction $f_{rm
PBH}gtrsim 2.0times(1~M_{odot}/m_{rm PBH})^2$ is ruled out at a 99.99%
confidence level. This method yields the most stringent limits on the PBH
abundance at the mass scales $sim (1-10^3)~M_{odot}$ and tightly constrains
the primordial origin of gravitational wave events observed by the LIGO
experiments.
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