Constraining Black Hole Populations in Globular Clusters using Microlensing: Application to Omega Centauri. (arXiv:1912.05701v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zaris_J/0/1/0/all/0/1">John Zaris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Veske_D/0/1/0/all/0/1">Doğa Veske</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Samsing_J/0/1/0/all/0/1">Johan Samsing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marka_Z/0/1/0/all/0/1">Zsuzsa Márka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bartos_I/0/1/0/all/0/1">Imre Bartos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marka_S/0/1/0/all/0/1">Szabolcs Márka</a>
We estimate the rate of gravitational microlensing events of cluster stars
due to black holes (BHs) in the globular cluster NGC 5139 ($omega Cen$).
Theory and observations both indicate that $omega Cen$ contains thousands of
BHs, but their mass spectrum and exact distribution are not well constrained.
In this Letter we show that one is able to observe microlensing events on a
timescale of years in $omega Cen$, and such an event sample can be used to
infer the BH distribution. Direct detection of BHs will, in the near future,
play a major role in distinguishing binary BH merger channels. Here we explore
how gravitational microlensing can be used to put constraints on BH populations
in globular clusters.
We estimate the rate of gravitational microlensing events of cluster stars
due to black holes (BHs) in the globular cluster NGC 5139 ($omega Cen$).
Theory and observations both indicate that $omega Cen$ contains thousands of
BHs, but their mass spectrum and exact distribution are not well constrained.
In this Letter we show that one is able to observe microlensing events on a
timescale of years in $omega Cen$, and such an event sample can be used to
infer the BH distribution. Direct detection of BHs will, in the near future,
play a major role in distinguishing binary BH merger channels. Here we explore
how gravitational microlensing can be used to put constraints on BH populations
in globular clusters.
http://arxiv.org/icons/sfx.gif
