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SUMMARY:Distinguishing high-mass binary neutron stars from binary black ho
 les with gravitational waves - An Chen (University College London)
DTSTART:20200515T120000Z
DTEND:20200515T130000Z
UID:TALK141592@talks.cam.ac.uk
CONTACT:Nathan Johnson-McDaniel
DESCRIPTION:The current gravitational-wave (GW) observatories have detecte
 d tens of binary black hole (BBH) and several binary neutron star (BNS) me
 rger events in the past few years. While the GW signal of the first BNS me
 rger GW170817 was accompanied by a variety of electromagnetic (EM) counter
 parts\, sufficiently high-mass BNS mergers are expected to be unable to po
 wer bright EM counterparts. The putative high-mass BNS merger GW190425\, f
 or which no confirmed EM counterpart has been identified\, may be an examp
 le of such a system. In addition\, primordial black holes may have the sam
 e masses as neutron stars. Hence it is important to understand how well we
  will be able to distinguish high-mass BNSs and low-mass BBHs solely from 
 their GW signals. To do this\, we consider the imprint of the tidal deform
 ability of the neutron stars on the GW signal. We simulate a set of BNS si
 gnals with different total masses and equations of state\, as well as the 
 analogous BBH signals. We perform Bayesian parameter estimation on these s
 ignals in three kinds of current and future GW observatory networks. Our a
 nalysis suggests that we cannot distinguish high-mass BNSs from BBHs with 
 the current O3 network at a high credible level\, but we can distinguish t
 hem at a high credible level using the O4 network\, and even higher for th
 e third-generation network. \n
LOCATION:Zoom
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