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Merging massive black holes the right place and the right time

Published online by Cambridge University Press:  29 January 2019

Astrid Lamberts Open the ORCID record for Astrid Lamberts [Opens in a new window]
Astrid Lamberts*
Affiliation:
Theoretical Astrophysics, California Institute of Technology, Pasadena, CA, 91125, USA email: lamberts@caltech.edu
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Abstract

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The LIGO/Virgo detections of gravitational waves from merging black holes of ≃ 30 solar mass suggest progenitor stars of low metallicity (Z/Z⊙ ≲ 0.3). In this talk I will provide constrains on where the progenitors of GW150914 and GW170104 may have formed, based on advanced models of galaxy formation and evolution combined with binary population synthesis models. First I will combine estimates of galaxy properties (star-forming gas metallicity, star formation rate and merger rate) across cosmic time to predict the low redshift BBH merger rate as a function of present day host galaxy mass, formation redshift of the progenitor system and different progenitor metallicities. I will show that the signal is dominated by binaries formed at the peak of star formation in massive galaxies with and binaries formed recently in dwarf galaxies. Then, I will present what very high resolution hydrodynamic simulations of different galaxy types can learn us about their black hole populations.

Keywords

galaxies:abundancesstellar contentstars:binariesblack holesevolutiongravitational waves
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S338: Gravitational Wave Astrophysics: Early Results from Gravitational Wave Searches and Electromagnetic Counterparts , October 2017 , pp. 40 - 45
Copyright
Copyright © International Astronomical Union 2019 

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