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  Reconstructing the massive black hole cosmic history through gravitational waves

Sesana, A., Gair, J. R., Berti, E., & Volonteri, M. (2011). Reconstructing the massive black hole cosmic history through gravitational waves. Physical Review D, 83(4): 044036. doi:10.1103/PhysRevD.83.044036.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-000F-1056-F Version Permalink: http://hdl.handle.net/11858/00-001M-0000-000F-1057-D
Genre: Journal Article

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Sesana, Alberto1, Author              
Gair, Jonathan R., Author
Berti, Emanuele, Author
Volonteri, Marta, Author
Affiliations:
1Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013              

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Free keywords: Astrophysics, Cosmology and Extragalactic Astrophysics, astro-ph.CO,General Relativity and Quantum Cosmology, gr-qc
 Abstract: The massive black holes we observe in galaxies today are the natural end-product of a complex evolutionary path, in which black holes seeded in proto-galaxies at high redshift grow through cosmic history via a sequence of mergers and accretion episodes. Electromagnetic observations probe a small subset of the population of massive black holes (namely, those that are active or those that are very close to us), but planned space-based gravitational-wave observatories such as the Laser Interferometer Space Antenna (LISA) can measure the parameters of ``electromagnetically invisible'' massive black holes out to high redshift. In this paper we introduce a Bayesian framework to analyze the information that can be gathered from a set of such measurements. Our goal is to connect a set of massive black hole binary merger observations to the underlying model of massive black hole formation. In other words, given a set of observed massive black hole coalescences, we assess what information can be extracted about the underlying massive black hole population model. For concreteness we consider ten specific models of massive black hole formation, chosen to probe four important (and largely unconstrained) aspects of the input physics used in structure formation simulations: seed formation, metallicity ``feedback'', accretion efficiency and accretion geometry. For the first time we allow for the possibility of ``model mixing'', by drawing the observed population from some combination of the ``pure'' models that have been simulated. A Bayesian analysis allows us to recover a posterior probability distribution for the ``mixing parameters'' that characterize the fractions of each model represented in the observed distribution. Our work shows that LISA has enormous potential to probe the underlying physics of structure formation.

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 Dates: 2010-11-252011
 Publication Status: Published in print
 Pages: 24 pages, 16 figures, submitted to Phys. Rev. D
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 Identifiers: arXiv: 1011.5893
DOI: 10.1103/PhysRevD.83.044036
URI: http://arxiv.org/abs/1011.5893
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Title: Physical Review D
  Other : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : Published for the American Physical Society by the American Institute of Physics
Pages: - Volume / Issue: 83 (4) Sequence Number: 044036 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: /journals/resource/111088197762258