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Gravitational waves from resolvable massive black hole binary systems and observations with Pulsar Timing Arrays

dc.contributor.authorSesana, Albertoen_US
dc.contributor.authorVecchio, A.en_US
dc.contributor.authorVolonteri, Martaen_US
dc.date.accessioned2010-06-01T22:22:36Z
dc.date.available2010-06-01T22:22:36Z
dc.date.issued2009-04-21en_US
dc.identifier.citationSesana, A.; Vecchio, A.; Volonteri, M. (2009). "Gravitational waves from resolvable massive black hole binary systems and observations with Pulsar Timing Arrays." Monthly Notices of the Royal Astronomical Society 394(4): 2255-2265. <http://hdl.handle.net/2027.42/75371>en_US
dc.identifier.issn0035-8711en_US
dc.identifier.issn1365-2966en_US
dc.identifier.urihttps://hdl.handle.net/2027.42/75371
dc.description.abstractMassive black holes are key components of the assembly and evolution of cosmic structures, and a number of surveys are currently on going or planned to probe the demographics of these objects and to gain insight into the relevant physical processes. Pulsar Timing Arrays (PTAs) currently provide the only means to observe gravitational radiation from massive black hole binary systems with masses >10 7  M ⊙ . The whole cosmic population produces a stochastic background that could be detectable with upcoming PTAs. Sources sufficiently close and/or massive generate gravitational radiation that significantly exceeds the level of the background and could be individually resolved. We consider a wide range of massive black hole binary assembly scenarios, investigate the distribution of the main physical parameters of the sources, such as masses and redshift, and explore the consequences for PTAs observations. Depending on the specific massive black hole population model, we estimate that on average at least one resolvable source produces timing residuals in the range ∼5–50 ns . PTAs, and in particular the future Square Kilometre Array, can plausibly detect these unique systems, although the events are likely to be rare. These observations would naturally complement on the high-mass end of the massive black hole distribution function future surveys carried out by the Laser Interferometer Space Antenna .en_US
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dc.format.extent3109 bytes
dc.format.mimetypeapplication/pdf
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dc.publisherBlackwell Publishing Ltden_US
dc.rightsJournal compilation © 2009 RASen_US
dc.subject.otherBlack Hole Physicsen_US
dc.subject.otherGravitational Wavesen_US
dc.subject.otherPulsars: Generalen_US
dc.subject.otherCosmology: Theoryen_US
dc.titleGravitational waves from resolvable massive black hole binary systems and observations with Pulsar Timing Arraysen_US
dc.typeArticleen_US
dc.subject.hlbsecondlevelAstronomyen_US
dc.subject.hlbtoplevelScienceen_US
dc.description.peerreviewedPeer Revieweden_US
dc.contributor.affiliationumDepartment of Astronomy, University of Michigan, Ann Arbor, MI 48109, USAen_US
dc.contributor.affiliationotherCenter for Gravitational Wave Physics, The Pennsylvania State University, University Park, PA 16802, USAen_US
dc.contributor.affiliationotherSchool of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TTen_US
dc.description.bitstreamurlhttp://deepblue.lib.umich.edu/bitstream/2027.42/75371/1/j.1365-2966.2009.14499.x.pdf
dc.identifier.doi10.1111/j.1365-2966.2009.14499.xen_US
dc.identifier.sourceMonthly Notices of the Royal Astronomical Societyen_US
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