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  Expected properties of the first gravitational wave signal detected with pulsar timing arrays

Rosado, P. A., Sesana, A., & Gair, J. (2015). Expected properties of the first gravitational wave signal detected with pulsar timing arrays. Monthly Notices of the Royal Astronomical Society, 451, 2417-2433. doi:10.1093/mnras/stv1098.

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Datensatz-Permalink: http://hdl.handle.net/11858/00-001M-0000-0028-9F51-4 Versions-Permalink: http://hdl.handle.net/11858/00-001M-0000-0028-9F52-2
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 Urheber:
Rosado, Pablo A.1, Autor              
Sesana, Alberto2, Autor              
Gair, Jonathan, Autor
Affiliations:
1Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, escidoc:24011              
2Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, escidoc:24013              

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Schlagwörter: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,General Relativity and Quantum Cosmology, gr-qc
 Zusammenfassung: In this paper we attempt to investigate the nature of the first gravitational wave (GW) signal to be detected by pulsar timing arrays (PTAs): will it be an individual, resolved supermassive black hole binary (SBHB), or a stochastic background made by the superposition of GWs produced by an ensemble of SBHBs? To address this issue, we analyse a broad set of simulations of the cosmological population of SBHBs, that cover the entire parameter space allowed by current electromagnetic observations in an unbiased way. For each simulation, we construct the expected GW signal and identify the loudest individual sources. We then employ appropriate detection statistics to evaluate the relative probability of detecting each type of source as a function of time for a variety of PTAs; we consider the current International PTA, and speculate into the era of the Square Kilometre Array. The main properties of the first detectable individual SBHBs are also investigated. Contrary to previous work, we cast our results in terms of the detection probability (DP), since the commonly adopted criterion based on a signal-to-noise ratio threshold is statistic-dependent and may result in misleading conclusions for the statistics adopted here. Our results confirm quantitatively that a stochastic signal is more likely to be detected first (with between 75 to 93 per cent probability, depending on the array), but the DP of single-sources is not negligible. Our framework is very flexible and can be easily extended to more realistic arrays and to signal models including environmental coupling and SBHB eccentricity.

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 Datum: 2015-03-162015-06-222015
 Publikationsstatus: Im Druck publiziert
 Seiten: 18 pages, 7 figures, published in MNRAS
 Ort, Verlag, Ausgabe: -
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 Identifikatoren: arXiv: 1503.04803
DOI: 10.1093/mnras/stv1098
URI: http://arxiv.org/abs/1503.04803
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Titel: Monthly Notices of the Royal Astronomical Society
Genre der Quelle: Zeitschrift
 Urheber:
Affiliations:
Ort, Verlag, Ausgabe: -
Seiten: - Band / Heft: 451 Artikelnummer: - Start- / Endseite: 2417 - 2433 Identifikator: -