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  Gravitational wave astronomy with the SKA

Janssen, G. H., Hobbs, G., McLaughlin, M., Bassa, C. G., Deller, A. T., Kramer, M., et al. (2015). Gravitational wave astronomy with the SKA. Proceedings of Science, PoS(AASKA14), 037. Retrieved from http://arxiv.org/abs/1501.00127.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0025-68B8-8 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-002B-A08C-E
Genre: Conference Paper

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 Creators:
Janssen, G. H.1, Author
Hobbs, G., Author
McLaughlin, M., Author
Bassa, C. G., Author
Deller, A. T., Author
Kramer, M., Author
Lee, K. J., Author
Mingarelli, C. M. F., Author
Rosado, P. A.2, Author              
Sanidas, S., Author
Sesana, A.3, Author              
Shao, L., Author
Stairs, I. H., Author
Stappers, B. W., Author
Verbiest, J. P. W., Author
Affiliations:
1ASTRON, ou_persistent22              
2Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24011              
3Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013              

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Free keywords: Astrophysics, Instrumentation and Methods for Astrophysics, astro-ph.IM, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 Abstract: On a time scale of years to decades, gravitational wave (GW) astronomy will become a reality. Low frequency (nanoHz) GWs are detectable through long-term timing observations of the most stable pulsars. Radio observatories worldwide are currently carrying out observing programmes to detect GWs, with data sets being shared through the International Pulsar Timing Array project. One of the most likely sources of low frequency GWs are supermassive black hole binaries (SMBHBs), detectable as a background due to a large number of binaries, or as continuous or burst emission from individual sources. No GW signal has yet been detected, but stringent constraints are already being placed on galaxy evolution models. The SKA will bring this research to fruition. In this chapter, we describe how timing observations using SKA1 will contribute to detecting GWs, or can confirm a detection if a first signal already has been identified when SKA1 commences observations. We describe how SKA observations will identify the source(s) of a GW signal, search for anisotropies in the background, improve models of galaxy evolution, test theories of gravity, and characterise the early inspiral phase of a SMBHB system. We describe the impact of the large number of millisecond pulsars to be discovered by the SKA; and the observing cadence, observation durations, and instrumentation required to reach the necessary sensitivity. We describe the noise processes that will influence the achievable precision with the SKA. We assume a long-term timing programme using the SKA1-MID array and consider the implications of modifications to the current design. We describe the possible benefits from observations using SKA1-LOW. Finally, we describe GW detection prospects with SKA1 and SKA2, and end with a description of the expectations of GW astronomy.

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 Dates: 2014-12-3120152015
 Publication Status: Published online
 Pages: 19 pages, 3 figures, to be published in: "Advancing Astrophysics with the Square Kilometre Array", Proceedings of Science, PoS(AASKA14)037
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 Identifiers: arXiv: 1501.00127
URI: http://arxiv.org/abs/1501.00127
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Title: Advancing Astrophysics with the Square Kilometre Arra
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Title: Proceedings of Science, PoS(AASKA14)
Source Genre: Journal
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Pages: - Volume / Issue: - Sequence Number: 037 Start / End Page: - Identifier: -