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    On detection of the stochastic gravitational-wave background using the Parkes pulsar timing array

    173479_51843_Yardley etal2011.pdf (505.7Kb)
    Access Status
    Open access
    Authors
    Yardley, D.
    Coles, W.
    Hobbs, G.
    Verbiest, J.
    Manchester R. N.
    van Straten W.
    Jenet F. A.
    Bailes M.
    Bhat, Ramesh
    Burke-Spolaor, S.
    Champion, D. J.
    Hotan, Aidan
    Oslowski, S.
    Reynolds, J. E.
    Sarkissian, J. M.
    Date
    2011
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Yardley, D. and Coles, W. and Hobbs, G. and Verbiest, J. and Manchester R.N. and van Straten W. and Jenet F. A. et al. 2011. On detection of the stochastic gravitational-wave background using the Parkes pulsar timing array. Monthly Notices of the Royal Astronomical Society. 414 (2): pp. 1777-1787.
    Source Title
    Monthly Notices of the Royal Astronomical Society
    DOI
    10.1111/j.1365-2966.2011.18517.x
    ISSN
    1365-2966
    School
    Curtin Institute of Radio Astronomy
    Remarks

    This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2011 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

    URI
    http://hdl.handle.net/20.500.11937/13890
    Collection
    • Curtin Research Publications
    Abstract

    We search for the signature of an isotropic stochastic gravitational-wave background in pulsar timing observations using a frequency-domain correlation technique. These observations, which span roughly 12 yr, were obtained with the 64-m Parkes radio telescope augmented by public domain observations from the Arecibo Observatory. A wide range of signal processing issues unique to pulsar timing and not previously presented in the literature are discussed. These include the effects of quadratic removal, irregular sampling and variable errors which exacerbate the spectral leakage inherent in estimating the steep red spectrum of the gravitational-wave background. These observations are found to be consistent with the null hypothesis that no gravitational-wave background is present, with 76 per cent confidence. We show that the detection statistic is dominated by the contributions of only a few pulsars because of the inhomogeneity of this data set. The issues of detecting the signature of a gravitational-wave background with future observations are discussed.

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