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    On modelling the Fast Radio Burst population and event rate predictions

    242011_242011.pdf (873.6Kb)
    Access Status
    Open access
    Authors
    Bera, A.
    Bhattacharyya, S.
    Bharadwaj, S.
    Bhat, Ramesh
    Chengalur, J.
    Date
    2016
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Bera, A. and Bhattacharyya, S. and Bharadwaj, S. and Bhat, R. and Chengalur, J. 2016. On modelling the Fast Radio Burst population and event rate predictions. Monthly Notices of the Royal Astronomical Society. 457 (3): pp. 2530-2539.
    Source Title
    Monthly Notices of the Royal Astronomical Society
    DOI
    10.1093/mnras/stw177
    ISSN
    1365-2966
    School
    Curtin Institute of Radio Astronomy (Physics)
    Remarks

    This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

    URI
    http://hdl.handle.net/20.500.11937/5916
    Collection
    • Curtin Research Publications
    Abstract

    Assuming that Fast Radio Bursts (FRBs) are of extragalactic origin, we have developed a formalism to predict the FRB detection rate and the redshift distribution of the detected events for a telescope with given parameters. We have adopted FRB 110220, for which the emitted pulse energy is estimated to be E0 =5.4×1033 J, as the reference event. The formalism requires us to assume models for (a) pulse broadening due to scattering in the ionized intergalactic medium – we consider two different models for this, (b) the frequency spectrum of the emitted pulse – we consider a power-law model Eν ∝ν −α with −5 ≤ α ≤ 5, and (c) the comoving number density of the FRB occurrence rate n(E, wi, z) – we ignore the z dependence and assume a fixed intrinsic pulse width wi = 1ms for all the FRBs. The distribution of the emitted pulse energy E is modelled through (a) a delta function where all the FRBs have the same energy E = E0, and (b) a Schechter luminosity function where the energies have a spread around E0. The models are all normalized using the four FRBs detected by Thornton et al. Our model predictions for the Parkes telescope are all consistent with the inferred redshift distribution of the 14 FRBs detected there to date. We also find that scattering places an upper limit on the redshift of the FRBs detectable by a given telescope; for the Parkes telescope, this is z ~ 2. Considering the upcoming Ooty Wide Field Array, we predict an FRB detection rate of ~0.01 to ~103 d−1.

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