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    FRB Event Rate Predictions for the Ooty Wide Field Array

    Access Status
    Fulltext not available
    Authors
    Bhattacharyya, S.
    Bera, A.
    Bharadwaj, S.
    Bhat, Ramesh
    Chengalur, J.
    Date
    2017
    Type
    Journal Article
    
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    Citation
    Bhattacharyya, S. and Bera, A. and Bharadwaj, S. and Bhat, R. and Chengalur, J. 2017. FRB Event Rate Predictions for the Ooty Wide Field Array. Journal of Astrophysics and Astronomy. 38 (1).
    Source Title
    Journal of Astrophysics and Astronomy
    DOI
    10.1007/s12036-017-9431-3
    ISSN
    0250-6335
    School
    Curtin Institute of Radio Astronomy (Physics)
    URI
    http://hdl.handle.net/20.500.11937/52780
    Collection
    • Curtin Research Publications
    Abstract

    © 2017, Indian Academy of Sciences.We developed a generic formalism to estimate the event rate and the redshift distribution of Fast Radio Bursts (FRBs) in our previous publication (Bera et al. 2016), considering FRBs are of an extragalactic origin. In this paper, we present (a) the predicted pulse widths of FRBs by considering two different scattering models, (b) the minimum total energy required to detect events, (c) the redshift distribution and (d) the detection rates of FRBs for the Ooty Wide Field Array (OWFA). The energy spectrum of FRBs is modelled as a power law with an exponent -a and our analysis spans a range -3=a=5. We find that OWFA will be capable of detecting FRBs with a=0. The redshift distribution and the event rates of FRBs are estimated by assuming two different energy distribution functions; a Delta function and a Schechter luminosity function with an exponent -2=?=2. We consider an empirical scattering model based on pulsar observations (model I) as well as a theoretical model (model II) expected for the intergalactic medium. The redshift distributions peak at a particular redshift zp for a fixed value of a, which lie in the range 0.3=zp=1 for the scattering model I and remain flat and extend up to high redshifts (z?5) for the scattering model II.

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