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    • Prospects of detecting fast radio bursts using Indian radio telescopes

      SIDDHARTHA BHATTACHARYYA

      Review Volume 39 Issue 4 August 2018 Article ID 0047

    • Fulltext

       

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      Permanent link:
      https://www.ias.ac.in/article/fulltext/joaa/039/04/0047

    • Keywords

       

      Cosmology; observations.

    • Abstract

       

      Fast Radio Bursts (FRBs) are short duration highly energetic dispersed radio pulses.We developed a generic formalism (Bera et al. 2016, MNRAS, 457, 2530) to estimate the FRB detection rate for any radiotelescope with given parameters. By using this model, we estimated the FRB detection rate for two Indian radio telescope; the Ooty Wide Field Array (OWFA) (Bhattacharyya et al. 2017, J. Astrophys. Astr., 38, 17)and the upgraded Giant Metrewave Radio Telescope (uGMRT) (Bhattacharyya et al. 2018, J. Astrophys. Astr.) with three beam-forming modes. Here, we summarize these two works.We considered the energy spectrum ofFRBs as a power law and the energy distribution of FRBs as a Dirac delta function and a Schechter luminosity function.We also considered two scattering models proposed by Bhat et al. (2004, Astrophys. J. Suppl. Series,206, 1) and Macquart & Koay (2013, ApJ, 776, 125) for these works and we consider FRB pulse without scattering as a special case. We found that the future prospects of detecting FRBs by using these two Indian radio telescopes is good. They are capable to detect a significant number of FRBs per day. According to our prediction, we can detect $\sim$10$^5$−10$^8$, $\sim$10$^3$−10$^6$ and $\sim$10$^5$−10$^7$ FRBs per day by using OWFA, commensal systems of GMRT and uGMRT respectively. Even a non detection of the predicted events will be very useful in constraining FRB properties.

    • Author Affiliations

       

      SIDDHARTHA BHATTACHARYYA1

      1. Department of Physics, Indian Institute of Technology Kharagpur, Kharagpur 721 302, India.

    • Dates

       
      Published
      30 August 2018
      Manuscript received
      10 May 2018
      Accepted
      24 July 2018
      Final version published online
      23 August 2018

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