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    • Prospects of Detecting HI using Redshifted 21-cm Radiation at $z \sim 3$

      Bharat Kumar Gehlot J. S. Bagla

      Review Article Volume 38 Issue 1 March 2017 Article ID 0013

    • Fulltext

       

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      Permanent link:
      https://www.ias.ac.in/article/fulltext/joaa/038/01/0013

    • Keywords

       

      Cosmology: large scale structure of the Universe; galaxies: evolution; radio-lines: galaxies.

    • Abstract

       

      Distribution of cold gas in the post-reionization era provides an important link between distribution of galaxies and the process of star formation. Redshifted $21$-cm radiation from the hyperfine transition of neutral hydrogen allows us to probe the neutral component of cold gas, most of which is to be found in the interstellar medium of galaxies. Existing and upcoming radio telescopes can probe the large scale distribution of neutral hydrogen via HI intensity mapping. In this paper, we use an estimate of the HI power spectrum derived using an ansatz to compute the expected signal from the large scale HI distribution at $z \sim 3$. We find that the scale dependence of bias at small scales makes a significant difference to the expected signal even at large angular scales. We compare the predicted signal strength with the sensitivity of radio telescopes that can observe such radiation and calculate the observation time required for detecting neutral hydrogen at these redshifts. We find that OWFA (Ooty Wide Field Array) offers the best possibility to detect neutral hydrogen at $z \sim 3$ before the SKA (Square Kilometer Array) becomes operational. We find that the OWFA should be able to make a $3 \sigma$ or a more significant detection in $2000$ hours of observations at several angular scales. Calculations done using the Fisher matrix approach indicate that a $5\sigma$ detection of the binned HI power spectrum via measurement of the amplitude of the HI power spectrum is possible in $1000$ h (Sarkar et al. 2017).

    • Author Affiliations

       

      Bharat Kumar Gehlot1 J. S. Bagla2

      1. Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands.
      2. Department of Physical Sciences, Indian Institute of Science Education and Research Mohali, Sector 81, S.A.S. Nagar, Punjab 140 306, India.

    • Dates

       
      Published
      15 March 2017
      Manuscript received
      19 July 2016
      Accepted
      13 February 2017

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