Suman Chatterjee

Visiting Fellow
Email: schatterjee [at]
Phone: 020-2571 9252
Extn: 9252
Office: 218C
National Centre for Radio Astrophysics
Tata Institute of Fundamental Research
Savitribai Phule Pune University Campus,
Pune 411 007
Maharashtra, INDIA

Main Research Areas: Cosmology; Large scale structure; 21-cm cosmology.


Suman Chatterjee obtained a B.Sc. in Physics in 2010 from the University of Calcutta, an M.Sc. in Physics in 2012 from the Indian Institute of Technology-Madras, Chennai, and a Ph.D. in 2020 from the Indian Institute of Technology-Kharagpur. He joined NCRA-TIFR in March 2020 as a Visiting Post-doctoral Fellow.

Research description:

The study of phenomena at the largest cosmological scales in the late time universe has recently seen a renewed interest. This has been mostly driven by the forthcoming generation of experiments which will scrutinise the cosmic large-scale structure with unprecedented accuracy over the biggest volume ever surveyed. Hydrogen is ubiquitous in the Universe, amounting to ~75% of the gas mass present in the intergalactic medium (IGM). The 21-cm line is produced by the spin-flip transition of an electron between two hyperfine levels of the neutral Hydrogen (HI). Intensity mapping (IM) with the HI 21-cm radiation is a promising tool to study the large scale structures Universe. Several ongoing and upcoming experiments aim to detect the HI 21-cm radiation from the dark ages to the post-reionization era. The Ooty Wide Field Array (OWFA) is an upgrade of the Ooty Radio telescope (ORT) that aims to detect and measure HI 21-cm signal from redshift z = 3.35. Over the last few years, I have been working on different aspects of detecting the HI 21-cm signal using OWFA.

Selected publications:

1. Simulated Predictions for HI at z=3.35 with the Ooty Wide Field Array(OWFA) - II : Foreground Avoidance (S. Chatterjee, S. Bharadwaj and V. R. Marthi 2020, MNRAS, in press, arxiv:1911.05372)

2. On the Prospects of Measuring the Cosmic Dawn 21-cm Power Spectrum using the Upgraded
Giant Metrewave Radio Telescope (uGMRT) (S. Chatterjee and S. Bharadwaj 2019, MNRAS, 483, 2269)

3. A Spherical Harmonic Analysis of the Ooty Wide Field Array (OWFA) Visibility Signal (S. Chatterjee and S. Bharadwaj 2018, MNRAS, 478, 2915)

4. Simulated foreground predictions for HI at z = 3.35 with the Ooty Wide Field Array: I. Instrument and the foregrounds (V. R. Marthi, S. Chatterjee, J. N. Chengalur and S. Bharadwaj 2017, MNRAS, 471, 3112)

5. Simulating the z = 3.35 HI 21-cm visibility signal for the Ooty Wide Field Array(OWFA) (S. Chatterjee, S. Bharadwaj and V. R. Marthi 2017, JAA, 38, 15)