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Distribution of cold gas in the post-reionization era provides an importantlink between distribution of galaxies and the process of star formation.Redshifted 21 cm radiation from the Hyperfine transition of neutral Hydrogenallows us to probe the neutral component of cold gas, most of which is to befound in the interstellar medium of galaxies. Existing and upcoming radiotelescopes can probe the large scale distribution of neutral Hydrogen via HIintensity mapping. In this paper we use an estimate of the HI power spectrumderived using an ansatz to compute the expected signal from the large scale HIdistribution at z ~ 3. We find that the scale dependence of bias at smallscales makes a significant difference to the expected signal even at largeangular scales. We compare the predicted signal strength with the sensitivityof radio telescopes that can observe such radiation and calculate theobservation time required for detecting neutral Hydrogen at these redshifts. Wefind that OWFA (Ooty Wide Field Array) offers the best possibility to detectneutral Hydrogen at z ~ 3 before the SKA (Square Kilometer Array) becomesoperational. We find that the OWFA should be able to make a 3 sigma or a moresignificant detection in 2000 hours of observations at several angular scales.Calculations done using the Fisher matrix approach indicate that a 5 sigmadetection of the binned HI power spectrum via measurement of the amplitude ofthe HI power spectrum is possible in 1000 hours (Sarkar, Bharadwaj and Ali,2017).

Prospects of detecting HI using redshifted 21 cm radiation at z ~ 3