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In this paper we explore for the first time the relative magnitudes of threefundamental sources of uncertainty, namely, foreground contamination, thermalnoise and sample variance in detecting the HI power spectrum from the Epoch ofReionization (EoR). We derive limits on the sensitivity of a Fourier synthesistelescope to detect EoR based on its array configuration and a statisticalrepresentation of images made by the instrument. We use the Murchison WidefieldArray (MWA) configuration for our studies. Using a unified framework forestimating signal and noise components in the HI power spectrum, we derive anexpression for and estimate the contamination from extragalactic point-likesources in three-dimensional k-space. Sensitivity for EoR HI power spectrumdetection is estimated for different observing modes with MWA. With 1000 hoursof observing on a single field using the 128-tile MWA, EoR detection isfeasible (S/N > 1 for $k\lesssim 0.8$ Mpc$^{-1}$). Bandpass shaping andrefinements to the EoR window are found to be effective in containingforeground contamination, which makes the instrument tolerant to imagingerrors. We find that for a given observing time, observing many independentfields of view does not offer an advantage over a single field observation whenthermal noise dominates over other uncertainties in the derived power spectrum.

A study of fundamental limitations to statistical detection of redshifted HI from the epoch of reionization