Enabling next Generation Dark Energy and Epoch of Reionization Radio Observatories with the Moff Correlator

Proposed HI structure observatories for studying the epoch of reionization (z ≈ 6–15) and dark energy (z ≈ 0–6) envision compact arrays with tens of thousands of antenna elements. Fully correlating this many elements is computationally expensive using XF or FX correlators, and has led some groups to reconsider direct imaging/FFT correlators. In this paper we develop a variation of the direct imaging correlator we call the MOFF correlator. The MOFF correlator shares the computational advantages of a direct imaging correlator, while avoiding a number of its shortcomings. In particular the MOFF correlator makes no constraints on the antenna arrangement or type, provides a fully calibrated output image including widefield polarimetry and non-coplanar baseline effects, and can be orders-of-magnitude more efficient than XF or FX correlators for compact radio cosmology arrays.