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We present the 21 cm power spectrum analysis approach of the MurchisonWidefield Array Epoch of Reionization project. In this paper, we compare theoutputs of multiple pipelines for the purpose of validating statistical limitscosmological hydrogen at redshifts between 6 and 12. Multiple, independent,data calibration and reduction pipelines are used to make power spectrum limitson a fiducial night of data. Comparing the outputs of imaging and powerspectrum stages highlights differences in calibration, foreground subtractionand power spectrum calculation. The power spectra found using these differentmethods span a space defined by the various tradeoffs between speed, accuracy,and systematic control. Lessons learned from comparing the pipelines range fromthe algorithmic to the prosaically mundane; all demonstrate the many pitfallsof neglecting reproducibility. We briefly discuss the way these differentmethods attempt to handle the question of evaluating a significant detection inthe presence of foregrounds.

The Murchison Widefield Array 21 cm Power Spectrum Analysis Methodology