First Limits on the 21 cm Power Spectrum during the Epoch of X-ray heating

TL;DR

This study presents initial constraints on the 21 cm power spectrum during the epoch of X-ray heating using Murchison Widefield Array data, highlighting systematic challenges and calibration needs for future cosmological measurements.

Contribution

First upper limits on the 21 cm power spectrum during redshifts 12 to 18, demonstrating the impact of calibration systematics and the importance of spectral calibration for future experiments.

Findings

RFI does not limit current measurements at the Murchison site.

Ionospheric effects are negligible for the modes of interest.

Calibration systematics dominate the current sensitivity limits.

Abstract

We present first results from radio observations with the Murchison Widefield Array seeking to constrain the power spectrum of 21 cm brightness temperature fluctuations between the redshifts of 11.6 and 17.9 (113 and 75 MHz). Three hours of observations were conducted over two nights with significantly different levels of ionospheric activity. We use these data to assess the impact of systematic errors at low frequency, including the ionosphere and radio-frequency interference, on a power spectrum measurement. We find that after the 1-3 hours of integration presented here, our measurements at the Murchison Radio Observatory are not limited by RFI, even within the FM band, and that the ionosphere does not appear to affect the level of power in the modes that we expect to be sensitive to cosmology. Power spectrum detections, inconsistent with noise, due to fine spectral structure imprinted on the foregrounds by reflections in the signal-chain, occupy the spatial Fourier modes where we would otherwise be most sensitive to the cosmological signal. We are able to reduce this contamination using calibration solutions derived from autocorrelations so that we achieve an sensitivity of $10^4$ mK on comoving scales $k\lesssim 0.5 h$Mpc$^{-1}$. This represents the first upper limits on the $21$ cm power spectrum fluctuations at redshifts $12\lesssim z \lesssim 18$ but is still limited by calibration systematics. While calibration improvements may allow us to further remove this contamination, our results emphasize that future experiments should consider carefully the existence of and their ability to calibrate out any spectral structure within the EoR window.