# Spectral Index of the Diffuse Radio Background Between 50 and 100 MHz

## TL;DR

This study measures the spectral index of the diffuse radio background between 50 and 100 MHz using EDGES data, revealing its variation with local sidereal time and comparison with sky models, with implications for understanding the Galactic radio emission.

## Contribution

First measurement of the spectral index of diffuse radio emission between 50 and 100 MHz with EDGES, including its variation with sidereal time and comparison to sky models.

## Key findings

- Spectral index ranges from -2.59 to -2.54, flattening near the Galactic Center.
- Measurements are stable with high night-to-night reproducibility.
- Closest sky model match is with Guzmán and Haslam maps.

## Abstract

We report the spectral index of diffuse radio emission between 50 and 100 MHz from data collected with two implementations of the Experiment to Detect the Global EoR Signature (EDGES) low-band system. EDGES employs a wide beam zenith-pointing dipole antenna centred on a declination of $-26.7^\circ$. We measure the sky brightness temperature as a function of frequency averaged over the EDGES beam from 244 nights of data acquired between 14 September 2016 to 27 August 2017. We derive the spectral index, $\beta$, as a function of local sidereal time (LST) using night-time data and a two-parameter fitting equation. We find $-2.59<\beta<-2.54 \pm 0.011$ between 0 and 12 h LST, ignoring ionospheric effects. When the Galactic Centre is in the sky, the spectral index flattens, reaching $\beta = -2.46 \pm 0.011$ at 18.2 h. The measurements are stable throughout the observations with night-to-night reproducibility of $\sigma_{\beta}<0.004$ except for the LST range of 7 to 12 h. We compare our measurements with predictions from various global sky models and find that the closest match is with the spectral index derived from the Guzm{\'a}n and Haslam sky maps, similar to the results found with the EDGES high-band instrument for 90-190 MHz. Three-parameter fitting was also evaluated with the result that the spectral index becomes more negative by $\sim$0.02 and has a maximum total uncertainty of 0.016. We also find that the third parameter, the spectral index curvature, $\gamma$, is constrained to $-0.11<\gamma<-0.04$. Correcting for expected levels of night-time ionospheric absorption causes $\beta$ to become more negative by $0.008$ - $0.016$ depending on LST.