📝 SummarXiv

Abstract

Precise measurement of the sky radio brightness below 1 GHz and estimation of any unaccounted-for extragalactic brightness is required to understand the Galactic cosmic ray electron spectrum, to constrain populations of nanojansky radio sources, and to constrain dark matter annihilation or decay. The foreground radio brightness must also be accurately accounted for when measuring the cosmic background radiation and departures from its Planck spectrum that trace astrophysical processes in the early Universe, cosmic dark ages, cosmic dawn and the epoch of reionisation. Here we report a new, precision measurement of the sky spectral brightness over radio frequencies from 60 MHz to 350 MHz. Our measurement motivates a significant correction to previous all-sky images made in this band and the Global Sky Model (GSM) that is constructed from these and other sky images made at radio wavelengths. We find that the GSM requires subtraction of an offset exceeding 100K below 100 MHz and scaling up by a factor of approximately 1.2 below 200 MHz rising to a factor of 1.5 at 350 MHz, thus significantly enhancing previous estimates of unaccounted excess in radio sky brightness. Our measurements were made with a new receiver architecture that dynamically self-calibrates for receiver noise and bandpass in situ, while connected to an antenna. We used a single, accurately modelled, wideband logperiodic antenna placed on a 40m diameter ground mesh. Our accurate measurement requires upward revision of sky brightness and motivates revisiting models for source populations and dark matter decay. Additionally, sky models scaled to our measurements serve as a stable reference in calibrating the absolute flux density scale for low-frequency radio telescopes. This will be important for calibration accuracy of the SKA-Low telescope, that will operate at the frequencies of our measurements.