Robust absolute solar flux density calibration for the Murchison Widefield Array

TL;DR

This paper introduces a robust, configuration-independent method for calibrating solar flux density measurements with the Murchison Widefield Array, achieving about 10% accuracy without dedicated calibrator observations.

Contribution

The authors develop a new calibration technique that does not depend on array configuration, enabling accurate solar flux measurements with MWA.

Findings

Achieved ~10% flux density uncertainty for solar observations.

Validated method using background sources and calibrator observations.

Applicable across different MWA configurations.

Abstract

Sensitive radio instruments are optimized for observing faint astronomical sources, and usually need to attenuate the received signal when observing the Sun. There are only a handful of flux density calibrators which can comfortably be observed with the same attenuation setup as the Sun. Additionally, for wide field-of-view (FoV) instruments like the Murchison Widefield Array (MWA) calibrator observations are generally done when the Sun is below the horizon to avoid the contamination from solar emissions. These considerations imply that the usual radio interferometric approach to flux density calibration is not applicable for solar imaging. A novel technique, relying on a good sky model and detailed characterization of the MWA hardware, was developed for solar flux density calibration for MWA. Though successful, this technique is not general enough to be extended to the data from the extended configuration of the MWA Phase II. Here, we present a robust flux density calibration method for solar observations with MWA independent of the array configuration. We use different approaches -- the serendipitous presence of strong sources; detection of numerous background sources using high dynamic range images in the FoV along with the Sun and observations of strong flux density calibrators with and without the additional attenuation used for solar observations; to obtain the flux scaling parameters required for the flux density calibration. Using the present method, we have achieved an absolute flux density uncertainty $\sim10\%$ for solar observations even in the absence of dedicated calibrator observations.