Solar Observing with the Atacama Large Millimeter-Submillimeter Array

TL;DR

ALMA has revolutionized solar physics by providing high-resolution millimeter and sub-millimeter observations, enabling new insights into solar phenomena with advanced data processing and imaging techniques.

Contribution

This paper reviews ALMA's current solar observing capabilities, data calibration, imaging techniques, and discusses future modes to enhance solar research.

Findings

ALMA offers high-resolution solar observations at millimeter wavelengths.

Development of new data calibration and imaging strategies.

Discussion of future observing modes for solar physics.

Abstract

The Atacama Large Millimeter-submillimeter Array (ALMA), sited on the high desert plains of Chajnantor in Chile, has opened a new window onto solar physics in 2016 by providing continuum observations at millimeter and sub-millimeter wavelengths with an angular resolution comparable to that available at optical (O), ultraviolet (UV), extreme ultraviolet (EUV), and X-ray wavelengths, and with superior time resolution. In the intervening years, progress has been made testing and commissioning new observing modes and capabilities, in developing data calibration strategies, and in data imaging and restoration techniques. Here we review ALMA current solar observing capabilities, the process by which a user may propose to use the instrument, and summarize the observing process and work flow. We then discuss some of the challenges users may encounter in imaging and analyzing their data. We conclude with a discussion of additional solar observing capabilities and modes under consideration that are intended to further exploit the unique spectral coverage provided by ALMA.