Cm-wavelength Studies of Molecular Gas and Star Formation at High Redshift with the SKA

Ran Wang; Jeff Wagg; Mark T. Sargent; Manuel Aravena; Mamta Pandey-Pommier; Elisabete da Cunha; Eric Murphy; Dominik Riechers; Jacqueline Hodge

arXiv · 2606.26640

Cm-wavelength Studies of Molecular Gas and Star Formation at High Redshift with the SKA

Ran Wang·Jeff Wagg·Mark T. Sargent·Manuel Aravena·Mamta Pandey-Pommier·Elisabete da Cunha·Eric Murphy·Dominik Riechers·Jacqueline Hodge

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Abstract

The Square Kilometre Array will be a revolutionary instrument for the study of gas in the distant Universe. At frequencies below ~50 GHz, observations of redshifted emission from low-J transitions of CO, HCN, HCO+, and HNC, etc. provide insight into the kinematics and mass budget of the cold, dense star-forming gas in galaxies. Over the past decade, sensitive imaging using ALMA has detected and resolved the redshifted high-J molecular CO line emission and far-infrared fine structure lines in samples of galaxies over a wide redshift range, shedding light on active star-formation processes at the early epoch of galaxy evolution. In recent years, increasing numbers of young galaxies at high redshift are discovered by JWST, which significantly improved our knowledge of different galaxy populations across cosmic time. In this updated chapter of the SKA science book, we would like to highlight the importance of studies of the low-J molecular lines in high-z galaxies using SKA toward high frequencies, discussing the request of frequency coverage beyond 15 GHz and emphasizing its crucial role in exploring the cold molecular gas content in the young galaxy populations in the early universe and investigating the regions of active-star formation using molecular CO and various dense gas tracers.

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Ran Wang, Jeff Wagg, Mark T. Sargent, Manuel Aravena, Mamta Pandey-Pommier, Elisabete da Cunha, Eric Murphy, Dominik Riechers, Jacqueline Hodge. 2026-06-25. Cm-wavelength Studies of Molecular Gas and Star Formation at High Redshift with the SKA. https://arxiv.org/abs/2606.26640

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