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Atacama Cosmology Telescope: A measurement of galaxy cluster temperatures through relativistic corrections to the thermal Sunyaev-Zeldovich effect

William R. Coulton1,2,3, Adriaan J. Duivenvoorden4,3,5, Zachary Atkins5, Nicholas Battaglia6, Elia Stefano Battistelli7, J Richard Bond8, Hongbo Cai9, Erminia Calabrese10, Steve K. Choi11 et al.

Kevin T. Crowley12, Mark J. Devlin13, Jo Dunkley5,14, Simone Ferraro15,16, Yilun Guan17, Carlos Hervías-Caimapo18, J. Colin Hill19,3, Matt Hilton20,21, Adam D. Hincks22,23, Arthur Kosowsky9, Mathew S. Madhavacheril13, Joshiwa van Marrewijk24, Fiona McCarthy2,1,3, Kavilan Moodley21, Tony Mroczkowski25, Michael D. Niemack26,6, Lyman A. Page5, Bruce Partridge27, Emmanuel Schaan28,29, Neelima Sehgal30, Blake D. Sherwin2,1, Cristóbal Sifón31, David N. Spergel3,14, Suzanne T. Staggs5, Alexander Van Engelen32, Eve M. Vavagiakis26, and Edward J. Wollack33

Phys. Rev. D 113, 043520 – Published 18 February, 2026

DOI: https://doi.org/10.1103/n7p5-pc66

Abstract

The high electron temperature in galaxy clusters (>1keV or >107K) leads to corrections at the level of a few percent in their thermal Sunyaev-Zeldovich effect signatures. Both the size and frequency dependence of these corrections, which are known as relativistic temperature corrections, depend upon the temperature of the objects. In this work we exploit this effect to measure the average temperature of a stack of Compton-y selected clusters. Specifically, we apply the “spectroscopic method” and search for the temperature that best fits the clusters’ signal measured at frequencies from 30 to 545 GHz by the Atacama Cosmology Telescope and Planck satellite. We measure the average temperature of clusters detected in the Atacama Cosmology Telescope maps to be 8.5±2.4keV, with an additional systematic error of comparable amplitude dominated by passband uncertainty. Upcoming surveys, such as the Simons Observatory and CMB-S4, have the potential to dramatically improve upon these measurements and thereby enable precision studies of cluster temperatures with millimeter observations. The key challenge for future observations will be mitigating instrumental systematic effects, which already limit this analysis.

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