The Atacama Cosmology Telescope: The Receiver and Instrumentation

TL;DR

The Atacama Cosmology Telescope employs advanced cryogenic bolometer arrays to measure small-scale CMB anisotropies and galaxy clusters, providing high-resolution data for cosmological research.

Contribution

This paper introduces the design, construction, and performance of the new receiver and instrumentation of the Atacama Cosmology Telescope, including the innovative bolometer arrays and optical systems.

Findings

Successful deployment of 1000-element bolometer arrays at multiple frequencies

High-quality measurements of CMB anisotropies achieved

Operational performance data of the telescope and receiver systems

Abstract

The Atacama Cosmology Telescope was designed to measure small-scale anisotropies in the Cosmic Microwave Background and detect galaxy clusters through the Sunyaev-Zel'dovich effect. The instrument is located on Cerro Toco in the Atacama Desert, at an altitude of 5190 meters. A six-meter off-axis Gregorian telescope feeds a new type of cryogenic receiver, the Millimeter Bolometer Array Camera. The receiver features three 1000-element arrays of transition-edge sensor bolometers for observations at 148 GHz, 218 GHz, and 277 GHz. Each detector array is fed by free space mm-wave optics. Each frequency band has a field of view of approximately 22' x 26'. The telescope was commissioned in 2007 and has completed its third year of operations. We discuss the major components of the telescope, camera, and related systems, and summarize the instrument performance.