The Cosmology Large Angular Scale Surveyor Receiver Design
Autor: | Joseph Cleary, Johannes Hubmayr, Ricardo Bustos, Gonzalo A. Palma, Kevin L. Denis, Nathan P Miller, Matthew Petroff, Jullianna Couto, Thomas Essinger-Hileman, Charles L. Bennett, Janet Weiland, Sumit Dahal, Michael K. Brewer, Tobias A. Marriage, Duncan J. Watts, Qinan Wang, Jeffrey Iuliano, Ivan L. Padilla, Lucas Parker, Karwan Rostem, Kyle Helson, Deniz Augusto Nunes Valle, David T. Chuss, Edward J. Wollack, Lingzhen Zeng, Carolina Núñez, Pedro Fluxa, John W. Appel, John Karakla, Rolando Dünner, Gene C. Hilton, Aamir Ali, Joseph Eimer, Carl D. Reintsema, Jeff McMahon, Rodrigo Reeves, Ziang Yan, Trevor Van Engelhoven, Zhilei Xu, Bingjie Wang, Bastian Pradenas Marquez, Gary Rhoades, Mark Halpern, Kathleen Harrington, Gary Hinshaw |
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Jazyk: | angličtina |
Rok vydání: | 2018 |
Předmět: |
Physics
Optical efficiency Cosmology Large Angular Scale Surveyor Stray light business.industry Cosmic microwave background Detector Astrophysics::Instrumentation and Methods for Astrophysics FOS: Physical sciences Cryogenics Astrophysics::Cosmology and Extragalactic Astrophysics Polarization (waves) 01 natural sciences 7. Clean energy 010309 optics Optics 0103 physical sciences Electromagnetic shielding business Astrophysics - Instrumentation and Methods for Astrophysics Instrumentation and Methods for Astrophysics (astro-ph.IM) 010303 astronomy & astrophysics |
Popis: | The Cosmology Large Angular Scale Surveyor consists of four instruments performing a CMB polarization survey. Currently, the 40 GHz and first 90 GHz instruments are deployed and observing, with the second 90 GHz and a multichroic 150/220 GHz instrument to follow. The receiver is a central component of each instrument's design and functionality. This paper describes the CLASS receiver design, using the first 90 GHz receiver as a primary reference. Cryogenic cooling and filters maintain a cold, low-noise environment for the detectors. We have achieved receiver detector temperatures below 50 mK in the 40 GHz instrument for 85% of the initial 1.5 years of operation, and observed in-band efficiency that is consistent with pre-deployment estimates. At 90 GHz, less than 26% of in-band power is lost to the filters and lenses in the receiver, allowing for high optical efficiency. We discuss the mounting scheme for the filters and lenses, the alignment of the cold optics and detectors, stray light control, and magnetic shielding. Fixed formatting of abstract; 20 Pages, 11 Figures, SPIE Conference Proceedings |
Databáze: | OpenAIRE |
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