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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7103
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dc.contributor.authorGalitzki, Nicholas-
dc.contributor.authorAli, Aamir-
dc.contributor.authorSathyanarayana Rao, Mayuri-
dc.contributor.author+74 Co-authors-
dc.date.accessioned2018-12-23T19:06:36Z-
dc.date.available2018-12-23T19:06:36Z-
dc.date.issued2018-
dc.identifier.citationProceedings of the SPIE Vol. 10708, p1070804, 2018 , Proceedings of Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX, edited by Jonas Zmuidzinas, Jian-Rong Gaoen_US
dc.identifier.issn0277-786X-
dc.identifier.issn1996-756X (electronic)-
dc.identifier.urihttp://hdl.handle.net/2289/7103-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en_US
dc.description.abstractThe Simons Observatory (SO) will make precise temperature and polarization measurements of the cosmic microwave background (CMB) using a set of telescopes which will cover angular scales between 1 arcminute and tens of degrees, contain over 60,000 detectors, and observe at frequencies between 27 and 270 GHz. SO will consist of a 6m aperture telescope coupled to over 30,000 transition-edge sensor bolometers along with three 42 cm aperture refractive telescopes, coupled to an additional 30,000+ detectors, all of which will be located in the Atacama Desert at an altitude of 5190 m. The powerful combination of large and small apertures in a CMB observatory will allow us to sample a wide range of angular scales over a common survey area. SO will measure fundamental cosmological parameters of our universe, constrain primordial uctuations, nd high redshift clusters via the Sunyaev-Zeldovich e ect, constrain properties of neutrinos, and trace the density and velocity of the matter in the universe over cosmic time. The complex set of technical and science requirements for this experiment has led to innovative instrumentation solutions which we will discuss. The large aperture telescope will couple to a cryogenic receiver that is 2.4m in diameter and nearly 3m long, creating a number of technical challenges. Concurrently, we are designing the array of cryogenic receivers housing the 42 cm aperture telescopes. We will discuss the sensor technology SO will use and we will give an overview of the drivers for and designs of the SO telescopes and receivers, with their cold optical components and detector arrays.en_US
dc.language.isoenen_US
dc.publisherSociety of Photo-Optical Instrumentation Engineers (SPIE)en_US
dc.relation.urihttp://arXiv:1808.10037en_US
dc.relation.urihttps://doi.org/10.1117/12.2312985en_US
dc.rights2018 Society of Photo-Optical Instrumentation Engineers (SPIE)en_US
dc.subjectSimons Observatoryen_US
dc.subjectmillimeter wavelengthsen_US
dc.subjectCMBen_US
dc.subjectcryogenicsen_US
dc.subjectbolometric cameraen_US
dc.subjecttransition-edge sensoren_US
dc.subjectmicrowave multiplexing readouten_US
dc.subjecthalf-wave plateen_US
dc.titleThe Simons Observatory: instrument overview Nicholasen_US
dc.typeArticleen_US
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