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The Simons Observatory Detectors: Fr...

Sonka, Rita F.,

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The Simons Observatory Detectors: From Specification to Sky /

紀錄類型:	書目-電子資源 : Monograph/item
正題名/作者:	The Simons Observatory Detectors: From Specification to Sky // Rita F Sonka.
作者:	Sonka, Rita F.,
面頁冊數:	1 electronic resource (186 pages)
附註:	Source: Dissertations Abstracts International, Volume: 86-12, Section: B.
Contained By:	Dissertations Abstracts International86-12B.
標題:	Astrophysics. -
電子資源:	https://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=31768392
ISBN:	9798280750012

The Simons Observatory Detectors: From Specification to Sky /
Sonka, Rita F.,

The Simons Observatory Detectors: From Specification to Sky /Rita F Sonka. - 1 electronic resource (186 pages)

Source: Dissertations Abstracts International, Volume: 86-12, Section: B.

The Cosmic Microwave Background (CMB) is the oldest observable radiation in our universe. The small fluctuations in its nearly uniform 2.7 K blackbody spectrum encode information on events spanning in time from the Big Bang to the modern day which can inform and test critical theories in cosmology and high energy physics. Most ground-based observatories use superconducting cryogenic Transition Edge Sensors (TESs) to detect the CMB. These detectors have become so sensitive that the main route by which scientists can improve on existing CMB maps is by increasing the number of detectors in a telescope's focal plane, to collect as many of the relatively scarce CMB photons as possible.The Simons Observatory collaboration (SO) that aims to observe the Cosmic Microwave Background with unprecedented precision and create high-resolution sky maps with up to an order of magnitude lower polarization noise than maps from the Planck satellite. SO will do so by using an ambitious microwave multiplexing (µMUX) scheme in which a single pair of RF (Radio Frequency) lines reads out O(1000) detectors to enable fielding dense focal planes with, in total, over 100,000 detectors. High-yield, good-sensitivity detector modules are critical to SO's mission to provide new information about the universe. After introducing some of the scientific aims of SO, this thesis focuses on describing some of the critical steps in optimizing the SO detectors and their readout. Ch. 2 describes the design, construction, testing and use of a wafer screener and miniature detector modules during the research and development process for SO. Ch. 3 describes the calculations and methods used to specify detector parameters. Ch. 4 describes the development and execution of the methods used to test and characterize tens of thousands of detectors in their final quarters, the Universal Focal Plane Modules (UFMs). It describes what systematic errors can arise therein, and some recent improvements to the analysis of detector IV curves. Finally, Ch. 5 briefly illustrates these concepts with IV curve data taken in the field.

English

ISBN: 9798280750012Subjects--Topical Terms:

535904
Astrophysics.
Subjects--Index Terms:

Cosmic Microwave Background

The Simons Observatory Detectors: From Specification to Sky /
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520 $a The Cosmic Microwave Background (CMB) is the oldest observable radiation in our universe. The small fluctuations in its nearly uniform 2.7 K blackbody spectrum encode information on events spanning in time from the Big Bang to the modern day which can inform and test critical theories in cosmology and high energy physics. Most ground-based observatories use superconducting cryogenic Transition Edge Sensors (TESs) to detect the CMB. These detectors have become so sensitive that the main route by which scientists can improve on existing CMB maps is by increasing the number of detectors in a telescope's focal plane, to collect as many of the relatively scarce CMB photons as possible.The Simons Observatory collaboration (SO) that aims to observe the Cosmic Microwave Background with unprecedented precision and create high-resolution sky maps with up to an order of magnitude lower polarization noise than maps from the Planck satellite. SO will do so by using an ambitious microwave multiplexing (µMUX) scheme in which a single pair of RF (Radio Frequency) lines reads out O(1000) detectors to enable fielding dense focal planes with, in total, over 100,000 detectors. High-yield, good-sensitivity detector modules are critical to SO's mission to provide new information about the universe. After introducing some of the scientific aims of SO, this thesis focuses on describing some of the critical steps in optimizing the SO detectors and their readout. Ch. 2 describes the design, construction, testing and use of a wafer screener and miniature detector modules during the research and development process for SO. Ch. 3 describes the calculations and methods used to specify detector parameters. Ch. 4 describes the development and execution of the methods used to test and characterize tens of thousands of detectors in their final quarters, the Universal Focal Plane Modules (UFMs). It describes what systematic errors can arise therein, and some recent improvements to the analysis of detector IV curves. Finally, Ch. 5 briefly illustrates these concepts with IV curve data taken in the field.
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