Bolometers for far-infrared and submillimetre astronomy

Griffin, Matthew Joseph ORCID: https://orcid.org/0000-0002-0033-177X 2000. Bolometers for far-infrared and submillimetre astronomy. Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 444 (1-2) , pp. 397-403. 10.1016/S0168-9002(99)01413-8

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Abstract

Department of Physics, Queen Mary and Westfield College, Mile End Road, London E1 4NS, UK Received 31 August 1999; Available online 19 April 2000. Abstract Important scientific goals of far-infrared and submillimetre astronomy include measurements of anisotropies in the cosmic background radiation, deep imaging surveys for detection of high-red-shift galaxies, and imaging and spectroscopy of star formation regions and the interstellar medium in the milky way and nearby galaxies. Use of sensitive bolometer arrays leads to very large improvements in observing speed. Recent progress in the development of bolometric detector systems for ground-based and space-borne far-infrared and submillimetre astronomical observations is reviewed, including spider-web NTD bolometers, transition-edge superconducting sensors, and micromachined planar arrays of ion-implanted silicon bolometers. Future arrays may be based on planar absorbers without feedhorns, which offer potential advantages including more efficient use of space in the focal plane and improved instantaneous sampling of the telescope point spread function, but present challenges in suppression of stray light and RF interference. FIRST and Planck Surveyor are planned satellite missions involving passively cooled (∼70 K) telescopes, and bolometer array developments for these missions are described.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Schools > Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Uncontrolled Keywords:	Astronomy; Bolometers
Publisher:	North Holland
ISSN:	0168-9002
Last Modified:	18 Oct 2022 12:41
URI:	https://orca.cardiff.ac.uk/id/eprint/10928

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