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Record 1 of 52
High Spectral Resolution, High Cadence, Imaging X-Ray Microcalorimeters for Solar Physics
External Online Source: doi:10.1117/12.857783
Author and Affiliation:
Bandler, Simon R.(Maryland Univ., CRESST, College Park, MD, United States)
Bailey, Catherine N.(Oak Ridge Associated Universities, Inc., NASA Postdoctoral Program Resident Research Associate, TN, United States)
Bookbinder, Jay A.(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, United States)
DeLuca, Edward E.(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, United States)
Chervenak, Jay A.(NASA Goddard Space Flight Center, Greenbelt, MD, United States)
Eckart, Megan E.(Maryland Univ. Baltimore County, NASA Postdoctoral Program Resident Research Associate, Baltimore, MD, United States)
Finkbeiner, Fred M.(Wyle Information Systems, LLC, McLean, VA, United States)
Kelley, Daniel P.(MEI Technologies, Inc., Seabrook, MD, United States)
Kelley, Richard L.(NASA Goddard Space Flight Center, Greenbelt, MD, United States)
Kilbourne, Caroline A.(NASA Goddard Space Flight Center, Greenbelt, MD, United States) Show more authors
Abstract: High spectral resolution, high cadence, imaging x-ray spectroscopy has the potential to revolutionize the study of the solar corona. To that end we have been developing transition-edge-sensor (TES) based x-ray micro calorimeter arrays for future solar physics missions where imaging and high energy resolution spectroscopy will enable previously impossible studies of the dynamics and energetics of the solar corona. The characteristics of these x-ray microcalorimeters are significantly different from conventional micro calorimeters developed for astrophysics because they need to accommodate much higher count rates (300-1000 cps) while maintaining high energy resolution of less than 4 eV FWHM in the X-ray energy band of 0.2-10 keV. The other main difference is a smaller pixel size (less than 75 x 75 square microns) than is typical for x-ray micro calorimeters in order to provide angular resolution less than 1 arcsecond. We have achieved at energy resolution of 2.15 eV at 6 keV in a pixel with a 12 x 12 square micron TES sensor and 34 x 34 x 9.1 micron gold absorber, and a resolution of 2.30 eV at 6 keV in a pixel with a 35 x 35 micron TES and a 57 x 57 x 9.1 micron gold absorber. This performance has been achieved in pixels that are fabricated directly onto solid substrates, ie. they are not supported by silicon nitride membranes. We present the results from these detectors, the expected performance at high count-rates, and prospects for the use of this technology for future Solar missions.
Publication Date: Jun 28, 2010
Document ID:
20110022573
(Acquired Nov 18, 2011)
Subject Category: SOLAR PHYSICS
Report/Patent Number: GSFC.JA.5080.2011
Document Type: Journal Article
Publication Information: Proceedings of SPIE; Volume 7732, 773238
Contract/Grant/Task Num: NNX08AE42G
Financial Sponsor: NASA; Washington, DC, United States
NASA Goddard Space Flight Center; Greenbelt, MD, United States
Organization Source: NASA Goddard Space Flight Center; Greenbelt, MD, United States
Description: 11p; In English; Original contains black and white illustrations
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: Copyright
NASA Terms: HIGH RESOLUTION; SPECTRAL RESOLUTION; CALORIMETERS; ANGULAR RESOLUTION; IMAGING TECHNIQUES; X RAY SPECTROSCOPY; SOLAR PHYSICS; ENERGY BANDS; SOLAR CORONA; PIXELS; SUBSTRATES
Availability Source: Other Sources
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