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Proceedings Paper

Sounding rocket mission to study the solar soft x-ray and EUV emission using transition-edge sensor technology
Author(s): Kolo D. Wamba; Arthur B. C. Walker II; Dennis S. Martinez-Galarce; Sae Woo Nam; Kent D. Irwin; Steven W. Deiker; Blas Cabrera; Lawrence Lesyna; Stephen F. Powell; Aaron J. Miller; David W. Robertson; Paul F. X. Boerner; Phillip C. Baker; Troy W. Barbee Jr.; Richard B. Hoover
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Paper Abstract

We are developing a new sounding rocket payload, the Advanced Technology Solar Spectroscopic Imager (ATSSI), that will use an 8 X 8 array of transition edge sensors (TES) to obtain true spectroheliograms in a spectral bandpass spanning approximately 50 eV to approximately 3 keV. The TES array will be flown at the focus of a Wolter I telescope, where it will image as 3 arc-min by 3 arc-min field of view with a pixel resolution of approximately 6 arc-sec. In this way, it will obtain approximately 1000 individual spectra with an expected average energy resolution of approximately 3 eV FWHM. In addition to the TES array, the ATSSI will employ six multilayer telescopes with bandpasses centered on atomic lines at 17.1 angstrom (Fe XVII), 195.1 angstrom (Fe XII), 171.1 angstrom (Fe IX), 57.9 angstrom (Mg X), 98.3 angstrom (Ne VIII), and 150.1 angstrom (O VI). Two additional telescopes with bandpasses centered at 1550 angstrom (C IV) and 1216 angstrom (H I) will also be used. The eight narrowband telescopes will provide high spatial resolution (<EQ 1 arc- sec), full-disk solar images and will be complemented by two grating slit spectroheliographs. One grating will obtain high resolution spectroheliograms between 2750 angstrom and 2850 angstrom (for Mg II h- and k-line studies), and the other will be multilayer-based and will probe the Fe IX/X - O V/VI complex around 171 Angstrom (73 eV). With this set of instruments, we expect to explore more fully the nature of the energy flow between small-scale coronal, chromospheric and transition region structures, as well as to address the issue of what mechanisms are responsible for heating the quiescent solar atmosphere.

Paper Details

Date Published: 13 December 2000
PDF: 13 pages
Proc. SPIE 4140, X-Ray and Gamma-Ray Instrumentation for Astronomy XI, (13 December 2000); doi: 10.1117/12.409134
Show Author Affiliations
Kolo D. Wamba, Stanford Univ. (United States)
Arthur B. C. Walker II, Stanford Univ. (United States)
Dennis S. Martinez-Galarce, Stanford Univ. (United States)
Sae Woo Nam, National Institute of Standards and Technology (United States)
Kent D. Irwin, National Institute of Standards and Technology (United States)
Steven W. Deiker, National Institute of Standards and Technology (United States)
Blas Cabrera, Stanford Univ. (United States)
Lawrence Lesyna, Lockheed Martin Missiles & Space (United States)
Stephen F. Powell, Stanford Univ. (United States)
Aaron J. Miller, Stanford Univ. (United States)
David W. Robertson, Stanford Univ. (United States)
Paul F. X. Boerner, Stanford Univ. (United States)
Phillip C. Baker, Baker Consulting (United States)
Troy W. Barbee Jr., Lawrence Livermore National Lab. (United States)
Richard B. Hoover, NASA Marshall Space Flight Ctr. (United States)

Published in SPIE Proceedings Vol. 4140:
X-Ray and Gamma-Ray Instrumentation for Astronomy XI
Kathryn A. Flanagan; Oswald H. W. Siegmund, Editor(s)

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