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Proceedings Paper

Transition-edge sensor pixel parameter design of the microcalorimeter array for the x-ray integral field unit on Athena
Author(s): S. J. Smith; J. S. Adams; S. R. Bandler; G. L. Betancourt-Martinez; J. A. Chervenak; M. P. Chiao; M. E. Eckart; F. M. Finkbeiner; R. L. Kelley; C. A. Kilbourne; A. R. Miniussi; F. S. Porter; J. E. Sadleir; K. Sakai; N. A. Wakeham; E. J. Wassell; W. Yoon; D. A. Bennett; W. B. Doriese; J. W. Fowler; G. C. Hilton; K. M. Morgan; C. G. Pappas; C. N. Reintsema; D. S. Swetz; J. N. Ullom; K. D. Irwin; H. Akamatsu; L. Gottardi; R. den Hartog; B. D. Jackson; J. van der Kuur; D. Barret; P. Peille
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Paper Abstract

The focal plane of the X-ray integral field unit (X-IFU) for ESA’s Athena X-ray observatory will consist of ~ 4000 transition edge sensor (TES) x-ray microcalorimeters optimized for the energy range of 0.2 to 12 keV. The instrument will provide unprecedented spectral resolution of ~ 2.5 eV at energies of up to 7 keV and will accommodate photon fluxes of 1 mCrab (90 cps) for point source observations. The baseline configuration is a uniform large pixel array (LPA) of 4.28” pixels that is read out using frequency domain multiplexing (FDM). However, an alternative configuration under study incorporates an 18 × 18 small pixel array (SPA) of 2” pixels in the central ~ 36” region. This hybrid array configuration could be designed to accommodate higher fluxes of up to 10 mCrab (900 cps) or alternately for improved spectral performance (< 1.5 eV) at low count-rates. In this paper we report on the TES pixel designs that are being optimized to meet these proposed LPA and SPA configurations. In particular we describe details of how important TES parameters are chosen to meet the specific mission criteria such as energy resolution, count-rate and quantum efficiency, and highlight performance trade-offs between designs. The basis of the pixel parameter selection is discussed in the context of existing TES arrays that are being developed for solar and x-ray astronomy applications. We describe the latest results on DC biased diagnostic arrays as well as large format kilo-pixel arrays and discuss the technical challenges associated with integrating different array types on to a single detector die.

Paper Details

Date Published: 20 July 2016
PDF: 19 pages
Proc. SPIE 9905, Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray, 99052H (20 July 2016); doi: 10.1117/12.2231749
Show Author Affiliations
S. J. Smith, NASA Goddard Space Flight Ctr. (United States)
Ctr. for Research and Exploration in Space Science and Technology (United States)
Univ. of Maryland, Baltimore County (United States)
J. S. Adams, NASA Goddard Space Flight Ctr. (United States)
Ctr. for Research and Exploration in Space Science and Technology (United States)
Univ. of Maryland, Baltimore County (United States)
S. R. Bandler, NASA Goddard Space Flight Ctr. (United States)
G. L. Betancourt-Martinez, NASA Goddard Space Flight Ctr. (United States)
Univ. of Maryland, College Park (United States)
J. A. Chervenak, NASA Goddard Space Flight Ctr. (United States)
M. P. Chiao, NASA Goddard Space Flight Ctr. (United States)
Ctr. for Research and Exploration in Space Science and Technology (United States)
Univ. of Maryland, Baltimore County (United States)
M. E. Eckart, NASA Goddard Space Flight Ctr. (United States)
F. M. Finkbeiner, Wyle Information Systems, Inc. (United States)
R. L. Kelley, NASA Goddard Space Flight Ctr. (United States)
C. A. Kilbourne, NASA Goddard Space Flight Ctr. (United States)
A. R. Miniussi, Universities Space Research Association (United States)
F. S. Porter, NASA Goddard Space Flight Ctr. (United States)
J. E. Sadleir, NASA Goddard Space Flight Ctr. (United States)
K. Sakai, Ctr. for Research and Exploration in Space Science and Technology (United States)
Universities Space Research Association (United States)
N. A. Wakeham, Universities Space Research Association (United States)
E. J. Wassell, Stinger-Ghaffarian Technologies (United States)
W. Yoon, Universities Space Research Association (United States)
D. A. Bennett, National Institute of Standards and Technology (United States)
W. B. Doriese, National Institute of Standards and Technology (United States)
J. W. Fowler, National Institute of Standards and Technology (United States)
G. C. Hilton, National Institute of Standards and Technology (United States)
K. M. Morgan, National Institute of Standards and Technology (United States)
C. G. Pappas, National Institute of Standards and Technology (United States)
C. N. Reintsema, National Institute of Standards and Technology (United States)
D. S. Swetz, National Institute of Standards and Technology (United States)
J. N. Ullom, National Institute of Standards and Technology (United States)
K. D. Irwin, Stanford Univ. (United States)
H. Akamatsu, SRON Netherlands Institute for Space Research (Netherlands)
L. Gottardi, SRON Netherlands Institute for Space Research (Netherlands)
R. den Hartog, SRON Netherlands Institute for Space Research (Netherlands)
B. D. Jackson, SRON Netherlands Institute for Space Research (Netherlands)
J. van der Kuur, SRON Netherlands Institute for Space Research (Netherlands)
D. Barret, Institut de Recherche en Astrophysique et Planétologie (France)
P. Peille, Institut de Recherche en Astrophysique et Planétologie (France)


Published in SPIE Proceedings Vol. 9905:
Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray
Jan-Willem A. den Herder; Tadayuki Takahashi; Marshall Bautz, Editor(s)

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