MICRO-X, THE HIGH RESOLUTION SOUNDING ROCKET X-RAY IMAGING SPECTROMETER

被引:0
作者
Wikus, P. [1 ]
Adams, J. S. [2 ]
Baker, R. [2 ]
Bandler, S. R. [2 ]
DeLaney, T. A. [1 ]
Dewey, D. [1 ]
Doriese, W. B. [3 ]
Eckart, M. E. [2 ]
Figueroa-Feliciano, E. [1 ]
Galeazzi, M. [4 ]
Goeke, R. [1 ]
Hamersma, R. [6 ]
Hilton, G. [3 ]
Hwang, U. [2 ]
Irwin, K. D. [3 ]
Kelley, R. L. [2 ]
Kilbourne, C. A. [2 ]
Leman, S. W. [1 ]
McCammon, D. [5 ]
Okajima, T. [2 ]
Porter, F. S. [2 ]
Reintsema, C. D. [3 ]
Rutherford, J. M. [1 ]
Saab, T. [6 ]
Serlemitsos, P. [2 ]
Soong, Y. [2 ]
Trowbridge, S. N. [1 ]
机构
[1] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA
[2] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
[3] Natl Inst Stand & Technol, Gaithersburg, MD USA
[4] Univ Miami, Coral Gables, FL 33146 USA
[5] Univ Wisconsin, Madison, WI 53706 USA
[6] Univ Florida, Gainesville, FL 32610 USA
来源
PROCEEDINGS OF THE 19TH ESA SYMPOSIUM ON EUROPEAN ROCKET AND BALLOON PROGRAMMES AND RELATED RESEARCH | 2009年 / 671卷
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中图分类号
V [航空、航天];
学科分类号
08 ; 0825 ;
摘要
The NASA-funded Micro-X instrument is a rocket - borne X-ray imaging spectrometer operating in the energy range from 0.3 to 2.5 keV. A Transition-Edge-Sensor (TES) microcalorimeter array, cooled to a temperature of 50 mK, is used to obtain images and spectra of astrophysical objects with an energy resolution of 2-4 eV at 3 keV, which constitutes an improvement of more than an order of magnitude over currently operating non-dispersive spectrometers on X-ray space telescopes. A thin-foil conical Wolter mirror with an effective collecting area of 200 cm(2) at 1 keV and a focal length of 2165 mm focuses the X-rays from the observation target onto the detector array. The instrument has a field of view (FOV) of 11.8 arc min. We describe the design of the Micro-X instrument and its planned flights, and report the current status of hardware development and testing.
引用
收藏
页码:573 / 577
页数:5
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