Large Area Transition Edge Sensor X-ray Microcalorimeters for Diffuse X-ray Background Studies

被引:0
作者
K. M. Morgan
S. E. Busch
M. E. Eckart
C. A. Kilbourne
D. McCammon
机构
[1] University of Wisconsin-Madison,Department of Physics
[2] NASA Goddard Space Flight Center,X
[3] NASA Postdoctoral Program at Goddard Space Flight Center,ray Astrophysics Lab
[4] CRESST and University of Maryland,undefined
来源
Journal of Low Temperature Physics | 2014年 / 176卷
关键词
Transition edge sensors; Microcalorimeters; X-ray astronomy;
D O I
暂无
中图分类号
学科分类号
摘要
We are developing transition edge sensor (TES) mirocalorimeters with large area (0.72 mm2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$^2$$\end{document}) absorbers to study the keV diffuse X-ray background. The goal is to develop a 2 cm2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$^2$$\end{document} array of 256 pixels for a sounding rocket payload. We present a pixel design which includes a Mo/Au bilayer TES coupled to a large (850 x 850 x 0.2 μ\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\upmu $$\end{document}m3\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$^3$$\end{document}) gold absorber. Our simulations indicate that such a design can achieve energy resolution as good as 1.6 eV FWHM in our target bandpass of 0.05–1 keV. Additionally, thermal modelling shows that for typical gold layers, the position-dependent variation of the pulse shape over the large area of the absorber is not expected to significantly degrade this energy resolution. An array of devices will be fabricated in late 2013 to test this design.
引用
收藏
页码:331 / 336
页数:5
相关论文
共 21 条
[1]  
Sanders W(1977)undefined Astrophys. J. 217 L87-undefined
[2]  
Kraushaar W(1987)undefined Annu. Rev. Astron. & Astrophys. 25 303-undefined
[3]  
Nousek J(1998)undefined Lect. Notes Phys. 506 121-undefined
[4]  
Cox D(2000)undefined Astrophys. J. 532 L153-undefined
[5]  
Reynold R(2002)undefined Astrophys J. 576 188-undefined
[6]  
Cox DP(2012)undefined Astrophys. J. 758 143-undefined
[7]  
Cravens TE(2009)undefined Astrophys. J. 696 1517-undefined
[8]  
McCammon D(2013)undefined IEEE Trans. Appl. Supercond. 23 2101705-undefined
[9]  
Crowder SG(2007)undefined Proc. SPIE 6686 668606-undefined
[10]  
Barger KA(2009)undefined AIP Conf. Proc. 1185 699-undefined