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UID:UW-Physics-Event-2156
DTSTART:20110418T183000Z
DURATION:PT1H0M0S
DTSTAMP:20260418T235608Z
LAST-MODIFIED:20110409T160330Z
LOCATION:5310
SUMMARY:Microcalorimeter Arrays for High-Resolution X-ray Spectroscopy
 \, NPAC (Nuclear/Particle/Astro/Cosmo) Forum\, Catherine Bailey\, NASA
  Goddard Space Flight Center
DESCRIPTION:High-resolution x-ray spectroscopy is a powerful tool for 
 studying the evolving universe.  Current x-ray missions have high-reso
 lution grating spectrometers\; however\, non-dispersive spectrometers 
 with improved spectral resolution around 6 keV will enable imaging spe
 ctroscopy of extended sources\, such as supernova remnants and galaxy 
 clusters.  Arrays of microcalorimeters with superconducting transition
 -edge sensors (TESs) are capable of filling this need.<br>
\n<br>
\nTE
 S microcalorimeters measure the temperature change that occurs when in
 dividual photons are absorbed.  In laboratory demonstrations\, our TES
  devices achieve energy resolutions of ~2 eV at 6 keV.  The X-ray Micr
 ocalorimeter Spectrometer (XMS) is a proposed instrument that will uti
 lize these TES devices in a kilopixel-scale array that would go onboar
 d the International X-ray Observatory (IXO).  This instrument will be 
 able to provide superior high-throughput\, non-dispersive spectroscopy
  with high resolution and imaging capabilities in the 0.1 - 10 keV ene
 rgy range.<br>
\n<br>
\nIn this talk I will introduce science drivers 
 for the XMS instrument.  I will then describe the XMS detector technol
 ogy and the transition from individual pixels to large-scale arrays.  
 I will conclude by showing state-of-the-art results as well as prelimi
 nary laboratory tests of a concept for the XMS anti-coincidence detect
 or\, which will be used to reject background events generated by cosmi
 c rays.
URL:https://www.physics.wisc.edu/events/?id=2156
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