Statistics – Applications
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...207.1205i&link_type=abstract
American Astronomical Society Meeting 207, #12.05; Bulletin of the American Astronomical Society, Vol. 37, p.1171
Statistics
Applications
Scientific paper
NIST is working with NASA/Goddard Space Flight Center (GSFC) to develop multiplexed x-ray microcalorimeter arrays optimized for the Constellation-X mission. These arrays are based on superconducting transition-edge sensors (TES) read out with multiplexed superconducting quantum interference device (SQUID) amplifiers. We present recent progress in improving the x-ray energy resolution through engineering the device geometry, and present recent results with 8- and 16-channel multiplexers.
In order to achieve the ambitious x-ray energy resolution goals for the Constellation-X microcalorimeters, we have conducted extensive investigations of the high-frequency unexplained noise in TES sensors as a function of operating resistance, current density, applied magnetic field, and device geometry. Using the measured dependencies of the unexplained noise, we have optimized the design of our TES x-ray sensors and achieved FWHM energy resolutions of 2.4 eV at the 5.9 keV Mn Kα complex, which is a significant step towards the Constellation-X resolution goal of 2 eV at 5.9 keV.
We also present progress in the development of time-division SQUID multiplexers for the readout of large x-ray calorimeter arrays. We present results from x-ray microcalorimeters in 8- and 16-channel multiplexers. We describe the constraints on the system architecture, and present a practical design for a 32-channel MUX to be used in a kilopixel array.
Finally, we have extended this work to develop TES microcalorimeters for higher energy applications, such as the study of Ti emission lines from supernova remnants, including high-resolution velocity diagnostics. We have obtained a spectral resolving power of 4300 (energy / half-energy width) at the 103 keV Gd γ -ray line using a TES with a Sn absorber.
We are grateful for technical support from the NASA/GSFC microcalorimeter group, and for financial support from NASA through the Constellation-X program and Grant NDPR S06561-G.
Beall James A.
Doriese Bertrand W.
Duncan William D.
Ferreira Leticia
Hilton Gene C.
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