Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aps..apr..n401i&link_type=abstract
American Physical Society, APS/AAPT Joint Meeting, April 18-21, 1997, abstract #N4.01
Astronomy and Astrophysics
Astronomy
Scientific paper
High resolution x-ray spectroscopy is a vital tool for the study of astronomical x-ray sources. Conventional detectors for x-ray astronomy have high energy resolution (e.g. gratings) or excellent imaging capability (e.g. CCD's) but combining these attributes has proven difficult. The introduction of the x-ray microcalorimeter has provided a combination of high energy resolution, high quantum efficiency, and imaging capability. The x-ray microcalorimeter consists of an absorber to convert incident x-ray photons into heat and a thermometer to sense the resulting temperature change. The first x-ray microcalorimeters, now being used in astronomical measurements, are based on silicon thermistors with a FET readout and ultra-low heat capacity absorbers. These devices have demonstrated energy resolutions as good as 7 eV FWHM at 6 keV, along with high quantum efficiency and imaging capability when fabricated in an array. Recently, x-ray microcalorimeters using superconducting transition-edge thermometers read out with SQUIDs (Superconducting QUantum Interference Devices) have been demonstrated. These detectors have energy resolution comparable to the silicon thermistor devices, but use absorbers with an order of magnitude larger heat capacity and much faster thermal response times. Because of their generous heat capacity budget, transition-edge microcalorimeters show promise of achieving higher energy resolution and higher count rates. Their compatibility with photolithographic processing and sensitive, ultra-low power superconducting electronics should make it possible to fabricate large format imaging arrays.
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