The X-ray Quantum Calorimeter Sounding Rocket Experiment: Improvements for the Next Flight

McCammon, D.; Barger, Kat; Brandl, D. E.; Brekosky, Regis P.; Crowder, S. G.; Gygax, J.; Kelley, R. L.; Kilbourne, Caroline A.; Lindeman, M. A.; Porter, F. S.; Rocks, L.; Szymkowiak, Andrew E.

doi:10.1007/s10909-008-9734-5

Cited by 25 publications

(15 citation statements)

References 6 publications

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“…The experiment was conducted on the ORNL ion-atom merged-beam apparatus (see, e.g., Ref [20]), using the microcalorimeter x-ray detector from a University of Wisconsin and Goddard Space Flight Center sounding rocket experiment [21]. An all-permanent magnet electron cyclotron resonance (ECR) ion source on a high-voltage platform [20] produced highly charged m = 13 carbon ions which were momentum analyzed by a dipole magnet to produce an uncontaminated C 6+ beam.…”

Section: Methodsmentioning

confidence: 99%

X-ray emission measurements following charge exchange between C6+and He

et al. 2013

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X-ray spectra following charge-exchange collisions between C 6+ and He are presented for collision energies between 460 and 32 000 eV/u. Spectra were obtained at the Oak Ridge National Laboratory Multicharged Ion Research Facility using a microcalorimeter x-ray detector capable of fully resolving the C VI Lyman series lines through Ly-γ . These line ratios are sensitive to the initial electron distribution and test our understanding of the charge-exchange process. In addition, these line ratios are important for identifying charge exchange in astrophysical contexts involving the interaction of solar wind ions with neutrals. Our measurements are performed at collision velocities (300-2500 km/s) which overlap most of the solar wind range. Additional data of this type can be combined with computations to provide an extensive set of reliable line ratios and absolute cross sections for the interpretation of a variety of astrophysical situations.

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Section: Methodsmentioning

confidence: 99%

X-ray emission measurements following charge exchange between C6+and He

et al. 2013

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“…Previous space experiments with doped-silicon X-ray micro-calorimeters, have used TF based on al coated polyimide [6][7][8][9][10]. The ATHENA X-IFU has similar requirements on IR attenuation, however, the use of TES technology and SQUID based electronics put an additional requirement on shielding RF EMI from the spacecraft operation and telemetry.…”

Section: Filter Design and Performance Modelingmentioning

confidence: 99%

Thermal Filters for the ATHENA X-IFU: Ongoing Activities Toward the Conceptual Design

et al. 2016

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ATHENA is the L2 mission selected by ESA to pursue the science theme "Hot and Energetic Universe". One of the two focal plane instruments is the X-ray Integral Field Unit, an array of TES microcalorimeters operated at T < 100 mK. To allow the X-ray photons focused by the telescope to reach the detector, windows have to be opened on the cryostat thermal shields. X-ray transparent filters need to be mounted on these open windows to attenuate the IR radiation from warm surfaces, to attenuate RF electromagnetic interferences on TES sensors and SQUID electronics, and to protect the detector from contamination. This paper reviews the ongoing activities driving the design of the X-IFU thermal filters.

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“…As seen in Fig. 1, a microcalorimeter X-ray detector from a University of Wisconsin and Goddard Space Flight Center sounding rocket experiment, which was thoroughly described by McCammon et al [24], is placed 23 cm above the beam line and, through a 2 cm opening, views a section of the beam line where CX take place with a Kr gas target at a constant pressure (3 Â 10 À4 Torr).…”

Section: Apparatusmentioning

confidence: 99%

“…The X-ray detector is a 1 Â 1.2 cm 2 microcalorimeter detector array and contains 36 pixels (see [24] for more details). Its resolution is better than 10 eV FWHM at 400 eV.…”

Section: Apparatusmentioning

confidence: 99%

Radiance line ratios Ly-β/Ly-α, Ly-γ/Ly-α, Ly-δ/Ly-α, and Ly-ε/Ly-α for soft X-ray emissions following charge exchange between C6+ and Kr

Andrianarijaona

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McCammon

et al. 2015

Nuclear Instruments and Methods in Physics Research Section B:

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The radiance line ratios Ly-b/Ly-a, Ly-c/Ly-a, Ly-d/Ly-a, and Ly-e/Ly-a for soft X-ray emission following charge exchange (CX) between C 6+ and Kr are reported for collision energies between approximately 320 and 46,000 eV/u. The corresponding collision velocities (250-3000 km/s) are characteristic of the solar wind. X-ray spectra were obtained at the Oak Ridge National Laboratory Multicharged Ion Research Facility using a microcalorimeter X-ray detector with a resolution on the order of 10 eV FWHM. The measured Ly-e/Ly-a is zero for all considered energies and suggests that very little, if any, capture to 6p occurs. The measured Ly-b/Ly-a and Ly-c/Ly-a ratios intersect and form a well resolved node around (950 ± 50) km/s, which could be used as an astrophysical velocity indicative tool. The results reported here are compared to calculations for C 6+ + H since no published theory for C 6+ + Kr is known to exist. Double-electron-capture (DEC) and other multi-electron processes are possible. True double capture is estimated to be only 10% of the single-electron-capture (SEC).

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The X-ray Quantum Calorimeter Sounding Rocket Experiment: Improvements for the Next Flight

Cited by 25 publications

References 6 publications

X-ray emission measurements following charge exchange between C6+and He

X-ray emission measurements following charge exchange between C6+and He

Thermal Filters for the ATHENA X-IFU: Ongoing Activities Toward the Conceptual Design

Radiance line ratios Ly-β/Ly-α, Ly-γ/Ly-α, Ly-δ/Ly-α, and Ly-ε/Ly-α for soft X-ray emissions following charge exchange between C6+ and Kr

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