Observations of the soft X-ray background with the XQC microcalorimeter sounding rocket

Porter, F. S.; Almy, R.; Apodaca, E.; Figueroa‐Feliciano, E.; Galeazzi, M.; Kelley, R. L.; McCammon, D.; Stahle, C. K.; Szymkowiak, A. E.; Sanders, W. T.

doi:10.1016/s0168-9002(99)01352-2

Cited by 12 publications

(2 citation statements)

References 3 publications

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“…The ADR design builds on as much heritage from prior programs as possible (Astro-E 3 and Astro-E2/Suzaku 4 , the XQC rocket program 5 , and the High-resolution Airborne Wide-band Camera (HAWC) 6 and Submillimeter and Far InfraRed Experiment (SAFIRE) 7 instruments on the Stratospheric Observatory For Infrared Astronomy (SOFIA)), but makes a significant departure from these designs in its use of multiple stages to achieve higher performance, efficiency, and the ability to operate with multiple heat sink temperatures. The design also adopts the use of refrigerants different from those used in similar applications.…”

Section: Adr Designmentioning

confidence: 99%

Design of a 3-stage ADR for the soft x-ray spectrometer instrument on the ASTRO-H mission

Shirron

Kimball

Wegel

et al. 2010

Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray

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The Japanese Astro-H mission will include the Soft X-ray Spectrometer (SXS) instrument, whose 36-pixel detector array of ultra-sensitive x-ray microcalorimeters requires cooling to 50 mK. This will be accomplished using a 3-stage adiabatic demagnetization refrigerator (ADR). The design is dictated by the need to operate with full redundancy with both a superfluid helium dewar at 1.3 K or below, and with a 4.5 K Joule-Thomson (JT) cooler. The ADR is configured as a 2-stage unit that is located in a well in the helium tank, and a third stage that is mounted to the top of the helium tank. The third stage is directly connected through two heat switches to the JT cooler and the helium tank, and manages heat flow between the two. When liquid helium is present, the 2-stage ADR operates in a single-shot manner using the superfluid helium as a heat sink. The third stage may be used independently to reduce the time-average heat load on the liquid to extend its lifetime. When the liquid is depleted, the 2nd and 3rd stages operate as a continuous ADR to maintain the helium tank at as low a temperature as possible -expected to be 1.2 K -and the 1st stage cools from that temperature as a single-stage, single-shot ADR. The ADR's design and operating modes are discussed, along with test results of the prototype 3-stage ADR.

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Section: Adr Designmentioning

confidence: 99%

Design of a 3-stage ADR for the soft x-ray spectrometer instrument on the ASTRO-H mission

Shirron

Kimball

Wegel

et al. 2010

Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray

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“…Our first flight instrument is the X-ray quantum calorimeter (XQC) rocket-borne suborbital spectrometer built in collaboration with the University of Wisconsin [7,8]. The XQC is a 36-pixel microcalorimeter array with 1 mm 2 pixels operated at 60 mK using an adiabatic demagnetization refrigerator (ADR) and a 4 L liquid helium bath.…”

Section: Introduction To Microcalorimetersmentioning

confidence: 99%

The XRS microcalorimeter spectrometer at the Livermore electron beam ion trap

Porter¹,

Beck²,

Beiersdörfer³

et al. 2008

Can. J. Phys.

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NASA's X-ray spectrometer (XRS) microcalorimeter instrument has been operating at the electron beam ion trap (EBIT) facility at Lawrence Livermore National Laboratory since July of 2000. The spectrometer is currently undergoing its third major upgrade to become an easy to use and extremely high-performance instrument for a broad range of EBIT experiments. The spectrometer itself is broadband, capable of simultaneously operating from 0.1 to 12 keV and has been operated at up to 100 keV by manipulating its operating conditions. The spectral resolution closely follows the spaceflight version of the XRS, beginning at 10 eV FWHM at 6 keV in 2000, upgraded to 5.5 eV in 2003, and will hopefully be ∼3.8 eV in the fall of 2007. Here we review the operating principles of this unique instrument, the extraordinary science that has been performed at EBIT over the last six years, and prospects for future upgrades. Specifically, we discuss upgrades to cover the high-energy band (to at least 100 keV) with a high quantum efficiency detector and prospects for using a new superconducting detector to reach 0.8 eV resolution at 1 keV and 2 eV at 6 keV with high counting rates. PACS Nos.: 52.25.Os, 52.70.La, 95.85.Nv, 32.30.Rj, 07.85.Fv, 78.70.En Résumé : Le spectromètre-X à microcalorimètre (XRS) de la NASA est en opération au piège ionique à faisceau d'électrons de Livermore (EBIT) depuis juillet 2000. Le spectromètre subit actuellement sa troisième mise à jour pour devenir un instrument facile à utiliser et extrêmement performant dans un large domaine des mesures possibles à EBIT. Le spectromètre lui-même est à large bande, capable de fonctionner simultanément entre 0.1 et 12 keV et a opéré jusqu'à 100 keV en ajustant ses paramètres d'opération. La résolution spectrale suit de près la version en orbite du XRS, débutant à 10 eV FWHM à 6 keV en 2000, améliorée à 5.5 eV en 2003 et nous espérons atteindre ∼3.8 eV à l'automne 2007. Nous passons ici en revue les principes d'opération de cet instrument unique, l'extraordinaire science faite à EBIT ces 6 dernières années et les promesses d'avenir. Plus spécifiquement, nous visons des améliorations pour couvrir le domaine de haute énergie (au moins jusqu'à 100 keV) avec une haute efficacité quantique et la perspective d'introduire un détecteur supraconducteur pour atteindre une résolution de 0.8 eV à 1 keV et 2 eV à 6 keV, avec de hauts taux de comptage. [Traduit par la Rédaction]

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