The HAWC and SAFIRE adiabatic demagnetization refrigerators

Tuttle, James; Shirron, Peter; DiPirro, Michael; Jackson, M.; Behr, Jason; Kamiya, Kōji; Warner, Brent A.; Kunes, Evan S.; Hait, T.

doi:10.1016/s0011-2275(01)00169-2

Cited by 11 publications

(7 citation statements)

References 1 publication

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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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“…This capability is being retained for SXS. Various helium containment shells have been used in flight and laboratory ADRs, including machined Ti15333 [6], Vespel with an outer Ti15333 foil [4], and gamma-alumina with an inner Ti15333 foil [7]. Below 1 K, the gamma-alumina composite appears to have the best thermal performance, but we are also investigating T300 carbon composite instead of gamma-alumina.…”

Section: Recycling Sequencementioning

confidence: 99%

“…For suspension systems, we use the kinematic design developed for HAWC [7], with modifications to allow easier assembly and integration. They use Kevlar ropes under spring tension to maintain a relatively constant pre-load during cooldown and launch loads.…”

Section: Recycling Sequencementioning

confidence: 99%

Optimization of a Two-Stage Adr for the Soft X-Ray Spectrometer (Sxs) Instrument on the Astro-H Mission

Shirron¹,

Kimball²,

Wegel³

et al. 2010

AIP Conference Proceedings

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NASA/Goddard Space Flight Center has begun developing the Soft X-ray Spectrometer (SXS) instrument that will be flown on the Japanese Astro-H mission. The SXS's 36-pixel detector array will be cooled to 50 mK using a two-stage adiabatic demagnetization refrigerator (ADR). A complicating factor for its design is that the ADR will be integrated into a superfluid helium dewar at 1.3 K that will be coupled to a 1.8 K Joule-Thomson (JT) stage through a heat switch. When liquid helium is present, the coupling will be weak, and the JT stage will act primarily as a shield to reduce parasitic heat loads. When the liquid is depleted, the heat switch will couple more strongly so that the ADR can continue to operate using the JT stage as its heat sink. A two-stage ADR is the most mass efficient option and it has the operational flexibility to work well with a stored cryogen and a cryocooler. The stages are operated independently, and this opens up a very large parameter space for optimizing the design. This paper discusses the optimization process and most relevant trades considered in the design of the SXS ADR, and its expected performance.

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“…A prototype instrument for the demonstration of these detectors is described elsewhere 3,4 . The detectors are cooled by an adiabatic demagnetization refrigerator built for SAFIRE, and similar to that used in the HAWC instrument on SOFIA 5,6 . In order to modularize these two components for testing, an insertable cryostat has been fabricated at the Goddard Space Flight Center.…”

Section: Wavelength Coverage Spectral Resolution and Field Of Viewmentioning

confidence: 99%

Far-infrared imaging spectroscopy with SAFIRE on SOFIA

et al. 2003

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The Submillimeter and Far-InfraRed Experiment (SAFIRE) on the SOFIA airborne observatory is an imaging FabryPerot spectrometer operating at wavelengths between 100µm and 700µm. SAFIRE's key science goal is to investigate line emission in galaxies at wavelengths not visible from the ground, and to map the variation in this line emission in nearby galaxies. SOFIA will fly at an altitude where the atmosphere is mostly transparent, permitting SAFIRE to achieve a high point source sensitivity at most wavelengths. With a field of view of 160''x320'' at a spectral resolution of ~200km/s, when SAFIRE achieved first light in 2006, it will add substantial capability to the first light instrument complement of SOFIA. SAFIRE's top priority observations will be to measure emission lines in the Galactic center, to map emission lines in nearby galaxies, and to understand the physics of the cores of ultraluminous galaxies from the local region to the high redshift universe through far-infrared fine-structure line emission.

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The HAWC and SAFIRE adiabatic demagnetization refrigerators

Abstract: HAWC and SAFIRE are far-infrared experiments which will fly on the SOFIA aircraft.HAWC's detectors will operate at 0.2 Kelvin, while those of SAFIRE will be at 0.

Cited by 11 publications

References 1 publication

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

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

Optimization of a Two-Stage Adr for the Soft X-Ray Spectrometer (Sxs) Instrument on the Astro-H Mission

Far-infrared imaging spectroscopy with SAFIRE on SOFIA

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