In-focal-plane SQUID multiplexer

Irwin, K. D.; Audley, M. D.; Beall, James A.; Beyer, J.; Deiker, Steve; Doriese, W. B.; Duncan, William; Hilton, G. C.; Holland, W. S.; Reintsema, C. D.; Ullom, Joel N.; Vale, Leila R.; Xu, Yu

doi:10.1016/j.nima.2003.11.310

Cited by 44 publications

(24 citation statements)

References 6 publications

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“…The TESs will be read out using superconducting quantum interference device (SQUID) current amplifiers with time-domain multiplexing (Chervenak et al 1999;de Korte et al 2003;Reintsema et al 2003;Irwin et al 2004). Ambient-temperature multichannel electronics (Battistelli et al 2008), initially developed for SCUBA2 ( Holland et al 2006), will work in concert with the time-domain multiplexers.…”

Section: The Instrumentmentioning

confidence: 99%

SpiderOptimization: Probing the Systematics of a Large‐ScaleB‐Mode Experiment

MacTavish

Ade

Battistelli

et al. 2008

Astrophysical Journal

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Spider is a long-duration, balloon-borne polarimeter designed to measure large-scale cosmic microwave background (CMB) polarization with very high sensitivity and control of systematics. The instrument will map over half the sky with degree angular resolution in the I, Q, and U Stokes parameters in four frequency bands from 96 to 275 GHz. Spider's ultimate goal is to detect the primordial gravity-wave signal imprinted on the CMB B-mode polarization. One of the challenges in achieving this goal is the minimization of the contamination of B-modes by systematic effects. This paper explores a number of instrument systematics and observing strategies in order to optimize B-mode sensitivity. This is done by injecting realistic-amplitude, time-varying systematics into a set of simulated time streams. Tests of the impact of detector noise characteristics, pointing jitter, payload pendulations, polarization angle offsets, beam systematics, and receiver gain drifts are shown. Spider's default observing strategy is to spin continuously in azimuth, with polarization modulation achieved by either a rapidly spinning half-wave plate or a rapidly spinning gondola and a slowly stepped half-wave plate. Although the latter is more susceptible to systematics, the results shown here indicate that either mode of operation can be used by Spider.

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Section: The Instrumentmentioning

confidence: 99%

SpiderOptimization: Probing the Systematics of a Large‐ScaleB‐Mode Experiment

MacTavish

Ade

Battistelli

et al. 2008

Astrophysical Journal

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“…[5][6][7] In a time-division multiplexer, amplifiers are turned on one at a time, with switching occurring fast enough that each detector is sampled faster than the detector time constants of interest. The signals from all first-stage amplifiers (only one of which is on at a time) are summed.…”

Section: Readout Electronicsmentioning

confidence: 99%

Science with Micro-X: the TES microcalorimeter x-ray imaging rocket

et al. 2006

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Micro-X is a proposed sounding rocket experiment that will combine a transition-edge-sensor X-ray-microcalorimeter array with a conical imaging mirror to obtain high-spectral-resolution images of extended and point X-ray sources. We describe the payload and the science targeted by this mission including the discussion of three possible Micro-X targets: the Puppis A supernova remnant, the Virgo Cluster, and Circinus X-1. For example, a Micro-X observation of the bright eastern knot of Puppis A will obtain a line-dominated spectrum with 90,000 counts collected in 300 seconds at 2 eV resolution across the 0.3-2.5 keV band. Micro-X will utilize plama diagnostics to determine the thermodynamic and ionization state of the plasma, to search for line shifts and broadening associated with dynamical processes, and seek evidence of ejecta enhancement. For clusters of galaxies, Micro-X can uniquely study turbulence and the temperature distribution function. For binaries, Micro-X's high resolution spectra will separate the different processes contributing to the Fe K lines at 6 keV and give a clear view of the geometry of the gas flows and circumstellar gas.

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“…Multi-chip modules (MCM), as suggested by NIST [3], provide an opportunity to test individual bolometers and the multiplexer chip, and thereby increase the yield of assembled cameras. However, the setup is more complex and additional interferences can degrade the system performance.…”

Section: Introductionmentioning

confidence: 99%

On-Chip Integrated SQUID Readout for Superconducting Bolometers

May

Zakosarenko

Kreysa

et al. 2005

IEEE Trans. Appl. Supercond.

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We present the first steps toward a 288 pixel sub-millimeter wavelength bolometer camera. We have used bolometers of the transition edge type, choosing a thermometer made of a proximity bilayer of Mo and the alloy Au/Pd with a designed transition temperature of about 500 mK. We have adapted our well-developed niobium based technology for SQUID manufacturing in order to be able to fabricate the current sensor and the bolometer on a common substrate. The function of both devices was successfully tested at the operating temperature of 300 mK.

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In-focal-plane SQUID multiplexer

Cited by 44 publications

References 6 publications

SpiderOptimization: Probing the Systematics of a Large‐ScaleB‐Mode Experiment

SpiderOptimization: Probing the Systematics of a Large‐ScaleB‐Mode Experiment

Science with Micro-X: the TES microcalorimeter x-ray imaging rocket

On-Chip Integrated SQUID Readout for Superconducting Bolometers

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