A microwave SQUID multiplexer optimized for bolometric applications

Dober, Bradley; Ahmed, Zeeshan; Arnold, K.; Becker, Daniel; Bennett, Douglas A.; Connors, J.; Cukierman, A.; D'Ewart, John; Duff, Shannon M.; Dusatko, John; Frisch, J.; Gard, Johnathon D.; Henderson, S.; Herbst, R.; Hilton, G. C.; Hubmayr, Johannes; Li, Yi; Mates, J. A. B.; McCarrick, Heather; Reintsema, C. D.; Silva-Feaver, Max; Ruckman, L.; Ullom, Joel N.; Vale, Leila R.; Winkle, Daniel D. Van; Vásquez, Jesus; Wang, Yiwen; Young, E.; Yu, Cyndia; Zheng, Kaiwen

doi:10.1063/5.0033416

Cited by 53 publications

(30 citation statements)

References 23 publications

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“…The off-diagonal leakage coefficients k ij for detectors within a SQUID are drawn once for each simulation (so that the crosstalk leakage matrix remains constant during the full observation time) from a normal distribution with a −0.03% mean and a 0.01% width [10]. These values are consistent with the current capabilities of the readout technologies considered for SO and CMB-S4 instruments [56,59]. The modulation frequency range is set between f min = 4 GHz and f max = 8 GHz for µMUX and f min = 1 MHz and f max = 5 MHz for the fMUX setup, which are typical values for these technologies.…”

Section: G Crosstalkmentioning

confidence: 91%

“…We give baseline results for a readout electronic setup similar to the one employed in µMUX technologies, where all 1,568 bolometers in a wafer are multiplexed together in a single SQUID (superconducting quantum interference device; used to read out the signal from the transition-edge sensors). Future experiments such as SO are expected to adopt a µMUX technology and therefore have a readout scheme close to the one we simulate [56]. We also consider an alternative setup with 7 frequencydomain multiplexers (fMUX) with 4 SQUIDs per fMUX, and 28 detector pairs per SQUID.…”

Section: G Crosstalkmentioning

confidence: 99%

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Instrumental systematics biases in CMB lensing reconstruction: A simulation-based assessment

et al. 2021

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Weak gravitational lensing of the cosmic microwave background (CMB) is an important cosmological tool that allows us to learn about the structure, composition and evolution of the Universe. Upcoming CMB experiments, such as the Simons Observatory (SO), will provide high-resolution and low-noise CMB measurements. We consider the impact of instrumental systematics on the corresponding high-precision lensing reconstruction power spectrum measurements. We simulate CMB temperature and polarization maps for an SO-like instrument and potential scanning strategy, and explore systematics relating to beam asymmetries and offsets, boresight pointing, polarization angle, gain drifts, gain calibration and electric crosstalk. Our analysis shows that the majority of the biases induced by the systematics we modeled are below a detection level of ∼ 0.6σ. We discuss potential mitigation techniques to further reduce the impact of the more significant systematics, and pave the way for future lensing-related systematics analyses.

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Section: G Crosstalkmentioning

confidence: 91%

Section: G Crosstalkmentioning

confidence: 99%

Instrumental systematics biases in CMB lensing reconstruction: A simulation-based assessment

et al. 2021

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“…Due to space limitations, one of the most significant challenges of the OT design was the routing of the readout cabling from the three UFMs at 100 mK to the 4 K components on the back of the OT magnetic shielding (Figure 10). The SO uses microwave multiplexing technology to read the detectors out (Dober et al 2021). For the target multiplexing factor of 1000, each OT needs 12 radio frequency (RF) coaxial cables to read out ∼5000 detectors and 3 direct current (DC) ribbon cables for detector/amplifier biases and flux ramps (Mates et al 2012).…”

Section: Detector Arrays and Readoutmentioning

confidence: 99%

The Simons Observatory Large Aperture Telescope Receiver

Zhu

Bhandarkar

Coppi

et al. 2021

ApJS

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The Simons Observatory is a ground-based cosmic microwave background experiment that consists of three 0.4 m small-aperture telescopes and one 6 m Large Aperture Telescope, located at an elevation of 5300 m on Cerro Toco in Chile. The Simons Observatory Large Aperture Telescope Receiver (LATR) is the cryogenic camera that will be coupled to the Large Aperture Telescope. The resulting instrument will produce arcminute-resolution millimeter-wave maps of half the sky with unprecedented precision. The LATR is the largest cryogenic millimeter-wave camera built to date, with a diameter of 2.4 m and a length of 2.6 m. The coldest stage of the camera is cooled to 100 mK, the operating temperature of the bolometric detectors with bands centered around 27, 39, 93, 145, 225, and 280 GHz. Ultimately, the LATR will accommodate 13 40 cm diameter optics tubes, each with three detector wafers and a total of 62,000 detectors. The LATR design must simultaneously maintain the optical alignment of the system, control stray light, provide cryogenic isolation, limit thermal gradients, and minimize the time to cool the system from room temperature to 100 mK. The interplay between these competing factors poses unique challenges. We discuss the trade studies involved with the design, the final optimization, the construction, and ultimate performance of the system.

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“…Measurements of single infrared photons in wavelengths from a few to a few tens µm or a small flux of athermal phonons (which are long-lived acoustic phonons) are required for using hydrogenrich targets to detect light DM. Transition-Edge Sensor (TES) detectors, which can be read out in large number of pixels with multiplexing technologies [115][116][117], are a developed technology to realize such ultra-sensitive measurements. TES detectors have been utilized to detect single photons for communication [118][119][120] and for axion-like particle detection [121].…”

Section: Low-tc Tes Detectorsmentioning

confidence: 99%

Light Dark Matter Detection with Hydrogen-rich Crystals and Low-Tc TES Detectors

Wang,

Chang,

Lisovenko

et al. 2022

Preprint

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Direct detection of nuclear scatterings of sub-GeV Dark Matter (DM) particles favors low-Z nuclei. Hydrogen nucleus, which has a single proton, provides the best kinematic match to a light dark matter particle. The characteristic nuclear recoil energy is boosted by a factor of a few tens from those for larger nuclei used in traditional Weakly Interacting Massive Particle (WIMP) searches. Furthermore, hydrogen is optimal not only for spin-independent nuclear scattering of a sub-GeV DM, but also for spin-dependent nuclear scatterings, where large parameter space remains unconstrained yet. In this paper, we first introduce hydrogen-rich crystals, which emit two classes of signals under kinetic excitations. One class of the signals is infrared photons, which are from optically active fundamental vibrational modes of molecules and at several characteristic wavelengths. Another is acoustic phonons, and optical phonons that decay into acoustic phonons. We then discuss the technical status and future researches of low-Tc Transition-Edge Sensor (TES) detectors, which measure single infrared photons and a small flux of acoustic phonons with desirable sensitivities. With theoretical modeling to select hydrogen-rich crystals for the optimized science reach, ultra-sensitive low-Tc TES detectors for readout, and experimental prototyping of a light DM detection scheme, a detection experiment can be built for measuring the large unexplored parameter space of light DM particles.

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A microwave SQUID multiplexer optimized for bolometric applications

Cited by 53 publications

References 23 publications

Instrumental systematics biases in CMB lensing reconstruction: A simulation-based assessment

Instrumental systematics biases in CMB lensing reconstruction: A simulation-based assessment

The Simons Observatory Large Aperture Telescope Receiver

Light Dark Matter Detection with Hydrogen-rich Crystals and Low-Tc TES Detectors

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