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1. A Microwave SQUID Multiplexer Optimized for Bolometric Applications

Author

Dober, B., Ahmed, Z., Arnold, K., Becker, D. T., Bennett, D. A., Connors, J. A., Cukierman, A., D'Ewart, J. M., Duff, S. M., Dusatko, J. E., Frisch, J. C., Gard, J. D., Henderson, S. W., Herbst, R., Hilton, G. C., Hubmayr, J., Li, Y., Mates, J. A. B., McCarrick, H., Reintsema, C. D, Silva-Feaver, M., Ruckman, L., Ullom, J. N., Vale, L. R., Van Winkle, D. D., Vasquez, J., Wang, Y., Young, E., Yu, C., and Zheng, K.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

A microwave SQUID multiplexer ($\mu$MUX) has been optimized for coupling to large arrays of superconducting transition-edge sensor (TES) bolometers. We present the scalable cryogenic multiplexer chip design in a 1820-channel multiplexer configuration for the 4-8 GHz rf band. The key metrics of yield, sensitivity, and crosstalk are determined through measurements of 455 readout channels, which span 4-5 GHz. The median white-noise level is 45 pA/$\sqrt{\textrm{Hz}}$, evaluated at 2 Hz, with a 1/f knee $\leq$ 20 mHz after common-mode subtraction. The white-noise level decreases the sensitivity of a TES bolometer optimized for detection of the cosmic microwave background at 150 GHz by only 3%. The measured crosstalk between any channel pair is $\leq$ 0.3%., Comment: 6 pages, 5 figures

Published
2020
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2. Magnetic Field Sensitivity of Microwave SQUID Multiplexers

Author

Connors, J. A., Ahmed, Z., Austermann, J., Denison, E. V., Dober, B., D’Ewart, J. M., Frisch, J. C., Henderson, S. W., Herbst, R., Hilton, G. C., Huber, Z. B., Hubmayr, J., Li, Y., Mates, J. A. B., Niemack, M., Vale, L. R., Van Winkle, D., Vavagiakis, E., Whipps, Z., Young, E., Yu, C., and Ullom, J.

Published
2022
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4. SLAC Microresonator Radio Frequency (SMuRF) Electronics for Read Out of Frequency-Division-Multiplexed Cryogenic Sensors

Author

Kernasovskiy, S. A., Kuenstner, S. E., Karpel, E., Ahmed, Z., Van Winkle, D. D., Smith, S., Dusatko, J., Frisch, J. C., Chaudhuri, S., Cho, H. M., Dober, B. J., Henderson, S. W., Hilton, G. C., Hubmayr, J., Irwin, K. D., Kuo, C. L., Li, D., Mates, J. A. B., Nasr, M., Tantawi, S., Ullom, J., Vale, L., and Young, B.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Large arrays of cryogenic sensors for various imaging applications ranging across x-ray, gamma-ray, Cosmic Microwave Background (CMB), mm/sub-mm, as well as particle detection increasingly rely on superconducting microresonators for high multiplexing factors. These microresonators take the form of microwave SQUIDs that couple to Transition-Edge Sensors (TES) or Microwave Kinetic Inductance Detectors (MKIDs). In principle, such arrays can be read out with vastly scalable software-defined radio using suitable FPGAs, ADCs and DACs. In this work, we share plans and show initial results for SLAC Microresonator Radio Frequency (SMuRF) electronics, a next-generation control and readout system for superconducting microresonators. SMuRF electronics are unique in their implementation of specialized algorithms for closed-loop tone tracking, which consists of fast feedback and feedforward to each resonator's excitation parameters based on transmission measurements. Closed-loop tone tracking enables improved system linearity, a significant increase in sensor count per readout line, and the possibility of overcoupled resonator designs for enhanced dynamic range. Low-bandwidth prototype electronics were used to demonstrate closed-loop tone tracking on twelve 300-kHz-wide microwave SQUID resonators, spaced at $\sim$6 MHz with center frequencies $\sim$5-6 GHz. We achieve multi-kHz tracking bandwidth and demonstrate that the noise floor of the electronics is subdominant to the noise intrinsic in the multiplexer., Comment: 7 pages, 5 figures, Submitted to the Journal of Low Temperature Physics (Proceedings of the 17th International Workshop on Low Temperature Detectors)

Published
2018
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5. Millimeter-Wave Polarimeters Using Kinetic Inductance Detectors for TolTEC and Beyond

Author

Austermann, J. E., Beall, J. A., Bryan, S. A., Dober, B., Gao, J., Hilton, G., Hubmayr, J., Mauskopf, P., McKenney, C. M., Simon, S. M., Ullom, J. N., Vissers, M. R., and Wilson, G. W.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Microwave Kinetic Inductance Detectors (MKIDs) provide a compelling path forward to the large-format polarimeter, imaging, and spectrometer arrays needed for next-generation experiments in millimeter-wave cosmology and astronomy. We describe the development of feedhorn-coupled MKID detectors for the TolTEC millimeter-wave imaging polarimeter being constructed for the 50-meter Large Millimeter Telescope (LMT). Observations with TolTEC are planned to begin in early 2019. TolTEC will comprise $\sim$7,000 polarization sensitive MKIDs and will represent the first MKID arrays fabricated and deployed on monolithic 150 mm diameter silicon wafers -- a critical step towards future large-scale experiments with over $10^5$ detectors. TolTEC will operate in observational bands at 1.1, 1.4, and 2.0 mm and will use dichroic filters to define a physically independent focal plane for each passband, thus allowing the polarimeters to use simple, direct-absorption inductive structures that are impedance matched to incident radiation. This work is part of a larger program at NIST-Boulder to develop MKID-based detector technologies for use over a wide range of photon energies spanning millimeter-waves to X-rays. We present the detailed pixel layout and describe the methods, tools, and flexible design parameters that allow this solution to be optimized for use anywhere in the millimeter and sub-millimeter bands. We also present measurements of prototype devices operating in the 1.1 mm band and compare the observed optical performance to that predicted from models and simulations., Comment: 7 pages, 4 figures, 1 table. Submitted to Journal of Low Temperature Physics

Published
2018
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6. Superconducting micro-resonator arrays with ideal frequency spacing and extremely low frequency collision rate

Author

Liu, X., Guo, W., Wang, Y., Dai, M., Wei, L. F., Dober, B., McKenney, C., Hilton, G. C., Hubmayr, J., Austermann, J. E., Ullom, J. N., Gao, J., and Vissers, M. R.

Subjects
Physics - Instrumentation and Detectors, Condensed Matter - Superconductivity
Abstract

We present a wafer trimming technique for producing superconducting micro-resonator arrays with highly uniform frequency spacing. With the light-emitting diode (LED) mapper technique demonstrated previously, we first map the measured resonance frequencies to the physical resonators. Then, we fine-tune each resonator's frequency by lithographically trimming a small length, calculated from the deviation of the measured frequency from its design value, from the interdigitated capacitor. We demonstrate this technique on a 127-resonator array made of titanium-nitride (TiN) and show that the uniformity of frequency spacing is greatly improved. The array yield in terms of frequency collisions improves from 84% to 97%, while the quality factors and noise properties are unaffected. The wafer trimming technique provides an easy-to-implement tool to improve the yield and multiplexing density of large resonator arrays, which is important for various applications in photon detection and quantum computing., Comment: 5 pages,4 figures

Published
2017

7. The Simons Observatory: Science goals and forecasts

Author

Ade, P, Aguirre, J, Ahmed, Z, Aiola, S, Ali, A, Alonso, D, Alvarez, MA, Arnold, K, Ashton, P, Austermann, J, Awan, H, Baccigalupi, C, Baildon, T, Barron, D, Battaglia, N, Battye, R, Baxter, E, Bazarko, A, Beall, JA, Bean, R, Beck, D, Beckman, S, Beringue, B, Bianchini, F, Boada, S, Boettger, D, Bond, JR, Borrill, J, Brown, ML, Bruno, SM, Bryan, S, Calabrese, E, Calafut, V, Calisse, P, Carron, J, Challinor, A, Chesmore, G, Chinone, Y, Chluba, J, Cho, HMS, Choi, S, Coppi, G, Cothard, NF, Coughlin, K, Crichton, D, Crowley, KD, Crowley, KT, Cukierman, A, D'Ewart, JM, Dünner, R, De Haan, T, Devlin, M, Dicker, S, Didier, J, Dobbs, M, Dober, B, Duell, CJ, Duff, S, Duivenvoorden, A, Dunkley, J, Dusatko, J, Errard, J, Fabbian, G, Feeney, S, Ferraro, S, Fluxà, P, Freese, K, Frisch, JC, Frolov, A, Fuller, G, Fuzia, B, Galitzki, N, Gallardo, PA, Ghersi, JTG, Gao, J, Gawiser, E, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Golec, J, Gordon, S, Gralla, M, Green, D, Grigorian, A, Groh, J, Groppi, C, Guan, Y, Gudmundsson, JE, Han, D, Hargrave, P, Hasegawa, M, Hasselfield, M, Hattori, M, Haynes, V, Hazumi, M, He, Y, Healy, E, Henderson, SW, Hervias-Caimapo, C, and Hill, CA

Subjects
CMBR experiments, CMBR polarisation, cosmological parameters from CMBR, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping 10% of the sky to a white noise level of 2 μK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r)=0.003. The large aperture telescope will map 40% of the sky at arcminute angular resolution to an expected white noise level of 6 μK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources.

Published
2019

8. Magnetic Sensitivity of AlMn TESes and Shielding Considerations for Next-Generation CMB Surveys

Author

Vavagiakis, E. M., Henderson, S. W., Zheng, K., Cho, H. -M., Cothard, N. F., Dober, B., Duff, S. M., Gallardo, P. A., Hilton, G., Hubmayr, J., Irwin, K. D., Koopman, B. J., Li, D., Nati, F., Niemack, M. D., Reintsema, C. D., Simon, S., Stevens, J. R., Suzuki, A., and Westbrook, B.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In the next decade, new ground-based Cosmic Microwave Background (CMB) experiments such as Simons Observatory (SO), CCAT-prime, and CMB-S4 will increase the number of detectors observing the CMB by an order of magnitude or more, dramatically improving our understanding of cosmology and astrophysics. These projects will deploy receivers with as many as hundreds of thousands of transition edge sensor (TES) bolometers coupled to Superconducting Quantum Interference Device (SQUID)-based readout systems. It is well known that superconducting devices such as TESes and SQUIDs are sensitive to magnetic fields. However, the effects of magnetic fields on TESes are not easily predicted due to the complex behavior of the superconducting transition, which motivates direct measurements of the magnetic sensitivity of these devices. We present comparative four-lead measurements of the critical temperature versus applied magnetic field of AlMn TESes varying in geometry, doping, and leg length, including Advanced ACT (AdvACT) and POLARBEAR-2/Simons Array bolometers. Molybdenum-copper bilayer ACTPol TESes are also tested and are found to be more sensitive to magnetic fields than the AlMn devices. We present an observation of weak-link-like behavior in AlMn TESes at low critical currents. We also compare measurements of magnetic sensitivity for time division multiplexing SQUIDs and frequency division multiplexing microwave rf-SQUIDs. We discuss the implications of our measurements on the magnetic shielding required for future experiments that aim to map the CMB to near-fundamental limits., Comment: 8 pages, 4 figures, conference proceedings submitted to the Journal of Low Temperature Physics

Published
2017
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9. Microwave SQUID Multiplexer demonstration for Cosmic Microwave Background Imagers

Author

Dober, B., Becker, D. T., Bennett, D. A., Bryan, S. A., Duff, S. M., Gard, J. D., Hays-Wehle, J. P., Hilton, G. C., Hubmayr, J., Mates, J. A. B., Reintsema, C. D., Vale, L. R., and Ullom, J. N.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Key performance characteristics are demonstrated for the microwave SQUID multiplexer ($\mu$MUX) coupled to transition edge sensor (TES) bolometers that have been optimized for cosmic microwave background (CMB) observations. In a 64-channel demonstration, we show that the $\mu$MUX produces a white, input referred current noise level of 29~pA$/\sqrt{\mathrm{Hz}}$ at -77~dB microwave probe tone power, which is well below expected fundamental detector and photon noise sources for a ground-based CMB-optimized bolometer. Operated with negligible photon loading, we measure 98~pA$/\sqrt{\mathrm{Hz}}$ in the TES-coupled channels biased at 65% of the sensor normal resistance. This noise level is consistent with that predicted from bolometer thermal fluctuation (i.e., phonon) noise. Furthermore, the power spectral density exhibits a white spectrum at low frequencies ($\sim$~100~mHz), which enables CMB mapping on large angular scales that constrain the physics of inflation. Additionally, we report cross-talk measurements that indicate a level below 0.3%, which is less than the level of cross-talk from multiplexed readout systems in deployed CMB imagers. These measurements demonstrate the $\mu$MUX as a viable readout technique for future CMB imaging instruments., Comment: 6 pages, 4 figures

Published
2017
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10. Cryogenic LED pixel-to-frequency mapper for kinetic inductance detector arrays

Author

Liu, X., Guo, W., Wang, Y., Wei, L. F., Mckenney, C. M., Dober, B., Billings, T., Hubmayr, J., Ferreira, L. S., Vissers, M. R., and Gao, J.

Subjects
Physics - Instrumentation and Detectors, Condensed Matter - Mesoscale and Nanoscale Physics, Physics - Applied Physics
Abstract

We present a cryogenic wafer mapper based on light emitting diodes (LEDs) for spatial mapping of a large microwave kinetic inductance detector (MKID) array. In this scheme, an array of LEDs, addressed by DC wires and collimated through horns onto the detectors, is mounted in front of the detector wafer. By illuminating each LED individually and sweeping the frequency response of all the resonators, we can unambiguously correspond a detector pixel to its measured resonance frequency. We have demonstrated mapping a 76.2 mm 90-pixel MKID array using a mapper containing 126 LEDs with 16 DC bias wires. With the frequency to pixel-position correspondence data obtained by the LED mapper, we have found a radially position-dependent frequency non-uniformity < 1.6% over the 76.2 mm wafer. Our LED wafer mapper has no moving parts and is easy to implement. It may find broad applications in superconducting detector and quantum computing/information experiments., Comment: accepted by J. Appl. Phys. 2017

Published
2017
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11. On the relation between the column density structures and the magnetic field orientation in the Vela C molecular complex

Author

Soler, J. D., Ade, P. A. R., Angilè, F. E., Ashton, P., Benton, S. J., Devlin, M. J., Dober, B., Fissel, L. M., Fukui, Y., Galitzki, N., Gandilo, N. N., Hennebelle, P., Klein, J., Li, Z. -Y., Korotkov, A. L., Martin, P. G., Matthews, T. G., Moncelsi, L., Netterfield, C. B., Novak, G., Pascale, E., Poidevin, F., Santos, F. P., Savini, G., Scott, D., Shariff, J. A., Thomas, N. E., Tucker, C. E., Tucker, G. S., and Ward-Thompson, D.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We statistically evaluate the relative orientation between gas column density structures, inferred from Herschel submillimetre observations, and the magnetic field projected on the plane of sky, inferred from polarized thermal emission of Galactic dust observed by BLASTPol at 250, 350, and 500 micron, towards the Vela C molecular complex. First, we find very good agreement between the polarization orientations in the three wavelength-bands, suggesting that, at the considered common angular resolution of 3.0 arcminutes that corresponds to a physical scale of approximately 0.61 pc, the inferred magnetic field orientation is not significantly affected by temperature or dust grain alignment effects. Second, we find that the relative orientation between gas column density structures and the magnetic field changes progressively with increasing gas column density, from mostly parallel or having no preferred orientation at low column densities to mostly perpendicular at the highest column densities. This observation is in agreement with previous studies by the Planck collaboration towards more nearby molecular clouds. Finally, we find a correspondence between the trends in relative orientation and the shape of the column density probability distribution functions. In the sub-regions of Vela C dominated by one clear filamentary structure, or "ridges", we find a sharp transition from preferentially parallel or having no preferred relative orientation at low column densities to preferentially perpendicular at highest column densities. In the sub-regions of Vela C dominated by several filamentary structures with multiple orientations, or "nests", such a transition is also present, but it is clearly less sharp than in the ridge-like sub-regions. Both of these results suggest that the magnetic field is dynamically important for the formation of density structures in this region., Comment: 16 pages, 17 figures. Submitted to A&A

Published
2017
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12. Optical Demonstration of THz, Dual-Polarization Sensitive Microwave Kinetic Inductance Detectors

Author

Dober, B., Austermann, J. A., Beall, J. A., Becker, D., Che, G., Cho, H. M., Devlin, M., Duff, S. M., Galitzki, N., Gao, J., Groppi, C., Hilton, G. C., Hubmayr, J., Irwin, K. D., McKenney, C. M., Li, D., Lourie, N., Mauskopf, P., Vissers, M. R., and Wang, Y.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The next generation BLAST experiment (BLAST-TNG) is a suborbital balloon payload that seeks to map polarized dust emission in the 250 $\mu$m, 350 $\mu$m and 500 $\mu$m wavebands. The instrument utilizes a stepped half-wave plate to reduce systematics. The general requirement of the detectors is that they are photon-noise-limited and dual-polarization sensitive. To achieve this goal, we are developing three monolithic arrays of cryogenic sensors, one for each waveband. Each array is feedhorn-coupled and each spatial pixel consists of two orthogonally spaced polarization-sensitive microwave kinetic inductance detectors (MKIDs) fabricated from a Ti/TiN multilayer film. In previous work, we demonstrated photon-noise-limited sensitivity in 250 $\mu$m waveband single polarization devices. In this work, we present the first results of dual-polarization sensitive MKIDs at 250 $\mu$m., Comment: 7 pages, 4 figures, published by JLTP

Published
2016
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13. The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry-BLASTPol: Performance and results from the 2012 Antarctic flight

Author

Galitzki, N., Ade, P. A. R., Angilé, F. E., Benton, S. J., Devlin, M. J., Dober, B., Fissel, L. M., Fukui, Y., Gandilo, N. N., Klein, J., Korotkov, A. L., Matthews, T. G., Moncelsi, L., Netterfield, C. B., Novak, G., Nutter, D., Pascale, E., Poidevin, F., Savini, G., Scott, D., Shariff, J. A., Soler, J. D., Tucker, C. E., Tucker, G. S., and Ward-Thompson, D.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol) is a suborbital mapping experiment, designed to study the role played by magnetic fields in the star formation process. BLASTPol observes polarized light using a total power instrument, photolithographic polarizing grids, and an achromatic half-wave plate to modulate the polarization signal. During its second flight from Antarctica in December 2012, BLASTPol made degree scale maps of linearly polarized dust emission from molecular clouds in three wavebands, centered at 250, 350, and 500 microns. The instrumental performance was an improvement over the 2010 BLASTPol flight, with decreased systematics resulting in a higher number of confirmed polarization vectors. The resultant dataset allows BLASTPol to trace magnetic fields in star-forming regions at scales ranging from cores to entire molecular cloud complexes., Comment: Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014

Published
2014
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14. Thermal design and performance of the balloon-borne large aperture submillimeter telescope for polarimetry BLASTPol

Author

Soler, J. D., Ade, P. A. R., Angilè, F. E., Benton, S. J., Devlin, M. J., Dober, B., Fissel, L. M., Fukui, Y., Galitzki, N., Gandilo, N. N., Klein, J., Korotkov, A. L., Matthews, T. G., Moncelsi, L., Mroczkowski, A., Netterfield, C. B., Novak, G., Nutter, D., Pascale, E., Poidevin, F., Savini, G., Scott, D., Shariff, J. A., Thomas, N. E., Truch, M. D., Tucker, C. E., Tucker, G. S., and Ward-Thompson, D.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present the thermal model of the Balloon-borne Large-Aperture Submillimeter Telescope for Polarimetry (BLASTPol). This instrument was successfully flown in two circumpolar flights from McMurdo, Antarctica in 2010 and 2012. During these two flights, BLASTPol obtained unprecedented information about the magnetic field in molecular clouds through the measurement of the polarized thermal emission of interstellar dust grains. The thermal design of the experiment addresses the stability and control of the payload necessary for this kind of measurement. We describe the thermal modeling of the payload including the sun-shielding strategy. We present the in-flight thermal performance of the instrument and compare the predictions of the model with the temperatures registered during the flight. We describe the difficulties of modeling the thermal behavior of the balloon-borne platform and establish landmarks that can be used in the design of future balloon-borne instruments., Comment: 18 pages, 11 figures. Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014. To be published in Proceedings of SPIE Volume 9145

Published
2014
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15. BLASTbus electronics: general-purpose readout and control for balloon-borne experiments

Author

Benton, S. J., Ade, P. A., Amiri, M., Angilè, F. E., Bock, J. J., Bond, J. R., Bryan, S. A., Chiang, H. C., Contaldi, C. R., Crill, B. P., Devlin, M. J., Dober, B., Doré, O. P., Dowell, C. D., Farhang, M., Filippini, J. P., Fissel, L. M., Fraisse, A. A., Fukui, Y., Galitzki, N., Gambrel, A. E., Gandilo, N. N., Golwala, S. R., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. D., Klein, J., Korotkov, A. L., Kuo, C. L., MacTavish, C. J., Mason, P. V., Matthews, T. G., Megerian, K. G., Moncelsi, L., Morford, T. A., Mroczkowski, T. K., Nagy, J. M., Netterfield, C. B., Novak, G., Nutter, D., O'Brient, R., Ogburn IV, R. W., Pascale, E., Poidevin, F., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Savini, G., Scott, D., Shariff, J. A., Soler, J. D., Thomas, N. E., Trangsrud, A., Truch, M. D., Tucker, C. E., Tucker, G. S., Tucker, R. S., Turner, A. D., Ward-Thompson, D., Weber, A. C., Wiebe, D. V., and Young, E. Y.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present the second generation BLASTbus electronics. The primary purposes of this system are detector readout, attitude control, and cryogenic housekeeping, for balloon-borne telescopes. Readout of neutron transmutation doped germanium (NTD-Ge) bolometers requires low noise and parallel acquisition of hundreds of analog signals. Controlling a telescope's attitude requires the capability to interface to a wide variety of sensors and motors, and to use them together in a fast, closed loop. To achieve these different goals, the BLASTbus system employs a flexible motherboard-daughterboard architecture. The programmable motherboard features a digital signal processor (DSP) and field-programmable gate array (FPGA), as well as slots for three daughterboards. The daughterboards provide the interface to the outside world, with versions for analog to digital conversion, and optoisolated digital input/output. With the versatility afforded by this design, the BLASTbus also finds uses in cryogenic, thermometry, and power systems. For accurate timing control to tie everything together, the system operates in a fully synchronous manner. BLASTbus electronics have been successfully deployed to the South Pole, and flown on stratospheric balloons., Comment: Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014. To be published in Proceedings of SPIE Volume 9145

Published
2014
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16. Attitude determination for balloon-borne experiments

Author

Gandilo, N. N., Ade, P. A. R., Amiri, M., Angile, F. E., Benton, S. J., Bock, J. J., Bond, J. R., Bryan, S. A., Chiang, H. C., Contaldi, C. R., Crill, B. P., Devlin, M. J., Dober, B., Dore, O. P., Farhang, M., Filippini, J. P., Fissel, L. M., Fraisse, A. A., Fukui, Y., Galitzki, N., Gambrel, A. E., Golwala, S., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. D., Klein, J., Korotkov, A. L., Kuo, C. L., MacTavish, C. J., Mason, P. V., Matthews, T. G., Megerian, K. G., Moncelsi, L., Morford, T. A., Mroczkowski, T. K., Nagy, J. M., Netterfield, C. B., Novak, G., Nutter, D., O'Brient, R., Pascale, E., Poidevin, F., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Savini, G., Scott, D., Shariff, J. A., Soler, J. D., Thomas, N. E., Trangsrud, A., Truch, M. D., Tucker, C. E., Tucker, G. S., Tucker, R. S., Turner, A. D., Ward-Thompson, D., Weber, A. C., Wiebe, D. V., and Young, E. Y.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

An attitude determination system for balloon-borne experiments is presented. The system provides pointing information in azimuth and elevation for instruments flying on stratospheric balloons over Antarctica. In-flight attitude is given by the real-time combination of readings from star cameras, a magnetometer, sun sensors, GPS, gyroscopes, tilt sensors and an elevation encoder. Post-flight attitude reconstruction is determined from star camera solutions, interpolated by the gyroscopes using an extended Kalman Filter. The multi-sensor system was employed by the Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol), an experiment that measures polarized thermal emission from interstellar dust clouds. A similar system was designed for the upcoming flight of SPIDER, a Cosmic Microwave Background polarization experiment. The pointing requirements for these experiments are discussed, as well as the challenges in designing attitude reconstruction systems for high altitude balloon flights. In the 2010 and 2012 BLASTPol flights from McMurdo Station, Antarctica, the system demonstrated an accuracy of <5' rms in-flight, and <5" rms post-flight., Comment: 16 pages, 10 figures, Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014. To be published in Proceedings of SPIE Volume 9145

Published
2014
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17. Microwave Multiplexing on the Keck Array

Author

Cukierman, A., Ahmed, Z., Henderson, S., Young, E., Yu, C., Barkats, D., Brown, D., Chaudhuri, S., Cornelison, J., D’Ewart, J. M., Dierickx, M., Dober, B. J., Dusatko, J., Fatigoni, S., Filippini, J. P., Frisch, J. C., Haller, G., Halpern, M., Hilton, G. C., Hubmayr, J., Irwin, K. D., Karkare, K. S., Karpel, E., Kernasovskiy, S. A., Kovac, J. M., Kovacs, A., Kuenstner, S. E., Kuo, C. L., Li, D., Mates, J. A. B., Smith, S., St. Germaine, T., Ullom, J. N., Vale, L. R., Van Winkle, D. D., Vasquez, J., Willmert, J., Zeng, L., Ade, P. A. R., Amiri, M., Basu Thakur, R., Bischoff, C. A., Bock, J. J., Boenish, H., Bullock, E., Buza, V., Cheshire, J., Connors, J., Crumrine, M., Duband, L., Hall, G., Harrison, S., Hildebrandt, S. R., Hui, H., Kang, J., Kefeli, S., Lau, K., Megerian, K. G., Moncelsi, L., Namikawa, T., Nguyen, H. T., O’Brient, R., Palladino, S., Pryke, C., Racine, B., Reintsema, C. D., Richter, S., Schillaci, A., Schwarz, R., Sheehy, C. D., Soliman, A., Steinbach, B., Sudiwala, R. V., Thompson, K. L., Tucker, C., Turner, A. D., Umiltà, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Wu, W. L. K., Yang, H., Yoon, K. W., and Zhang, C.

Published
2020
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21. The Simons Observatory: A large-diameter truss for a refracting telescope cooled to 1 K

Author

Crowley, K, Dow, P, Shroyer, J, Groh, J, Dober, B, Spisak, J, Galitzki, N, Bhandarkar, T, Devlin, M, Dicker, S, Gallardo, P, Harrington, K, Iuliano, J, Johnson, B, Johnson, D, Kofman, A, Kusaka, A, Lee, A, Limon, M, Nati, F, Orlowski-Scherer, J, Page, L, Randall, M, Teply, G, Tsan, T, Wollack, E, Xu, Z, Zhu, N, Crowley K. D., Dow P., Shroyer J. E., Groh J. C., Dober B., Spisak J., Galitzki N., Bhandarkar T., Devlin M. J., Dicker S., Gallardo P. A., Harrington K., Iuliano J., Johnson B. R., Johnson D., Kofman A. M., Kusaka A., Lee A., Limon M., Nati F., Orlowski-Scherer J., Page L., Randall M., Teply G., Tsan T., Wollack E. J., Xu Z., Zhu N., Crowley, K, Dow, P, Shroyer, J, Groh, J, Dober, B, Spisak, J, Galitzki, N, Bhandarkar, T, Devlin, M, Dicker, S, Gallardo, P, Harrington, K, Iuliano, J, Johnson, B, Johnson, D, Kofman, A, Kusaka, A, Lee, A, Limon, M, Nati, F, Orlowski-Scherer, J, Page, L, Randall, M, Teply, G, Tsan, T, Wollack, E, Xu, Z, Zhu, N, Crowley K. D., Dow P., Shroyer J. E., Groh J. C., Dober B., Spisak J., Galitzki N., Bhandarkar T., Devlin M. J., Dicker S., Gallardo P. A., Harrington K., Iuliano J., Johnson B. R., Johnson D., Kofman A. M., Kusaka A., Lee A., Limon M., Nati F., Orlowski-Scherer J., Page L., Randall M., Teply G., Tsan T., Wollack E. J., Xu Z., and Zhu N.

Abstract

We present the design and measured performance of a new carbon fiber strut design that is used in a cryogenically cooled truss for the Simons Observatory small aperture telescope. The truss consists of two aluminum 6061 rings separated by 24 struts. Each strut consists of a central carbon fiber tube fitted with two aluminum end caps. We tested the performance of the strut and truss by (i) cryogenically cycling and destructively pull-Testing strut samples, (ii) non-destructively pull-Testing the final truss, and (iii) measuring the thermal conductivity of the carbon fiber tubes. We found that the strut strength is limited by the mounting fasteners and the strut end caps, not the epoxy adhesive or the carbon fiber tube. This result is consistent with our numerical predictions. Our thermal measurements suggest that the conductive heat load through the struts (from 4 to 1 K) will be less than 1 mW. This strut design may be a promising candidate for use in other cryogenic support structures.

Published
2022

22. The Simons Observatory: Magnetic Sensitivity Measurements of Microwave SQUID Multiplexers

Author

Vavagiakis, E, Ahmed, Z, Ali, A, Arnold, K, Austermann, J, Bruno, S, Choi, S, Connors, J, Cothard, N, Dicker, S, Dober, B, Duff, S, Fanfani, V, Healy, E, Henderson, S, Ho, S, Hoang, D, Hilton, G, Hubmayr, J, Krachmalnicoff, N, Li, Y, Mates, J, Mccarrick, H, Nati, F, Niemack, M, Silva-Feaver, M, Staggs, S, Stevens, J, Vissers, M, Ullom, J, Wagoner, K, Xu, Z, Zhu, N, Vavagiakis E. M., Ahmed Z., Ali A., Arnold K., Austermann J., Bruno S. M., Choi S. K., Connors J., Cothard N., Dicker S., Dober B., Duff S., Fanfani V., Healy E., Henderson S., Ho S. -P. P., Hoang D. -T., Hilton G., Hubmayr J., Krachmalnicoff N., Li Y., Mates J., McCarrick H., Nati F., Niemack M., Silva-Feaver M., Staggs S., Stevens J., Vissers M., Ullom J., Wagoner K., Xu Z., Zhu N., Vavagiakis, E, Ahmed, Z, Ali, A, Arnold, K, Austermann, J, Bruno, S, Choi, S, Connors, J, Cothard, N, Dicker, S, Dober, B, Duff, S, Fanfani, V, Healy, E, Henderson, S, Ho, S, Hoang, D, Hilton, G, Hubmayr, J, Krachmalnicoff, N, Li, Y, Mates, J, Mccarrick, H, Nati, F, Niemack, M, Silva-Feaver, M, Staggs, S, Stevens, J, Vissers, M, Ullom, J, Wagoner, K, Xu, Z, Zhu, N, Vavagiakis E. M., Ahmed Z., Ali A., Arnold K., Austermann J., Bruno S. M., Choi S. K., Connors J., Cothard N., Dicker S., Dober B., Duff S., Fanfani V., Healy E., Henderson S., Ho S. -P. P., Hoang D. -T., Hilton G., Hubmayr J., Krachmalnicoff N., Li Y., Mates J., McCarrick H., Nati F., Niemack M., Silva-Feaver M., Staggs S., Stevens J., Vissers M., Ullom J., Wagoner K., Xu Z., and Zhu N.

Abstract

The Simons Observatory (SO) will be a cosmic microwave background (CMB) survey experiment with three small-aperture telescopes and one large-aperture telescope, which will observe from the Atacama Desert in Chile. In total, SO will field $\sim$70,000 transition-edge sensor (TES) bolometers in six spectral bands centered between 27 and 280 GHz in order to achieve the sensitivity necessary to measure or constrain numerous cosmological quantities. The SO Universal Focal Plane Modules (UFMs) each contain a 150 mm diameter TES detector array, horn or lenslet optical coupling, cold readout components, and magnetic shielding. SO will use a microwave SQUID multiplexing ($\mu$MUX) readout at an initial multiplexing factor of $\sim$1000; the cold (100 mK) readout components are packaged in a $\mu$MUX readout module, which is part of the UFM, and can also be characterized independently. The 100 mK stage TES bolometer arrays and microwave SQUIDs are sensitive to magnetic fields, and their measured response will vary with the degree to which they are magnetically shielded. We present measurements of the magnetic pickup of test microwave SQUID multiplexers as a study of various shielding configurations for the Simons Observatory. We discuss how these measurements motivated the material choice and design of the UFM magnetic shielding.

Published
2021

23. Erratum: The Simons Observatory Large Aperture Telescope Receiver (ApJS (2021) 256: 23 DOI: 10.3847/1538-4365/ac0db7)

Author

Zhu N., Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dunner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keating, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Zhu N., Bhandarkar T., Coppi G., Kofman A. M., Orlowski-Scherer J. L., Xu Z., Adachi S., Ade P., Aiola S., Austermann J., Bazarko A. O., Beall J. A., Bhimani S., Bond J. R., Chesmore G. E., Choi S. K., Connors J., Cothard N. F., Devlin M., Dicker S., Dober B., Duell C. J., Duff S. M., Dunner R., Fabbian G., Galitzki N., Gallardo P. A., Golec J. E., Haridas S. K., Harrington K., Healy E., Patty Ho S. -P., Huber Z. B., Hubmayr J., Iuliano J., Johnson B. R., Keating B., Kiuchi K., Koopman B. J., Lashner J., Lee A. T., Li Y., Limon M., Link M., Lucas T. J., McCarrick H., Moore J., Nati F., Newburgh L. B., Niemack M. D., Pierpaoli E., Randall M. J., Sarmiento K. P., Saunders L. J., Seibert J., Sierra C., Sonka R., Spisak J., Sutariya S., Tajima O., Teply G. P., Thornton R. J., Tsan T., Tucker C., Ullom J., Vavagiakis E. M., Vissers M. R., Walker S., Westbrook B., Wollack E. J., Zannoni M., Zhu N., Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dunner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keating, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Zhu N., Bhandarkar T., Coppi G., Kofman A. M., Orlowski-Scherer J. L., Xu Z., Adachi S., Ade P., Aiola S., Austermann J., Bazarko A. O., Beall J. A., Bhimani S., Bond J. R., Chesmore G. E., Choi S. K., Connors J., Cothard N. F., Devlin M., Dicker S., Dober B., Duell C. J., Duff S. M., Dunner R., Fabbian G., Galitzki N., Gallardo P. A., Golec J. E., Haridas S. K., Harrington K., Healy E., Patty Ho S. -P., Huber Z. B., Hubmayr J., Iuliano J., Johnson B. R., Keating B., Kiuchi K., Koopman B. J., Lashner J., Lee A. T., Li Y., Limon M., Link M., Lucas T. J., McCarrick H., Moore J., Nati F., Newburgh L. B., Niemack M. D., Pierpaoli E., Randall M. J., Sarmiento K. P., Saunders L. J., Seibert J., Sierra C., Sonka R., Spisak J., Sutariya S., Tajima O., Teply G. P., Thornton R. J., Tsan T., Tucker C., Ullom J., Vavagiakis E. M., Vissers M. R., Walker S., Westbrook B., Wollack E. J., and Zannoni M.

Abstract

After the publication of the article, it was brought to our attention that the description of Equation (1) may cause potential confusion. Thus, we have decided to provide a newer reference and added a unit for qtot in the description. The updated paragraph should read as the following:.

Published
2021

24. Development of a Microwave SQUID-Multiplexed TES Array for MUSTANG-2

Author

Stanchfield, S. M., Ade, P. A. R., Aguirre, J., Brevik, J. A., Cho, H. M., Datta, R., Devlin, M. J., Dicker, S. R., Dober, B., Egan, D., Ford, P., Hilton, G., Hubmayr, J., Irwin, K. D., Marganian, P., Mason, B. S., Mates, J. A. B., McMahon, J., Mello, M., Mroczkowski, T., Romero, C., Tucker, C., Vale, L., White, S., Whitehead, M., and Young, A. H.

Published
2016
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25. Characterization of Transition Edge Sensors for the Simons Observatory

Author

Stevens, J, Cothard, N, Vavagiakis, E, Ali, A, Arnold, K, Austermann, J, Choi, S, Dober, B, Duell, C, Duff, S, Hilton, G, Ho, S, Hoang, T, Hubmayr, J, Lee, A, Mangu, A, Nati, F, Niemack, M, Raum, C, Renzullo, M, Salatino, M, Sasse, T, Simon, S, Staggs, S, Suzuki, A, Truitt, P, Ullom, J, Vivalda, J, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Xu, Z, Yohannes, D, Stevens J. R., Cothard N. F., Vavagiakis E. M., Ali A., Arnold K., Austermann J. E., Choi S. K., Dober B. J., Duell C., Duff S. M., Hilton G. C., Ho S. -P. P., Hoang T. D., Hubmayr J., Lee A. T., Mangu A., Nati F., Niemack M. D., Raum C., Renzullo M., Salatino M., Sasse T., Simon S. M., Staggs S., Suzuki A., Truitt P., Ullom J., Vivalda J., Vissers M. R., Walker S., Westbrook B., Wollack E. J., Xu Z., Yohannes D., Stevens, J, Cothard, N, Vavagiakis, E, Ali, A, Arnold, K, Austermann, J, Choi, S, Dober, B, Duell, C, Duff, S, Hilton, G, Ho, S, Hoang, T, Hubmayr, J, Lee, A, Mangu, A, Nati, F, Niemack, M, Raum, C, Renzullo, M, Salatino, M, Sasse, T, Simon, S, Staggs, S, Suzuki, A, Truitt, P, Ullom, J, Vivalda, J, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Xu, Z, Yohannes, D, Stevens J. R., Cothard N. F., Vavagiakis E. M., Ali A., Arnold K., Austermann J. E., Choi S. K., Dober B. J., Duell C., Duff S. M., Hilton G. C., Ho S. -P. P., Hoang T. D., Hubmayr J., Lee A. T., Mangu A., Nati F., Niemack M. D., Raum C., Renzullo M., Salatino M., Sasse T., Simon S. M., Staggs S., Suzuki A., Truitt P., Ullom J., Vivalda J., Vissers M. R., Walker S., Westbrook B., Wollack E. J., Xu Z., and Yohannes D.

Abstract

The Simons Observatory is building both large (6 m) and small (0.5 m) aperture telescopes in the Atacama Desert in Chile to observe the cosmic microwave background CMB radiation with unprecedented sensitivity. Simons Observatory telescopes in total will use over 60,000 transition edge sensor (TES) detectors spanning center frequencies between 27 and 285 GHz and operating near 100 mK. TES devices have been fabricated for the Simons Observatory by NIST, Berkeley, and HYPRES/SeeQC corporation. Iterations of these devices have been tested cryogenically in order to inform the fabrication of further devices, which will culminate in the final TES designs to be deployed in the field. The detailed design specifications have been independently iterated at each fabrication facility for particular detector frequencies. We present test results for prototype devices, with emphasis on NIST high frequency detectors. A dilution refrigerator was used to achieve the required temperatures. Measurements were taken both with 4-lead resistance measurements and with a time-domain Superconducting Quantum Interference Device (SQUID) multiplexer system. The SQUID readout measurements include analysis of current versus voltage (IV) curves at various temperatures, square wave bias step measurements, and detector noise measurements. Normal resistance, superconducting critical temperature, saturation power, thermal and natural time constants, and thermal properties of the devices are extracted from these measurements.

Published
2020

26. In-flight performance of the BLAST-TNG Kinetic Inductance Detector arrays and Readout Electronics

Author

Sinclair, A, Gordon, S, Ade, P, Ashton, P, Cho, H, Coppi, G, Corso, A, Devlin, M, Dicker, S, Dober, B, Fissel, L, Galitzky, N, Gao, J, Groppi, C, Hilton, G, Hubmayr, J, Irwin, K, Klein, J, Li, D, Lourie, N, Lowe, I, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pascale, E, Pisano, G, Soler, J, Tucker, C, Underhil, M, Vissers, M, Wheeler, C, Williams, P, Sinclair A., Gordon S. B., Ade P., Ashton P., Cho H. -M., Coppi G., Corso A., Devlin M., Dicker S., Dober B., Fissel L., Galitzky N., Gao J., Groppi C., Hilton G. C., Hubmayr J., Irwin K., Klein J., Li D., Lourie N., Lowe I., Mani H., Mauskopf P. D., McKenney C., Nati F., Novak G., Pascale E., Pisano G., Soler J., Tucker C., Underhil M., Vissers M., Wheeler C., Williams P., Sinclair, A, Gordon, S, Ade, P, Ashton, P, Cho, H, Coppi, G, Corso, A, Devlin, M, Dicker, S, Dober, B, Fissel, L, Galitzky, N, Gao, J, Groppi, C, Hilton, G, Hubmayr, J, Irwin, K, Klein, J, Li, D, Lourie, N, Lowe, I, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pascale, E, Pisano, G, Soler, J, Tucker, C, Underhil, M, Vissers, M, Wheeler, C, Williams, P, Sinclair A., Gordon S. B., Ade P., Ashton P., Cho H. -M., Coppi G., Corso A., Devlin M., Dicker S., Dober B., Fissel L., Galitzky N., Gao J., Groppi C., Hilton G. C., Hubmayr J., Irwin K., Klein J., Li D., Lourie N., Lowe I., Mani H., Mauskopf P. D., McKenney C., Nati F., Novak G., Pascale E., Pisano G., Soler J., Tucker C., Underhil M., Vissers M., Wheeler C., and Williams P.

Published
2020

27. Characterization, deployment, and in-flight performance of the BLAST-TNG cryogenic receiver

Author

Zmuidzinas J.,Gao J.-R., Lowe, I, Ade, P, Ashton, P, Austermann, J, Coppi, G, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lourie, N, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pisano, G, Romualdez, J, Soler, J, Sinclair, A, Tucker, C, Ullom, J, Vissers, M, Wheeler, C, Williams, P, Lowe I., Ade P. A. R., Ashton P. C., Austermann J. E., Coppi G., Cox E. G., Devlin M. J., Dober B. J., Fanfani V., Fissel L. M., Galitzki N., Gao J., Gordon S., Groppi C. E., Hilton G. C., Hubmayr J., Klein J., Li D., Lourie N. P., Mani H., Mauskopf P., McKenney C., Nati F., Novak G., Pisano G., Romualdez J., Soler J. D., Sinclair A., Tucker C., Ullom J., Vissers M., Wheeler C., Williams P. A., Zmuidzinas J.,Gao J.-R., Lowe, I, Ade, P, Ashton, P, Austermann, J, Coppi, G, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lourie, N, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pisano, G, Romualdez, J, Soler, J, Sinclair, A, Tucker, C, Ullom, J, Vissers, M, Wheeler, C, Williams, P, Lowe I., Ade P. A. R., Ashton P. C., Austermann J. E., Coppi G., Cox E. G., Devlin M. J., Dober B. J., Fanfani V., Fissel L. M., Galitzki N., Gao J., Gordon S., Groppi C. E., Hilton G. C., Hubmayr J., Klein J., Li D., Lourie N. P., Mani H., Mauskopf P., McKenney C., Nati F., Novak G., Pisano G., Romualdez J., Soler J. D., Sinclair A., Tucker C., Ullom J., Vissers M., Wheeler C., and Williams P. A.

Abstract

The Next Generation Balloon-borne Large Aperture Submillimeter Telescope (BLAST-TNG) is a submillimeter polarimeter designed to map interstellar dust and galactic foregrounds at 250, 350, and 500 microns during a 24-day Antarctic flight. The BLAST-TNG detector arrays are comprised of 918, 469, and 272 MKID pixels, respectively. The pixels are formed from two orthogonally oriented, crossed, linear-polarization sensitive MKID antennae. The arrays are cooled to sub 300 mK temperatures and stabilized via a closed cycle 3He sorption fridge in combination with a 4He vacuum pot. The detectors are read out through a combination of the second-generation Reconfigurable Open Architecture Computing Hardware (ROACH2) and custom RF electronics designed for BLAST-TNG. The firmware and software designed to readout and characterize these detectors was built from scratch by the BLAST team around these detectors, and has been adapted for use by other MKID instruments such as TolTEC and OLIMPO.1 We present an overview of these systems as well as in-depth methodology of the ground-based characterization and the measured in-flight performance.

Published
2020

30. In-flight performance of the BLAST-TNG Kinetic Inductance Detector arrays and Readout Electronics

Author

Sinclair A., Gordon S. B., Ade P., Ashton P., Cho H. -M., Coppi G., Corso A., Devlin M., Dicker S., Dober B., Fissel L., Galitzky N., Gao J., Groppi C., Hilton G. C., Hubmayr J., Irwin K., Klein J., Li D., Lourie N., Lowe I., Mani H., Mauskopf P. D., McKenney C., Nati F., Novak G., Pascale E., Pisano G., Soler J., Tucker C., Underhil M., Vissers M., Wheeler C., Williams P., Sinclair, A, Gordon, S, Ade, P, Ashton, P, Cho, H, Coppi, G, Corso, A, Devlin, M, Dicker, S, Dober, B, Fissel, L, Galitzky, N, Gao, J, Groppi, C, Hilton, G, Hubmayr, J, Irwin, K, Klein, J, Li, D, Lourie, N, Lowe, I, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pascale, E, Pisano, G, Soler, J, Tucker, C, Underhil, M, Vissers, M, Wheeler, C, and Williams, P

Subjects
kinetic inductance detectors, infrared astronomy, balloon borne telescopes
Published
2020

31. The Simons Observatory Large Aperture Telescope Receiver

Author

Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Richard Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dünner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keatin, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, J Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Perez Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Ningfeng Zhu, Tanay Bhandarkar, Gabriele Coppi, Anna M. Kofman, John L. Orlowski-Scherer, Zhilei Xu, Shunsuke Adachi, Peter Ade, Simone Aiola, Jason Austermann, Andrew O. Bazarko, James A. Beall, Sanah Bhimani, J. Richard Bond, Grace E. Chesmore, Steve K. Choi, Jake Connors, Nicholas F. Cothard, Mark Devlin, Simon Dicker, Bradley Dober, Cody J. Duell, Shannon M. Duff, Rolando Dünner, Giulio Fabbian, Nicholas Galitzki, Patricio A. Gallardo, Joseph E. Golec, Saianeesh K. Haridas, Kathleen Harrington, Erin Healy, Shuay-Pwu Patty Ho, Zachary B. Huber, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Brian Keatin, Kenji Kiuchi, Brian J. Koopman, Jack Lashner, Adrian T. Lee, Yaqiong Li, Michele Limon, Michael Link, Tammy J Lucas, Heather McCarrick, Jenna Moore, Federico Nati, Laura B. Newburgh, Michael D. Niemack, Elena Pierpaoli, Michael J. Randall, Karen Perez Sarmiento, Lauren J. Saunders, Joseph Seibert, Carlos Sierra, Rita Sonka, Jacob Spisak, Shreya Sutariya, Osamu Tajima, Grant P. Teply, Robert J. Thornton, Tran Tsan, Carole Tucker, Joel Ullom, Eve M. Vavagiakis, Michael R. Vissers, Samantha Walker, Benjamin Westbrook, Edward J. Wollack, Mario Zannoni, Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Richard Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dünner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keatin, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, J Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Perez Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Ningfeng Zhu, Tanay Bhandarkar, Gabriele Coppi, Anna M. Kofman, John L. Orlowski-Scherer, Zhilei Xu, Shunsuke Adachi, Peter Ade, Simone Aiola, Jason Austermann, Andrew O. Bazarko, James A. Beall, Sanah Bhimani, J. Richard Bond, Grace E. Chesmore, Steve K. Choi, Jake Connors, Nicholas F. Cothard, Mark Devlin, Simon Dicker, Bradley Dober, Cody J. Duell, Shannon M. Duff, Rolando Dünner, Giulio Fabbian, Nicholas Galitzki, Patricio A. Gallardo, Joseph E. Golec, Saianeesh K. Haridas, Kathleen Harrington, Erin Healy, Shuay-Pwu Patty Ho, Zachary B. Huber, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Brian Keatin, Kenji Kiuchi, Brian J. Koopman, Jack Lashner, Adrian T. Lee, Yaqiong Li, Michele Limon, Michael Link, Tammy J Lucas, Heather McCarrick, Jenna Moore, Federico Nati, Laura B. Newburgh, Michael D. Niemack, Elena Pierpaoli, Michael J. Randall, Karen Perez Sarmiento, Lauren J. Saunders, Joseph Seibert, Carlos Sierra, Rita Sonka, Jacob Spisak, Shreya Sutariya, Osamu Tajima, Grant P. Teply, Robert J. Thornton, Tran Tsan, Carole Tucker, Joel Ullom, Eve M. Vavagiakis, Michael R. Vissers, Samantha Walker, Benjamin Westbrook, Edward J. Wollack, and Mario Zannoni

Abstract

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.

Published
2021

32. A microwave SQUID multiplexer optimized for bolometric applications

Author

Dober, B., primary, Ahmed, Z., additional, Arnold, K., additional, Becker, D. T., additional, Bennett, D. A., additional, Connors, J. A., additional, Cukierman, A., additional, D'Ewart, J. M., additional, Duff, S. M., additional, Dusatko, J. E., additional, Frisch, J. C., additional, Gard, J. D., additional, Henderson, S. W., additional, Herbst, R., additional, Hilton, G. C., additional, Hubmayr, J., additional, Li, Y., additional, Mates, J. A. B., additional, McCarrick, H., additional, Reintsema, C. D., additional, Silva-Feaver, M., additional, Ruckman, L., additional, Ullom, J. N., additional, Vale, L. R., additional, Van Winkle, D. D., additional, Vasquez, J., additional, Wang, Y., additional, Young, E., additional, Yu, C., additional, and Zheng, K., additional

Published
2021
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33. Magnetic Sensitivity of AlMn TESes and Shielding Considerations for Next-Generation CMB Surveys

Author

Vavagiakis, E, Henderson, S, Zheng, K, Cho, H, Cothard, N, Dober, B, Duff, S, Gallardo, P, Hilton, G, Hubmayr, J, Irwin, K, Koopman, B, Li, D, Nati, F, Niemack, M, Reintsema, C, Simon, S, Stevens, J, Suzuki, A, Westbrook, B, Vavagiakis E. M., Henderson S. W., Zheng K., Cho H. -M., Cothard N. F., Dober B., Duff S. M., Gallardo P. A., Hilton G., Hubmayr J., Irwin K. D., Koopman B. J., Li D., Nati F., Niemack M. D., Reintsema C. D., Simon S., Stevens J. R., SUZUKI, AKANE, Westbrook B., Vavagiakis, E, Henderson, S, Zheng, K, Cho, H, Cothard, N, Dober, B, Duff, S, Gallardo, P, Hilton, G, Hubmayr, J, Irwin, K, Koopman, B, Li, D, Nati, F, Niemack, M, Reintsema, C, Simon, S, Stevens, J, Suzuki, A, Westbrook, B, Vavagiakis E. M., Henderson S. W., Zheng K., Cho H. -M., Cothard N. F., Dober B., Duff S. M., Gallardo P. A., Hilton G., Hubmayr J., Irwin K. D., Koopman B. J., Li D., Nati F., Niemack M. D., Reintsema C. D., Simon S., Stevens J. R., SUZUKI, AKANE, and Westbrook B.

Abstract

In the next decade, new ground-based cosmic microwave background (CMB) experiments such as Simons Observatory, CCAT-prime, and CMB-S4 will increase the number of detectors observing the CMB by an order of magnitude or more, dramatically improving our understanding of cosmology and astrophysics. These projects will deploy receivers with as many as hundreds of thousands of transition edge sensor (TES) bolometers coupled to superconducting quantum interference device (SQUID)-based readout systems. It is well known that superconducting devices such as TESes and SQUIDs are sensitive to magnetic fields. However, the effects of magnetic fields on TESes are not easily predicted due to the complex behavior of the superconducting transition, which motivates direct measurements of the magnetic sensitivity of these devices. We present comparative four-lead measurements of the critical temperature versus applied magnetic field of AlMn TESes varying in geometry, doping, and leg length, including Advanced ACT and POLARBEAR-2/Simons Array bolometers. MoCu ACTPol TESes are also tested and are found to be more sensitive to magnetic fields than the AlMn devices. We present an observation of weak-link-like behavior in AlMn TESes at low critical currents. We also compare measurements of magnetic sensitivity for time division multiplexing SQUIDs and frequency division multiplexing microwave rf-SQUIDs. We discuss the implications of our measurements on the magnetic shielding required for future experiments that aim to map the CMB to near-fundamental limits.

Published
2018

34. The Simons Observatory: Instrument overview

Author

Jonas Zmuidzinas, Jian-Rong Gao, Galitzki, N, Ali, A, Arnold, K, Ashton, P, Austermann, J, Baccigalupi, C, Baildon, T, Barron, D, Beall, J, Beckman, S, Bruno, S, Bryan, S, Calisse, P, Chesmore, G, Chinone, Y, Choi, S, Coppi, G, Crowley, K, Cukierman, A, Devlin, M, Dicker, S, Dober, B, Duff, S, Dunkley, J, Fabbian, G, Gallardo, P, Gerbino, M, Goeckner-Wald, N, Golec, J, Gudmundsson, J, Healy, E, Henderson, S, Hill, C, Hilton, G, Ho, S, Howe, L, Hubmayr, J, Jeong, O, Keating, B, Koopman, B, Kiuchi, K, Kusaka, A, Lashner, J, Lee, A, Li, Y, Limon, M, Lungu, M, Matsuda, F, Mauskopf, P, May, A, Mccallum, N, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Piccirillo, L, Sathyanarayana Rao, M, Raum, C, Salatino, M, Seibert, J, Sierra, C, Silva-Feaver, M, Simon, S, Staggs, S, Stevens, J, Suzuki, A, Teply, G, Thornton, R, Tsai, C, Ullom, J, Vavagiakis, E, Vissers, M, Westbrook, B, Wollack, E, Xu, Z, Zhu, N, Galitzki N., Ali A., Arnold K. S., Ashton P. C., Austermann J. E., Baccigalupi C., Baildon T., Barron D., Beall J. A., Beckman S., Bruno S. M. M., Bryan S., Calisse P. G., Chesmore G. E., Chinone Y., Choi S. K., Coppi G., Crowley K. D., Crowley K. T., Cukierman A., Devlin M. J., Dicker S., Dober B., Duff S. M., Dunkley J., Fabbian G., Gallardo P. A., Gerbino M., Goeckner-Wald N., Golec J. E., Gudmundsson J. E., Healy E. E., Henderson S., Hill C. A., Hilton G. C., Ho S. -P. P., Howe L. A., Hubmayr J., Jeong O., Keating B., Koopman B. J., Kiuchi K., Kusaka A., Lashner J., Lee A. T., Li Y., Limon M., Lungu M., Matsuda F., Mauskopf P. D., May A. J., McCallum N., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Piccirillo L., Sathyanarayana Rao M., Raum C., Salatino M., Seibert J. S., Sierra C., Silva-Feaver M., Simon S. M., Staggs S. T., Stevens J. R., Suzuki A., Teply G., Thornton R., Tsai C., Ullom J. N., Vavagiakis E. M., Vissers M. R., Westbrook B., Wollack E. J., Xu Z., Zhu N., Jonas Zmuidzinas, Jian-Rong Gao, Galitzki, N, Ali, A, Arnold, K, Ashton, P, Austermann, J, Baccigalupi, C, Baildon, T, Barron, D, Beall, J, Beckman, S, Bruno, S, Bryan, S, Calisse, P, Chesmore, G, Chinone, Y, Choi, S, Coppi, G, Crowley, K, Cukierman, A, Devlin, M, Dicker, S, Dober, B, Duff, S, Dunkley, J, Fabbian, G, Gallardo, P, Gerbino, M, Goeckner-Wald, N, Golec, J, Gudmundsson, J, Healy, E, Henderson, S, Hill, C, Hilton, G, Ho, S, Howe, L, Hubmayr, J, Jeong, O, Keating, B, Koopman, B, Kiuchi, K, Kusaka, A, Lashner, J, Lee, A, Li, Y, Limon, M, Lungu, M, Matsuda, F, Mauskopf, P, May, A, Mccallum, N, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Piccirillo, L, Sathyanarayana Rao, M, Raum, C, Salatino, M, Seibert, J, Sierra, C, Silva-Feaver, M, Simon, S, Staggs, S, Stevens, J, Suzuki, A, Teply, G, Thornton, R, Tsai, C, Ullom, J, Vavagiakis, E, Vissers, M, Westbrook, B, Wollack, E, Xu, Z, Zhu, N, Galitzki N., Ali A., Arnold K. S., Ashton P. C., Austermann J. E., Baccigalupi C., Baildon T., Barron D., Beall J. A., Beckman S., Bruno S. M. M., Bryan S., Calisse P. G., Chesmore G. E., Chinone Y., Choi S. K., Coppi G., Crowley K. D., Crowley K. T., Cukierman A., Devlin M. J., Dicker S., Dober B., Duff S. M., Dunkley J., Fabbian G., Gallardo P. A., Gerbino M., Goeckner-Wald N., Golec J. E., Gudmundsson J. E., Healy E. E., Henderson S., Hill C. A., Hilton G. C., Ho S. -P. P., Howe L. A., Hubmayr J., Jeong O., Keating B., Koopman B. J., Kiuchi K., Kusaka A., Lashner J., Lee A. T., Li Y., Limon M., Lungu M., Matsuda F., Mauskopf P. D., May A. J., McCallum N., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Piccirillo L., Sathyanarayana Rao M., Raum C., Salatino M., Seibert J. S., Sierra C., Silva-Feaver M., Simon S. M., Staggs S. T., Stevens J. R., Suzuki A., Teply G., Thornton R., Tsai C., Ullom J. N., Vavagiakis E. M., Vissers M. R., Westbrook B., Wollack E. J., Xu Z., and Zhu N.

Abstract

The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales between 1 arcminute and tens of degrees, contain over 40,000 detectors, and sample frequencies between 27 and 270 GHz. SO will consist of a six-meter-aperture telescope coupled to over 20,000 detectors along with an array of half-meter aperture refractive cameras, coupled to an additional 20,000+ detectors. The unique combination of large and small apertures in a single CMB observatory, which will be located in the Atacama Desert at an altitude of 5190 m, will allow us to sample a wide range of angular scales over a common survey area. SO will measure fundamental cosmological parameters of our universe, find high redshift clusters via the Sunyaev-Zeldovich effect, constrain properties of neutrinos, and seek signatures of dark matter through gravitational lensing. The complex set of technical and science requirements for this experiment has led to innovative instrumentation solutions which we will discuss. The large aperture telescope will couple to a cryogenic receiver that is 2.4 m in diameter and over 2 m long, creating a number of interesting technical challenges. Concurrently, we are designing an array of half-meter-aperture cryogenic cameras which also have compelling design challenges. We will give an overview of the drivers for and designs of the SO telescopes and the cryogenic cameras that will house the cold optical components and detector arrays.

Published
2018

35. Studies of systematic uncertainties for Simons Observatory: Detector array effects

Author

Gao, JR, Crowley, K, Simon, S, Silva-Feaver, M, Goeckner-Wald, N, Ali, A, Austermann, J, Brown, M, Chinone, Y, Cukierman, A, Dober, B, Duff, S, Dunkley, J, Errard, J, Fabbian, G, Gallardo, P, Ho, S, Hubmayr, J, Keating, B, Kusaka, A, Mccallum, N, Mcmahon, J, Nati, F, Niemack, M, Puglisi, G, Sathyanarayana Rao, M, Reichardt, C, Salatino, M, Siritanasak, P, Staggs, S, Suzuki, A, Teply, G, Thomas, D, Ullom, J, Verges, C, Vissers, M, Westbrook, B, Wollack, E, Xu, Z, Zhu, N, Crowley K. T., Simon S. M., Silva-Feaver M., Goeckner-Wald N., Ali A., Austermann J., Brown M. L., Chinone Y., Cukierman A., Dober B., Duff S. M., Dunkley J., Errard J., Fabbian G., Gallardo P. A., Ho S. -P. P., Hubmayr J., Keating B., Kusaka A., McCallum N., McMahon J., Nati F., Niemack M. D., Puglisi G., Sathyanarayana Rao M., Reichardt C. L., Salatino M., Siritanasak P., Staggs S., Suzuki A., Teply G., Thomas D. B., Ullom J. N., Verges C., Vissers M. R., Westbrook B., Wollack E. J., Xu Z., Zhu N., Gao, JR, Crowley, K, Simon, S, Silva-Feaver, M, Goeckner-Wald, N, Ali, A, Austermann, J, Brown, M, Chinone, Y, Cukierman, A, Dober, B, Duff, S, Dunkley, J, Errard, J, Fabbian, G, Gallardo, P, Ho, S, Hubmayr, J, Keating, B, Kusaka, A, Mccallum, N, Mcmahon, J, Nati, F, Niemack, M, Puglisi, G, Sathyanarayana Rao, M, Reichardt, C, Salatino, M, Siritanasak, P, Staggs, S, Suzuki, A, Teply, G, Thomas, D, Ullom, J, Verges, C, Vissers, M, Westbrook, B, Wollack, E, Xu, Z, Zhu, N, Crowley K. T., Simon S. M., Silva-Feaver M., Goeckner-Wald N., Ali A., Austermann J., Brown M. L., Chinone Y., Cukierman A., Dober B., Duff S. M., Dunkley J., Errard J., Fabbian G., Gallardo P. A., Ho S. -P. P., Hubmayr J., Keating B., Kusaka A., McCallum N., McMahon J., Nati F., Niemack M. D., Puglisi G., Sathyanarayana Rao M., Reichardt C. L., Salatino M., Siritanasak P., Staggs S., Suzuki A., Teply G., Thomas D. B., Ullom J. N., Verges C., Vissers M. R., Westbrook B., Wollack E. J., Xu Z., and Zhu N.

Abstract

In this proceeding, we present studies of instrumental systematic effects for the Simons Obsevatory (SO) that are associated with the detector system and its interaction with the full SO experimental systems. SO will measure the Cosmic Microwave Background (CMB) temperature and polarization anisotropies over a wide range of angular scales in six bands with bandcenters spanning from 27 GHz to 270 GHz. We explore effects including intensity-to-polarization leakage due to coupling optics, bolometer nonlinearity, uncalibrated gain variations of bolometers, and readout crosstalk. We model the level of signal contamination, discuss proposed mitigation schemes, and present instrument requirements to inform the design of SO and future CMB projects.

Published
2018

36. Preflight characterization of the BLAST-TNG receiver and detector arrays

Author

Zmuidzinas, Jona, Gao, Jian-Rong, Lourie, N, Ade, P, Angile, F, Ashton, P, Austermann, J, Devlin, M, Dober, B, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Klein, J, Hilton, G, Hubmayr, J, Li, D, Lowe, I, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pascale, E, Pisano, G, Sinclair, A, Soler, J, Tucker, C, Ullom, J, Vissers, M, Williams, P, Lourie N. P., Ade P. A. R., Angile F. E., Ashton P. C., Austermann J. E., Devlin M. J., Dober B., Galitzki N., Gao J., Gordon S., Groppi C. E., Klein J., Hilton G. C., Hubmayr J., Li D., Lowe I., Mani H., Mauskopf P., McKenney C. M., Nati F., Novak G., Pascale E., Pisano G., Sinclair A., Soler J. D., Tucker C., Ullom J. N., Vissers M., Williams P. A., Zmuidzinas, Jona, Gao, Jian-Rong, Lourie, N, Ade, P, Angile, F, Ashton, P, Austermann, J, Devlin, M, Dober, B, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Klein, J, Hilton, G, Hubmayr, J, Li, D, Lowe, I, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pascale, E, Pisano, G, Sinclair, A, Soler, J, Tucker, C, Ullom, J, Vissers, M, Williams, P, Lourie N. P., Ade P. A. R., Angile F. E., Ashton P. C., Austermann J. E., Devlin M. J., Dober B., Galitzki N., Gao J., Gordon S., Groppi C. E., Klein J., Hilton G. C., Hubmayr J., Li D., Lowe I., Mani H., Mauskopf P., McKenney C. M., Nati F., Novak G., Pascale E., Pisano G., Sinclair A., Soler J. D., Tucker C., Ullom J. N., Vissers M., and Williams P. A.

Abstract

The Next Generation Balloon-borne Large Aperture Submillimeter Telescope (BLAST-TNG) is a submillimeter mapping experiment planned for a 28 day long-duration balloon (LDB) flight from McMurdo Station, Antarctica during the 2018-2019 season. BLAST-TNG will detect submillimeter polarized interstellar dust emission, tracing magnetic fields in galactic molecular clouds. BLAST-TNG will be the first polarimeter with the sensitivity and resolution to probe the similar to 0.1 parsec-scale features that are critical to understanding the origin of structures in the interstellar medium.BLAST-TNG features three detector arrays operating at wavelengths of 250, 350, and 500 mu m (1200, 857, and 600 GHz) comprised of 918, 469, and 272 dual-polarization pixels, respectively. Each pixel is made up of two crossed microwave kinetic inductance detectors (MKIDs). These arrays are cooled to 275 mK in a cryogenic receiver. Each MKID has a different resonant frequency, allowing hundreds of resonators to be read out on a single transmission line. This inherent ability to be frequency-domain multiplexed simplifies the cryogenic readout hardware, but requires careful optical testing to map out the physical location of each resonator on the focal plane. Receiver-level optical testing was carried out using both a cryogenic source mounted to a movable xy-stage with a shutter, and a beam-filling, heated blackbody source able to provide a 10-50 degrees C temperature chop. The focal plane array noise properties, responsivity, polarization efficiency, instrumental polarization were measured. We present the preflight characterization of the BLAST-TNG cryogenic system and array-level optical testing of the MKID detector arrays in the flight receiver.

Published
2018

37. Design and characterization of a balloon-borne diffraction-limited submillimeter telescope platform for BLAST-TNG

Author

Marshall, Heather K, Spyromilio, Jason, Lourie, N, Angile, F, Ashton, P, Catanzaro, B, Devlin, M, Dicker, S, Didier, J, Dober, B, Fissel, L, Galitzki, N, Gordon, S, Klein, J, Lowe, I, Mauskopf, P, Nati, F, Novak, G, Romualdez, L, Soler, J, Williams, P, Lourie N. P., Angile F. E., Ashton P. C., Catanzaro B., Devlin M. J., Dicker S., Didier J., Dober B., Fissel L. M., Galitzki N., Gordon S., Klein J., Lowe I., Mauskopf P., Nati F., Novak G., Romualdez L. J., Soler J. D., Williams P. A., Marshall, Heather K, Spyromilio, Jason, Lourie, N, Angile, F, Ashton, P, Catanzaro, B, Devlin, M, Dicker, S, Didier, J, Dober, B, Fissel, L, Galitzki, N, Gordon, S, Klein, J, Lowe, I, Mauskopf, P, Nati, F, Novak, G, Romualdez, L, Soler, J, Williams, P, Lourie N. P., Angile F. E., Ashton P. C., Catanzaro B., Devlin M. J., Dicker S., Didier J., Dober B., Fissel L. M., Galitzki N., Gordon S., Klein J., Lowe I., Mauskopf P., Nati F., Novak G., Romualdez L. J., Soler J. D., and Williams P. A.

Abstract

The Next Generation Balloon-borne Large Aperture Submillimeter Telescope (BLAST-TNG) is a submillimeter mapping experiment planned for a 28 day long-duration balloon (LDB) flight from McMurdo Station, Antarctica during the 2018-2019 season. BLAST-TNG will detect submillimeter polarized interstellar dust emission, tracing magnetic fields in galactic molecular clouds. BLAST-TNG will be the first polarimeter with the sensitivity and resolution to probe the similar to 0.1 parsec-scale features that are critical to understanding the origin of structures in the interstellar medium. With three detector arrays operating at 250, 350, and 500 mu m (1200, 857, and 600 GHz), BLAST-TNG will obtain diffraction-limited resolution at each waveband of 30, 41, and 59 arcseconds respectively.To achieve the submillimeter resolution necessary for its science goals, the BLAST-TNG telescope features a 2.5 m aperture carbon fiber composite primary mirror, one of the largest mirrors flown on a balloon platform. Successful performance of such a large telescope on a balloon-borne platform requires stiff, lightweight optical components and mounting structures. Through a combination of optical metrology and finite element modeling of thermal and mechanical stresses on both the telescope optics and mounting structures, we expect diffraction-limited resolution at all our wavebands. We expect pointing errors due to deformation of the telescope mount to be negligible. We have developed a detailed thermal model of the sun shielding, gondola, and optical components to optimize our observing strategy and increase the stability of the telescope over the flight. We present preflight characterization of the telescope and its platform.

Published
2018

38. Simons Observatory Small Aperture Telescope overview

Author

Marshall, HK, Spyromilio, J, Usuda, T, Kiuchi, K, Adachi, S, Ali, AM, Arnold, K, Ashton, P, Austermann, JE, Bazako, A, Beall, JA, Chinone, Y, Coppi, G, Crowley, KD, Crowley, KT, Dicker, S, Dober, B, Duff, SM, Fabbian, G, Galitzki, N, Golec, JE, Gudmundsson, JE, Harrington, K, Hasegawa, M, Hattori, M, Hill, CA, Ho, SPP, Hubmayr, J, Johnson, BR, Kaneko, D, Katayama, N, Keating, B, Kusaka, A, Lashner, J, Lee, AT, Matsuda, F, McCarrick, H, Murata, M, Nati, F, Nishinomiya, Y, Page, L, Sathyanarayana Rao, M, Reichardt, CL, Sakaguri, K, Sakurai, Y, Sibert, J, Spisak, J, Tajima, O, Teply, GP, Terasaki, T, Tsan, T, Walker, S, Wollack, EJ, Xu, Z, Yamada, K, Zannoni, M, Zhu, N, Marshall, HK, Spyromilio, J, Usuda, T, Kiuchi, K, Adachi, S, Ali, AM, Arnold, K, Ashton, P, Austermann, JE, Bazako, A, Beall, JA, Chinone, Y, Coppi, G, Crowley, KD, Crowley, KT, Dicker, S, Dober, B, Duff, SM, Fabbian, G, Galitzki, N, Golec, JE, Gudmundsson, JE, Harrington, K, Hasegawa, M, Hattori, M, Hill, CA, Ho, SPP, Hubmayr, J, Johnson, BR, Kaneko, D, Katayama, N, Keating, B, Kusaka, A, Lashner, J, Lee, AT, Matsuda, F, McCarrick, H, Murata, M, Nati, F, Nishinomiya, Y, Page, L, Sathyanarayana Rao, M, Reichardt, CL, Sakaguri, K, Sakurai, Y, Sibert, J, Spisak, J, Tajima, O, Teply, GP, Terasaki, T, Tsan, T, Walker, S, Wollack, EJ, Xu, Z, Yamada, K, Zannoni, M, and Zhu, N

Abstract

The Simons Observatory (SO) will be a cosmic microwave background (CMB) survey experiment with three small-aperture telescopes (SATs) and one large-aperture telescope (LAT), which will observe from the Atacama Desert in Chile. In total, SO will field over 60,000 transition-edge sensor (TES) bolometers in six spectral bands centered between 27 and 280 GHz in order to achieve the sensitivity necessary to measure or constrain numerous cosmological quantities. The SATs are optimized for a primordial gravitational wave signal in a parity odd polarization power spectrum at a large angular scale. We will present the latest status of the SAT development.

Published
2020

39. The Balloon-borne Large Aperture Submillimeter Telescope Observatory

Author

Lowe, I, Coppi, G, Ade, P, Ashton, P, Austermann, J, Beall, J, Clark, S, Cox, E, Devlin, M, Dicker, S, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Hensley, B, Hubmayr, J, Li, S, Li, Z, Lourie, N, Martin, P, Mauskopf, P, Nati, F, Novak, G, Pisano, G, Romualdez, L, Sinclair, A, Soler, J, Tucker, C, Vissers, M, Wheeler, J, Williams, P, Zannoni, M, Lowe, Ian N., Coppi, Gabriele, Ade, Peter A., Ashton, Peter C., Austermann, Jason E., Beall, James, Clark, Susan, Cox, Erin G., Devlin, Mark J., Dicker, Simon, Dober, Bradley J., Fanfani, Valentina, Fissel, Laura M., Galitzki, Nicholas, Gao, Jiangsong, Hensley, Brandon, Hubmayr, Johannes, Li, Steven, Li, Zhi-yun, Lourie, Nathan P., Martin, Peter G., Mauskopf, Philip, Nati, Federico, Novak, Giles, Pisano, Giampaolo, Romualdez, L J., Sinclair, Adrian, Soler, Juan D., Tucker, Carole, Vissers, Michael, Wheeler, Jordan, Williams, Paul A., Zannoni, Mario, Lowe, I, Coppi, G, Ade, P, Ashton, P, Austermann, J, Beall, J, Clark, S, Cox, E, Devlin, M, Dicker, S, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Hensley, B, Hubmayr, J, Li, S, Li, Z, Lourie, N, Martin, P, Mauskopf, P, Nati, F, Novak, G, Pisano, G, Romualdez, L, Sinclair, A, Soler, J, Tucker, C, Vissers, M, Wheeler, J, Williams, P, Zannoni, M, Lowe, Ian N., Coppi, Gabriele, Ade, Peter A., Ashton, Peter C., Austermann, Jason E., Beall, James, Clark, Susan, Cox, Erin G., Devlin, Mark J., Dicker, Simon, Dober, Bradley J., Fanfani, Valentina, Fissel, Laura M., Galitzki, Nicholas, Gao, Jiangsong, Hensley, Brandon, Hubmayr, Johannes, Li, Steven, Li, Zhi-yun, Lourie, Nathan P., Martin, Peter G., Mauskopf, Philip, Nati, Federico, Novak, Giles, Pisano, Giampaolo, Romualdez, L J., Sinclair, Adrian, Soler, Juan D., Tucker, Carole, Vissers, Michael, Wheeler, Jordan, Williams, Paul A., and Zannoni, Mario

Abstract

The BLAST Observatory is a proposed superpressure balloon-borne polarimeter designed for a future ultra- long duration balloon campaign from Wanaka, New Zealand. To maximize scientific output while staying within the stringent superpressure weight envelope, BLAST will feature new 1.8m off-axis optical system contained within a lightweight monocoque structure gondola. The payload will incorporate a 300 L 4He cryogenic receiver which will cool 8,274 microwave kinetic inductance detectors (MKIDs) to 100mK through the use of an adiabatic demagnetization refrigerator (ADR) in combination with a 3He sorption refrigerator all backed by a liquid helium pumped pot operating at 2 K. The detector readout utilizes a new Xilinx RFSOC-based system which will run the next-generation of the BLAST-TNG KIDPy software. With this instrument we aim to answer outstanding questions about dust dynamics as well as provide community access to the polarized submillimeter sky made possible by high-altitude observing unrestricted by atmospheric transmission. The BLAST Observatory is designed for a minimum 31-day flight of which 70% will be dedicated to observations for BLAST scientific goals and the remaining 30% will be open to proposals from the wider astronomical community through a shared-risk proposals program.

Published
2020

40. In-flight performance of the BLAST-TNG telescope platform

Author

Marshall, HK, Spyromilio, J, Usuda, T, Coppi, G, Ade, P, Ashton, P, Austermann, J, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lowe, I, Lourie, N, Mckinney, C, Mani, H, Mauskopf, P, Nati, F, Novak, G, Pisano, G, Romualdez, J, Sinclair, A, Soler, J, Tucker, C, Ullom, J, Visser, M, Wheeler, C, Williams, P, Coppi, Gabriele, Ade, Peter A., Ashton, Peter C., Austermann, Jason E., Cox, Erin G., Devlin, Mark J., Dober, Bradley J., Fanfani, Valentina, Fissel, Laura M., Galitzki, Nicholas B., Gao, Jiansong, Gordon, Samuel, Groppi, Christopher E., Hilton, Gene C., Hubmayr, Johannes, Klein, Jeffrey, Li, Dale, Lowe, Ian, Lourie, Nathan P., Mckinney, Christopher, Mani, Hamdi, Mauskopf, Philip D., Nati, Federico, Novak, Giles, Pisano, Giampaolo, Romualdez, Javier L., Sinclair, Adrian K., Soler, Juan D., Tucker, Carole, Ullom, Joel, Visser, Michael, Wheeler, Caleb H., Williams, Paul A., Marshall, HK, Spyromilio, J, Usuda, T, Coppi, G, Ade, P, Ashton, P, Austermann, J, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lowe, I, Lourie, N, Mckinney, C, Mani, H, Mauskopf, P, Nati, F, Novak, G, Pisano, G, Romualdez, J, Sinclair, A, Soler, J, Tucker, C, Ullom, J, Visser, M, Wheeler, C, Williams, P, Coppi, Gabriele, Ade, Peter A., Ashton, Peter C., Austermann, Jason E., Cox, Erin G., Devlin, Mark J., Dober, Bradley J., Fanfani, Valentina, Fissel, Laura M., Galitzki, Nicholas B., Gao, Jiansong, Gordon, Samuel, Groppi, Christopher E., Hilton, Gene C., Hubmayr, Johannes, Klein, Jeffrey, Li, Dale, Lowe, Ian, Lourie, Nathan P., Mckinney, Christopher, Mani, Hamdi, Mauskopf, Philip D., Nati, Federico, Novak, Giles, Pisano, Giampaolo, Romualdez, Javier L., Sinclair, Adrian K., Soler, Juan D., Tucker, Carole, Ullom, Joel, Visser, Michael, Wheeler, Caleb H., and Williams, Paul A.

Abstract

The Next Generation Balloon-Borne Large Aperture Submillimeter Telescope (BLAST-TNG) was a unique instrument for characterizing the polarized submillimeter sky at high-angular resolution. BLAST-TNG flew from the Long Duration Balloon Facility in Antarctica in January 2020. Despite the short flight duration, the instrument worked very well and is providing significant information about each subsystem that will be invaluable for future balloon missions. In this contribution, we discuss the performance of telescope and gondola.

Published
2020

42. Microwave Multiplexing on the Keck Array

Author

Cukierman, A., primary, Ahmed, Z., additional, Henderson, S., additional, Young, E., additional, Yu, C., additional, Barkats, D., additional, Brown, D., additional, Chaudhuri, S., additional, Cornelison, J., additional, D’Ewart, J. M., additional, Dierickx, M., additional, Dober, B. J., additional, Dusatko, J., additional, Fatigoni, S., additional, Filippini, J. P., additional, Frisch, J. C., additional, Haller, G., additional, Halpern, M., additional, Hilton, G. C., additional, Hubmayr, J., additional, Irwin, K. D., additional, Karkare, K. S., additional, Karpel, E., additional, Kernasovskiy, S. A., additional, Kovac, J. M., additional, Kovacs, A., additional, Kuenstner, S. E., additional, Kuo, C. L., additional, Li, D., additional, Mates, J. A. B., additional, Smith, S., additional, St. Germaine, T., additional, Ullom, J. N., additional, Vale, L. R., additional, Van Winkle, D. D., additional, Vasquez, J., additional, Willmert, J., additional, Zeng, L., additional, Ade, P. A. R., additional, Amiri, M., additional, Basu Thakur, R., additional, Bischoff, C. A., additional, Bock, J. J., additional, Boenish, H., additional, Bullock, E., additional, Buza, V., additional, Cheshire, J., additional, Connors, J., additional, Crumrine, M., additional, Duband, L., additional, Hall, G., additional, Harrison, S., additional, Hildebrandt, S. R., additional, Hui, H., additional, Kang, J., additional, Kefeli, S., additional, Lau, K., additional, Megerian, K. G., additional, Moncelsi, L., additional, Namikawa, T., additional, Nguyen, H. T., additional, O’Brient, R., additional, Palladino, S., additional, Pryke, C., additional, Racine, B., additional, Reintsema, C. D., additional, Richter, S., additional, Schillaci, A., additional, Schwarz, R., additional, Sheehy, C. D., additional, Soliman, A., additional, Steinbach, B., additional, Sudiwala, R. V., additional, Thompson, K. L., additional, Tucker, C., additional, Turner, A. D., additional, Umiltà, C., additional, Vieregg, A. G., additional, Wandui, A., additional, Weber, A. C., additional, Wiebe, D. V., additional, Wu, W. L. K., additional, Yang, H., additional, Yoon, K. W., additional, and Zhang, C., additional

Published
2019
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43. Crosstalk in microwave SQUID multiplexers

Author

Mates, J. A. B., primary, Becker, D. T., additional, Bennett, D. A., additional, Dober, B. J., additional, Gard, J. D., additional, Hilton, G. C., additional, Swetz, D. S., additional, Vale, L. R., additional, and Ullom, J. N., additional

Published
2019
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44. SLAC Microresonator Radio Frequency (SMuRF) Electronics for Read Out of Frequency-Division-Multiplexed Cryogenic Sensors

Author

Kernasovskiy, S. A., primary, Kuenstner, S. E., additional, Karpel, E., additional, Ahmed, Z., additional, Van Winkle, D. D., additional, Smith, S., additional, Dusatko, J., additional, Frisch, J. C., additional, Chaudhuri, S., additional, Cho, H. M., additional, Dober, B. J., additional, Henderson, S. W., additional, Hilton, G. C., additional, Hubmayr, J., additional, Irwin, K. D., additional, Kuo, C. L., additional, Li, D., additional, Mates, J. A. B., additional, Nasr, M., additional, Tantawi, S., additional, Ullom, J., additional, Vale, L., additional, and Young, B., additional

Published
2018
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46. Publisher's Note: “Microwave SQUID multiplexer demonstration for cosmic microwave background imagers” [Appl. Phys. Lett. 111, 243510 (2017)]

Author

Dober, B., primary, Becker, D. T., additional, Bennett, D. A., additional, Bryan, S. A., additional, Duff, S. M., additional, Gard, J. D., additional, Hays-Wehle, J. P., additional, Hilton, G. C., additional, Hubmayr, J., additional, Mates, J. A. B., additional, Reintsema, C. D., additional, Vale, L. R., additional, and Ullom, J. N., additional

Published
2018
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47. Superconducting micro-resonator arrays with ideal frequency spacing

Author

Liu, X., primary, Guo, W., additional, Wang, Y., additional, Dai, M., additional, Wei, L. F., additional, Dober, B., additional, McKenney, C. M., additional, Hilton, G. C., additional, Hubmayr, J., additional, Austermann, J. E., additional, Ullom, J. N., additional, Gao, J., additional, and Vissers, M. R., additional

Published
2017
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50. The design of the Ali CMB Polarization Telescope receiver

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Salatino, M., Austermann, J., Thompson, K. L., Ade, P. A. R., Bai, X., Beall, J. A., Becker, D. T., Cai, Y., Chang, Z., Chen, D., Connors, J., Chen, P., Dober, B., Delabrouille, J., Duff, S. M., Gao, G., Givhan, R. C., Ghosh, S., Hilton, G., Hu, B., Hubmayr, J., Karpel, E., Kuo, C.-L., Li, H., Li, M., Li, S.-Y., Li, X., Link, M., Li, Y., Liu, H., Liu, L., Liu, Y., Lu, F., Lukas, T., Lu, X., Mates, J. A. B., Mathewson, J., Mauskopf, P., Meinke, J., Montana-Lopez, J., Moore, J., Shi, J., Sinclair, A. K., Stephenson, R., Sun, W., Tseng, Y.‐H., Tucker, C., Ullom, J., Vale, L., van Lanen, J., Vissers, M., Walker, S., Wang, B., Wang, G., Wang, J., Weeks, E., Wu, Di, Wu, Y.-H., Xia, J., Xu, H., Yao, J., Yao, Y., Yoon, K. W., Yue, B., Zhai, H., Zhang, A., Zhang, Laiyu, Zhang, Le, Zhang, P., Zhang, T., Zhang, Xinmin, Zhang, Yifei, Zhang, Yongjie, Zhao, G.-B., and Zhao, W.

Published
2020
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