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1. Design and Performance of a 30/40 GHz Diplexed Focal Plane for the BICEP Array

Author

Corwin Shiu, Ahmed Soliman, Roger O’Brient, Bryan Steinbach, James J. Bock, Clifford F. Frez, William C. Jones, Krikor. G. Megerian, Lorenzo Moncelsi, Alessandro Schillaci, Anthony D. Turner, Alexis C. Weber, Cheng Zhang, and Silvia Zhang

Subjects
Astronomical instrumentation, CMBR detectors, Polarimeters, Astrophysics, QB460-466
Abstract

We demonstrate a wideband diplexed focal plane suitable for observing low-frequency foregrounds that are important for cosmic microwave background polarimetry. The antenna elements are composed of slotted bowtie antennas with 60% bandwidth that can be partitioned into two bands. Each pixel is composed of two interleaved 12 × 12 pairs of linearly polarized antenna elements forming a phased array, designed to synthesize a symmetric beam with no need for focusing optics. The signal from each antenna element is captured in-phase and uniformly weighted by a microstrip summing tree. The antenna signal is diplexed into two bands through the use of two complementary, six-pole Butterworth filters. This filter architecture ensures a contiguous impedance match at all frequencies, and thereby achieves minimal reflection loss between both bands. Subsequently, out-of-band rejection is increased with a bandpass filter and the signal is then deposited on a transition-edge sensor bolometer island. We demonstrate the performance of this focal plane with two distinct bands, 30 and 40 GHz, each with a bandwidth of ∼20 and 15 GHz, respectively. The unequal bandwidths between the two bands are caused by an unintentional shift in diplexer frequency from its design values. The end-to-end optical efficiency of these detectors is relatively modest, at 20%–30%, with an efficiency loss due to an unknown impedance mismatch in the summing tree. Far-field beam maps show good optical characteristics, with edge pixels having no more than ∼5% ellipticity and ∼10%–15% peak-to-peak differences for A–B polarization pairs.

Published
2024
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2. Improved polarization calibration of the BICEP3 CMB polarimeter at the South Pole

Author

James Cornelison, Clara Verges, P A. Ade, Zeeshan Ahmed, Mandana Amiri, Denis Barkats, Ritoban Basu Thakur, Dominic Beck, Colin A. Bischoff, James J. Bock, Victor Buza, James R. Cheshire, Jake Connors, Michael Crumrine, Ari Jozef Cukierman, Edward Denison, Marion Dierickx, Lionel Duband, Miranda Eiben, Sofia Fatigoni, Jeff P. Filippini, Christos Giannakopoulos, Neil Goeckner-Wald, David C. Goldfinger, James A. Grayson, Paul Grimes, Grantland Hall, George Halal, Mark Halpern, Emma Hand, Sam A. Harrison, Shawn Henderson, Sergi Hildebrandt, Gene C. Hilton, Johannes Hubmayr, Howard Hui, Kent D. Irwin, Jae Hwan Kang, Kirit S. Karkare, Sinan Kefeli, John Kovac, Chao-Lin Kuo, King Lau, Erik M. Leitch, Amber Lennox, Tongtian Liu, Karsten Look, K(oko). G. Megerian, Lorenzo Minutolo, Lorenzo Moncelsi, Yuka Nakato, Toshiya Namikawa, H. T. Nguyen, Roger O'brient, Steven Palladino, Matthew Petroff, Thomas Prouve, Clement Pryke, Benjamin Racine, Carl D. Reintsema, Maria Salatino, Alessandro Schillaci, Benjamin Schmitt, Baibhav Singari, Ahmed Soliman, Tyler St Germaine, Bryan Steinbach, Rashmi Sudiwala, Keith L. Thompson, Calvin Tsai, Carole Tucker, Anthony D. Turner, Caterina Umiltà, Abigail G. Vieregg, Albert Wandui, Alexis C. Weber, Don Wiebe, Justin Willmert, Wai Ling K. Wu, Hung-I Yang, Ki Won Yoon, Edward Young, Cyndia Yu, Lingzhen Zeng, Cheng Zhang, Silvia Zhang, Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Polarization, Cosmic Microwave Background, Calibration, FOS: Physical sciences, Cosmic Birefringence, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The BICEP3 Polarimeter is a small aperture, refracting telescope, dedicated to the observation of the Cosmic Microwave Background (CMB) at 95GHz. It is designed to target degree angular scale polarization patterns, in particular the very-much-sought-after primordial B-mode signal, which is a unique signature of cosmic inflation. The polarized signal from the sky is reconstructed by differencing co-localized, orthogonally polarized superconducting Transition Edge Sensor (TES) bolometers. In this work, we present absolute measurements of the polarization response of the detectors for more than $\sim 800$ functioning detector pairs of the BICEP3 experiment, out of a total of $\sim 1000$. We use a specifically designed Rotating Polarized Source (RPS) to measure the polarization response at multiple source and telescope boresight rotation angles, to fully map the response over 360 degrees. We present here polarization properties extracted from on-site calibration data taken in January 2022. A similar calibration campaign was performed in 2018, but we found that our constraint was dominated by systematics on the level of $\sim0.5^\circ$. After a number of improvements to the calibration set-up, we are now able to report a significantly lower level of systematic contamination. In the future, such precise measurements will be used to constrain physics beyond the standard cosmological model, namely cosmic birefringence., Submitted to: SPIE Astronomical Telescopes + Instrumentation (AS22)

Published
2022
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3. Design and performance of wide-band corrugated walls for the BICEP Array detector modules at 30/40 GHz

Author

Jakob Vanzyl, Caterina Umiltà, Anthony D. Turner, Carole Tucker, James E. Tolan, Keith L. Thompson, Grant P. Teply, Rashmi Sudiwala, Bryan Steinbach, Zachary K. Staniszewski, Tyler St Germaine, Chris D. Sheehy, Grantland Hall, Lionel Duband, Marion Dierickx, Michael Crumrine, Brendan Crill, James Cornelison, Jake Connors, Victor Buza, Immanuel Buder, Justus A. Brevik, Rachel Bowens-Rubin, Denis Barkats, Kate D. Alexander, Randol Aikin, Zeeshan Ahmed, P. A. R. Ade, Cheng Zhang, Ki Won Yoon, Hung-I. Yang, Wai Ling K. Wu, Chin Lin Wong, Justin Willmert, Don Wiebe, Alexis C. Weber, Albert Wandui, Abigail G. Vieregg, Robert Schwarz, Alessandro Schillaci, Steffen Richter, Benjamin Racine, Clement Pryke, Stephen Palladino, R. Walt Ogburn IV, Roger O'brient, H. T. Nguyen, C. B. Netterfield, Toshiya Namikawa, Lorenzo Moncelsi, K(oko). G. Megerian, Martin Lueker, Erik M. Leitch, King Lau, Nicole Larson, Chao-Lin Kuo, J. M. Kovac, Sarah A. Kernasovskiy, Sinan Kefeli, Brian G. Keating, Jonathan Kaufman, Ethan Karpel, Kirit S. Karkare, Jae Hwan Kang, Kent D. Irwin, Howard Hui, Gene C. Hilton, Sergi Hildebrandt, Sam A. Harrison, Mark Halpern, James A. Grayson, Stefan Fliescher, Jeff P. Filippini, Cora Dvorkin, Eric Bullock, James J. Bock, Colin A. Bischoff, Steve J. Benton, Ahmed Soliman, Zmuidzinas, Jonas, and Gao, Jian-Rong

Subjects
Physics, Pixel, business.industry, Cosmic microwave background, Bandwidth (signal processing), Detector, Beam steering, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 01 natural sciences, Optics, 0103 physical sciences, 010306 general physics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Beam (structure), Leakage (electronics)
Abstract

BICEP Array is a degree-scale Cosmic Microwave Background (CMB) experiment that will search for primordial B-mode polarization while constraining Galactic foregrounds. BICEP Array will be comprised of four receivers to cover a broad frequency range with channels at 30/40, 95, 150 and 220/270 GHz. The first low-frequency receiver will map synchrotron emission at 30 and 40 GHz and will deploy to the South Pole at the end of 2019. In this paper, we give an overview of the BICEP Array science and instrument, with a focus on the detector module. We designed corrugations in the metal frame of the module to suppress unwanted interactions with the antenna-coupled detectors that would otherwise deform the beams of edge pixels. This design reduces the residual beam systematics and temperature-to-polarization leakage due to beam steering and shape mismatch between polarized beam pairs. We report on the simulated performance of single- and wide-band corrugations designed to minimize these effects. Our optimized design alleviates beam differential ellipticity caused by the metal frame to about 7% over 57% bandwidth (25 to 45 GHz), which is close to the level due the bare antenna itself without a metal frame. Initial laboratory measurements are also presented., 12 pages and 14 figures

Published
2018

4. 2017 upgrade and performance of BICEP3: a 95GHz refracting telescope for degree-scale CMB polarization

Author

Jae Hwan Kang, Cheng Zhang, Ki Won Yoon, Hung-I Yang, Wai Ling K. Wu, Chin Lin Wong, Justin Willmert, Don Wiebe, Alexis C. Weber, Albert Wandui, Abigail G. Vieregg, Caterina Umiltà, Anthony D. Turner, Carole Tucker, James E. Tolan, Keith L. Thompson, Grant P. Teply, Rashmi Sudiwala, Bryan Steinbach, Zachary K. Staniszewski, Tyler St Germaine, Ahmed Soliman, Chris D. Sheehy, Robert Schwarz, Alessandro Schillaci, Steffen Richter, Benjamin Racine, Clement Pryke, Stephen Palladino, R. W. Ogburn IV, Roger O'brient, Hien T. Nguyen, C. B. Netterfield, Toshiya Namikawa, Lorenzo Moncelsi, Koko G. Megerian, Martin Lueker, Erik M. Leitch, King Lau, Nicole Larsen, Chao-Lin Kuo, John M. Kovac, Sarah A. Kernasovskiy, Sinan Kefeli, Brian G. Keating, Jonathan Kaufman, Ethan Karpel, Kirit S. Karkare, Kent D. Irwin, Howard Hui, Gene C. Hilton, Sergi Hildebrandt, Sam A. Harrison, Mark Halpern, Grantland Hall, James A. Grayson, Stefan Fliescher, Jeff P. Filippini, Cora Dvorkin, Lionel Duband, Marion Dierickx, Michael Crumrine, Brendan Crill, James Cornelison, Jake Conners, Victor Buza, Eric Bullock, Immanuel Buder, Justus A. Brevik, Rachel Bowens-Rubin, Hans Boenish, James J. Bock, Colin A. Bischoff, Steve J. Benton, Denis Barkats, Kate D. Alexander, Randol Aikin, Zeeshan Ahmed, Peter A. Ade, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Zmuidzinas, Jonas, and Gao, Jian-Rong

Subjects
noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), detector: performance, Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, BICEP3, law.invention, cosmic background radiation: B-mode, Optics, bolometer, law, Polarization, 0103 physical sciences, Cosmic Microwave Background, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, Physics, Gravitational Waves, Gravitational wave, business.industry, beam: width, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, Polarization (waves), detector: upgrade, Inflation, optics, Cardinal point, Upgrade, Refracting telescope, Keck Array, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

BICEP3 is a 520mm aperture on-axis refracting telescope observing the polarization of the cosmic microwave background (CMB) at 95GHz in search of the B-mode signal originating from inflationary gravitational waves. BICEP3's focal plane is populated with modularized tiles of antenna-coupled transition edge sensor (TES) bolometers. BICEP3 was deployed to the South Pole during 2014-15 austral summer and has been operational since. During the 2016-17 austral summer, we implemented changes to optical elements that lead to better noise performance. We discuss this upgrade and show the performance of BICEP3 at its full mapping speed from the 2017 and 2018 observing seasons. BICEP3 achieves an order-of-magnitude improvement in mapping speed compared to a Keck 95GHz receiver. We demonstrate $6.6\mu K\sqrt{s}$ noise performance of the BICEP3 receiver., Comment: 12 pages, 9 figures, Published in Proc. SPIE. Presented at SPIE Astronomical Telescopes and Instrumentation Conference 10708: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI, June 2018

Published
2018
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5. A Bulk-Micromachined Bistable Relay With U-Shaped Thermal Actuators.

Author

Jin Qiu, Lang, Jeffrey H., Slocum, Alexander H., and Alexis C. Weber

Subjects
AUTOMATIC control systems, FINITE element method, CONTROL theory (Engineering), MICROELECTROMECHANICAL systems, ELECTROMECHANICAL devices, MECHATRONICS
Abstract

This paper reports a deep-reactive ion etching (DRIE)-th rough-etched laterally bistable MEMS relay for power applications, with a primary emphasis on the design and modeling of its U-shaped transient thermal actuators, and a secondary emphasis on the design and fabrication of its contact element. In this relay, a contact crossbar is carried by a curved-beam bistable mechanism [1], which is toggled by transient U-shaped thermal actuators with their hot beam adiabaticly heated by electrical pulses. Each U-shaped thermal actuator comprises uniform-thickness hot and cold beams with a gap between them so they bend differently. This paper develops both a basic model and a complete model for the actuator that are verified by Finite Element Analysis and serve as effective design tools. The DRIE process creates nonideal etched surfaces, which pose challenges for good relay contacts. Both contact design and process development are discussed to help alleviate this problem. The fabricated relay exhibits a minimum total on-state resistance of 60 mΩ, and a maximum current carrying capacity of 3 A. It switches with a I ms actuation pulse, and a maximum 5 Hz repetition rate. [ABSTRACT FROM AUTHOR]

Published
2005
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6. Thermal testing for cryogenic CMB instrument optical design

Author

David C. Goldfinger, Peter A. R. Ade, Zeeshan Ahmed, Mandana Amiri, Denis Barkats, Ritoban Basu Thakur, Dominic Beck, Colin A. Bischoff, James J. Bock, Victor Buza, James R. Cheshire, Jake Connors, James Cornelison, Michael Crumrine, Ari J. Cukierman, Edward V. Denison, Marion I. Dierickx, Lionel Duband, Miranda Eiben, Sofia Fatigoni, Jeff P. Filippini, Christos Giannakopoulos, Neil Goeckner-Wald, James A. Grayson, Paul K. Grimes, Grantland Hall, George Halal, Mark Halpern, Emma Hand, Sam A. Harrison, Shawn Henderson, Sergi R. Hildebrandt, Gene C. Hilton, Johannes Hubmayr, Howard Hui, Kent D. Irwin, Jae Hwan Kang, Kirit S. Karkare, Sinan Kefeli, John M. Kovac, Chao-Lin Kuo, King Lau, Erik M. Leitch, Amber Lennox, Tongtian Liu, Krikor G. Megerian, Lorenzo Minutolo, Lorenzo Moncelsi, Yuka Nakato, Toshiya Namikawa, Hien T. Nguyen, Roger O'Brient, Steven M. Palladino, Matthew Petroff, Thomas Prouvé, Clement L. Pryke, Benjamin Racine, Carl D. Reintsema, Maria Salatino, Alessandro Schillaci, Benjamin L. Schmitt, Baibhav Singari, Ahmed Soliman, Amanda G. Smith, Tyler St. Germaine, Bryan Steinbach, Rashmi V. Sudiwala, Keith L. Thompson, Calvin Tsai, Carole E. Tucker, Anthony D. Turner, Caterina Umiltà, Clara Verges, Abigail G. Vieregg, Albert K. Wandui, Alexis C. Weber, Don V. Wiebe, Justin Willmert, Wai Ling K. Wu, Hung-I Yang, Ki Won Yoon, Edward Young, Cyndia Yu, Lingzhen Zeng, Cheng Zhang, Silvia Zhang, Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
Thermal Testing, Cryogenics, Polarization, Cosmic Microwave Background, FOS: Physical sciences, BICEP Array, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Observations of the Cosmic Microwave Background rely on cryogenic instrumentation with cold detectors, readout, and optics providing the low noise performance and instrumental stability required to make more sensitive measurements. It is therefore critical to optimize all aspects of the cryogenic design to achieve the necessary performance, with low temperature components and acceptable system cooling requirements. In particular, we will focus on our use of thermal filters and cold optics, which reduce the thermal load passed along to the cryogenic stages. To test their performance, we have made a series of in situ measurements while integrating the third receiver for the BICEP Array telescope. In addition to characterizing the behavior of this receiver, these measurements continue to refine the models that are being used to inform design choices being made for future instruments., Comment: 9 pages, 8 figures, Proceedings of SPIE 2022

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