Lorenzo Minutolo, Bryan Steinbach, Albert Wandui, Roger O'Brient
We have developed a flexible radio-frequency readout system suitable for a variety of superconducting detectors commonly used in millimeter and submillimeter astrophysics, including Kinetic Inductance detectors (KIDs), Thermal KID bolometers (TKIDs), and Quantum Capacitance Detectors (QCDs). Our system avoids custom FPGA-based readouts and instead uses commercially available software radio hardware for ADC/DAC and a GPU to handle real time signal processing. Because this system is written in common C++/CUDA, the range of different algorithms that can be quickly implemented make it suitable for the readout of many others cryogenic detectors and for the testing of different and possibly more effective data acquisition schemes.
Roger OBrient, Peter Ade, Kam Arnold, Jennifer Edwards, Greg Engargiola, William L Holzapfel, Adrian T Lee, Michael J Myers, Erin Quealy, Gabriel Rebeiz, Paul Richards, Aritoki Suzuki
We describe the design, fabrication, and testing of a broadband log-periodic antenna coupled to multiple cryogenic bolometers. This detector architecture, optimized here for astrophysical observations, simultaneously receives two linear polarizations with two octaves of bandwidth at millimeter wavelengths. The broad bandwidth signal received by the antenna is divided into sub-bands with integrated in-line frequency-selective filters. We demonstrate two such filter banks: a diplexer with two sub-bands and a log-periodic channelizer with seven contiguous sub-bands. These detectors have receiver efficiencies of 20-40% and percent level polarization isolation. Superconducting transition-edge sensor bolometers detect the power in each sub-band and polarization. We demonstrate circularly symmetric beam patterns, high polarization isolation, accurately positioned bands, and high optical efficiency. The pixel design is applicable to astronomical observations of intensity and polarization at millimeter through sub-millimeter wavelengths. As compared with an imaging array of pixels measuring only one band, simultaneous measurements of multiple bands in each pixel has the potential to result in a higher signal-to-noise measurement while also providing spectral information. This development facilitates compact systems with high mapping speeds for observations that require information in multiple frequency bands.
R. O'Brient, P. A. R. Ade, Z. Ahmed, R. W. Aikin, M. Amiri, S. Benton, C. Bischoff, J. J. Bock, J. A. Bonetti, J. A. Brevik, B. Burger, G. Davis, P. Day, C. D. Dowell, L. Duband, J. P. Filippini, S. Fliescher, S. R. Golwala, J. Grayson, M. Halpern, M. Hasselfield, G. Hilton, V. V. Hristov, H. Hui, K. Irwin, S. Kernasovskiy, J. M. Kovac, C. L. Kuo, E. Leitch, M. Lueker, K. Megerian, L. Moncelsi, C. B. Netterfield, H. T. Nguyen, R. W. Ogburn, C. L. Pryke, C. Reintsema, J. E. Ruhl, M. C. Runyan, R. Schwarz, C. D. Sheehy, Z. Staniszewski, R. Sudiwala, G. Teply, J. E. Tolan, A. D. Turner, R. S. Tucker, A. Vieregg, D. V. Wiebe, P. Wilson, C. L. Wong, W. L. K. Wu, K. W. Yoon
Between the BICEP2 and Keck Array experiments, we have deployed over 1500 dual polarized antenna coupled bolometers to map the Cosmic Microwave Background's polarization. We have been able to rapidly deploy these detectors because they are completely planar with an integrated phased-array antenna. Through our experience in these experiments, we have learned of several challenges with this technology- specifically the beam synthesis in the antenna- and in this paper we report on how we have modified our designs to mitigate these challenges. In particular, we discus differential steering errors between the polarization pairs' beam centroids due to microstrip cross talk and gradients of penetration depth in the niobium thin films of our millimeter wave circuits. We also discuss how we have suppressed side lobe response with a Gaussian taper of our antenna illumination pattern. These improvements will be used in Spider, Polar-1, and this season's retrofit of Keck Array.
P. A. R. Ade, R. W. Aikin, M. Amiri, D. Barkats, S. J. Benton, C. A. Bischoff, J. J. Bock, J. A. Bonetti, J. A. Brevik, I. Buder, E. Bullock, G. Chattopadhyay, G. Davis, P. K. Day, C. D. Dowell, L. Duband, J. P. Filippini, S. Fliescher, S. R. Golwala, M. Halpern, M. Hasselfield, S. R. Hildebrandt, G. C. Hilton, V. Hristov, H. Hui, K. D. Irwin, W. C. Jones, K. S. Karkare, J. P. Kaufman, B. G. Keating, S. Kefeli, S. A. Kernasovskiy, J. M. Kovac, C. L. Kuo, H. G. Leduc, E. M. Leitch, N. Llombart, M. Lueker, P. Mason, K. Megerian, L. Moncelsi, C. B. Netterfield, H. T. Nguyen, R. O'Brient, R. W. Ogburn, A. Orlando, C. Pryke, A. S. Rahlin, C. D. Reintsema, S. Richter, M. C. Runyan, R. Schwarz, C. D. Sheehy, Z. K. Staniszewski, R. V. Sudiwala, G. P. Teply, J. E. Tolan, A. Trangsrud, R. S. Tucker, A. D. Turner, A. G. Vieregg, A. Weber, D. V. Wiebe, P. Wilson, C. L. Wong, K. W. Yoon, J. Zmuidzinas
We have developed antenna-coupled transition-edge sensor (TES) bolometers for a wide range of cosmic microwave background (CMB) polarimetry experiments, including BICEP2, Keck Array, and the balloon borne SPIDER. These detectors have reached maturity and this paper reports on their design principles, overall performance, and key challenges associated with design and production. Our detector arrays repeatedly produce spectral bands with 20%-30% bandwidth at 95, 150, or 220~GHz. The integrated antenna arrays synthesize symmetric co-aligned beams with controlled side-lobe levels. Cross-polarized response on boresight is typically ~0.5%, consistent with cross-talk in our multiplexed readout system. End-to-end optical efficiencies in our cameras are routinely 35% or higher, with per detector sensitivities of NET~300 uKrts. Thanks to the scalability of this design, we have deployed 2560 detectors as 1280 matched pairs in Keck Array with a combined instantaneous sensitivity of ~9 uKrts, as measured directly from CMB maps in the 2013 season. Similar arrays have recently flown in the SPIDER instrument, and development of this technology is ongoing.
Marion Dierickx, P. A. R. Ade, Zeeshan Ahmed, Mandana Amiri, Denis Barkats, Ritoban Basu Thakur, Colin A. Bischoff, Dominic Beck, James J. Bock, Victor Buza, James R. Cheshire, Jake Connors, James Cornelison, Michael Crumrine, Ari Jozef Cukierman, Edward Denison, Lionel Duband, Miranda Eiben, Sofia Fatigoni, Jeff P. Filippini, Christos Giannakopoulos, Neil Goeckner-Wald, David 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, J. M. Kovac, Chao-Lin Kuo, King Lau, Erik M. Leitch, Amber Lennox, K, . G. Megerian, Lorenzo Minutolo, Lorenzo Moncelsi, Yuka Nakato, Toshiya Namikawa, H. T. Nguyen, Roger O'brient, Steven Palladino, Matthew Petroff, Nathan Precup, Thomas Prouve, Clement Pryke, Benjamin Racine, Carl D. Reintsema, Destiny Santalucia, Alessandro Schillaci, Benjamin Schmitt, Baibhav Singari, Ahmed Soliman, Tyler St Germaine, Bryan Steinbach, Rashmi Sudiwala, Keith L. Thompson, Carole Tucker, Anthony D. Turner, Caterina Umiltà, Clara Verges, 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
Nov 29, 2021·astro-ph.IM·PDF The BICEP/Keck series of experiments target the Cosmic Microwave Background at degree-scale resolution from the South Pole. Over the next few years, the "Stage-3" BICEP Array (BA) telescope will improve the program's frequency coverage and sensitivity to primordial B-mode polarization by an order of magnitude. The first receiver in the array, BA1, began observing at 30/40 GHz in early 2020. The next two receivers, BA2 and BA3, are currently being assembled and will map the southern sky at frequencies ranging from 95 GHz to 150 GHz. Common to all BA receivers is a refractive, on-axis, cryogenic optical design that focuses microwave radiation onto a focal plane populated with antenna-coupled bolometers. High-performance antireflective coatings up to 760 mm in aperture are needed for each element in the optical chain, and must withstand repeated thermal cycles down to 4 K. Here we present the design and fabrication of the 30/40 GHz anti-reflection coatings for the recently deployed BA1 receiver, then discuss laboratory measurements of their reflectance. We review the lamination method for these single- and dual-layer plastic coatings with indices matched to various polyethylene, nylon and alumina optics. We also describe ongoing efforts to optimize coatings for the next BA cryostats, which may inform technological choices for future Small-Aperture Telescopes of the CMB "Stage 4" experiment.
Karl Young, Marcelo Alvarez, Nicholas Battaglia, Jamie Bock, Julian Borrill, David Chuss, Brendan Crill, Jacques Delabrouille, Mark Devlin, Laura Fissel, Raphael Flauger, Daniel Green, Kris Gorski, Shaul Hanany, Richard Hills, Johannes Hubmayr, Bradley Johnson, Bill Jones, Lloyd Knox, Al Kogut, Charles Lawrence, Tomotake Matsumura, Jim McGuire, Jeff McMahon, Roger O'Brient, Clem Pryke, Brian M. Sutin, Xin Zhi Tan, Amy Trangsrud, Qi Wen, Gianfranco de Zotti
The Probe of Inflation and Cosmic Origins (PICO) is a probe-class mission concept currently under study by NASA. PICO will probe the physics of the Big Bang and the energy scale of inflation, constrain the sum of neutrino masses, measure the growth of structures in the universe, and constrain its reionization history by making full sky maps of the cosmic microwave background with sensitivity 80 times higher than the Planck space mission. With bands at 21-799 GHz and arcmin resolution at the highest frequencies, PICO will make polarization maps of Galactic synchrotron and dust emission to observe the role of magnetic fields in Milky Way's evolution and star formation. We discuss PICO's optical system, focal plane, and give current best case noise estimates. The optical design is a two-reflector optimized open-Dragone design with a cold aperture stop. It gives a diffraction limited field of view (DLFOV) with throughput of 910 square cm sr at 21 GHz. The large 82 square degree DLFOV hosts 12,996 transition edge sensor bolometers distributed in 21 frequency bands and maintained at 0.1 K. We use focal plane technologies that are currently implemented on operating CMB instruments including three-color multi-chroic pixels and multiplexed readouts. To our knowledge, this is the first use of an open-Dragone design for mm-wave astrophysical observations, and the only monolithic CMB instrument to have such a broad frequency coverage. With current best case estimate polarization depth of 0.65 microK(CMB}-arcmin over the entire sky, PICO is the most sensitive CMB instrument designed to date.
Brian Sutin, Marcelo Alvarez, Nicholas Battaglia, Jamie Bock, Matteo Bonato, Julian Borrill, David T. Chuss, Joelle Cooperrider, Brendan Crill, Jacques Delabrouille, Mark Devlin, Thomas Essinger-Hileman, Laura Fissel, Raphael Flauger, Krzysztof Gorski, Daniel Green, Shaul Hanany, Johannes Hubmayr, Bradley Johnson, William C. Jones, Lloyd Knox, Alan Kogut, Charles Lawrence, Jeff McMahon, Tomotake Matsumura, Mattia Negrello, Roger O'Brient, Christopher Paine, Clement Pryke, Peter Shirron, Amy Trangsrud, Qi Wen, Karl Young, Gianfranco de Zotti
The Probe of Inflation and Cosmic Origins (PICO) is a NASA-funded study of a Probe-class mission concept. The top-level science objectives are to probe the physics of the Big Bang by measuring or constraining the energy scale of inflation, probe fundamental physics by measuring the number of light particles in the Universe and the sum of neutrino masses, to measure the reionization history of the Universe, and to understand the mechanisms driving the cosmic star formation history, and the physics of the galactic magnetic field. PICO would have multiple frequency bands between 21 and 799 GHz, and would survey the entire sky, producing maps of the polarization of the cosmic microwave background radiation, of galactic dust, of synchrotron radiation, and of various populations of point sources. Several instrument configurations, optical systems, cooling architectures, and detector and readout technologies have been and continue to be considered in the development of the mission concept. We will present a snapshot of the baseline mission concept currently under development.
Aritoki Suzuki, Kam Arnold, Jennifer Edwards, Greg Engargiola, Adnan Ghribi, William Holzapfel, Adrian T. Lee, Xiao Fan Meng, Michael J. Myers, Roger O'Brient, Erin Quealy, Gabriel Rebeiz, Paul Richards, Darin Rosen, Praween Siritanasak
Oct 31, 2012·astro-ph.IM·PDF We are developing multi-chroic antenna-coupled TES detectors for CMB polarimetry. Multi-chroic detectors increase the mapping speed per focal plane area and provide greater discrimination of polarized galactic foregrounds with no increase in weight or cryogenic cost. In each pixel, a silicon lens-coupled dual polarized sinuous antenna collects light over a two-octave frequency band. The antenna couples the broadband millimeter wave signal into microstrip transmission lines, and on-chip filter banks split the broadband signal into several frequency bands. Separate TES bolometers detect the power in each frequency band and linear polarization. We will describe the design and performance of these devices and present optical data taken with prototype pixels. Our measurements show beams with percent level ellipticity, percent level cross-polarization leakage, and partitioned bands using banks of 2, 3, and 7 filters. We will also describe the development of broadband anti-reflection coatings for the high dielectric constant lens. The broadband anti-reflection coating has approximately 100 percent bandwidth and no detectable loss at cryogenic temperature. Finally, we will describe an upgrade for the POLARBEAR CMB experiment and installation for the LITEBird CMB satellite experiment both of which have focal planes with kilo-pixel of these detectors to achieve unprecedented mapping speed.
Albert Wandui, Jamie Bock, Clifford Frez, Matthew Hollister, Lorenzo Minutolo, Hien Nguyen, Bryan Steinbach, Anthony Turner, Jonas Zmuidzinas, Roger O'Brient
Thermal Kinetic Inductance Detectors (TKIDs) combine the excellent noise performance of traditional bolometers with a radio frequency multiplexing architecture that enables the large detector counts needed for the next generation of millimeter-wave instruments. In this paper, we first discuss the expected noise sources in TKIDs and derive the limits where the phonon noise contribution dominates over the other detector noise terms: generation-recombination, amplifier, and two-level system (TLS) noise. Second, we characterize aluminum TKIDs in a dark environment. We present measurements of TKID resonators with quality factors of about $10^5$ at 80 mK. We also discuss the bolometer thermal conductance, heat capacity, and time constants. These were measured by the use of a resistor on the thermal island to excite the bolometers. These dark aluminum TKIDs demonstrate a noise equivalent power NEP = $2 \times 10^{-17} \mathrm{W}/\mathrm{\sqrt{Hz}} $, with a $1/f$ knee at 0.1 Hz, which provides background noise limited performance for ground-based telescopes observing at 150 GHz.
Attila Kovács, Peter S. Barry, Charles M. Bradford, Goutam Chattopadhyay, Peter Day, Simon Doyle, Steve Hailey-Dunsheath, Matthew Hollister, Christopher McKenney, Henry G. LeDuc, Nuria Llombart, Daniel P. Marrone, Philip Mauskopf, Roger O'Brient, Stephen Padin, Loren J. Swenson, Jonas Zmuidzinas
SuperSpec is a pathfinder for future lithographic spectrometer cameras, which promise to energize extra-galactic astrophysics at (sub)millimeter wavelengths: delivering 200--500 km/s spectral velocity resolution over an octave bandwidth for every pixel in a telescope's field of view. We present circuit simulations that prove the concept, which enables complete millimeter-band spectrometer devices in just a few square-millimeter footprint. We evaluate both single-stage and two-stage channelizing filter designs, which separate channels into an array of broad-band detectors, such as bolometers or kinetic inductance detector (KID) devices. We discuss to what degree losses (by radiation or by absorption in the dielectric) and fabrication tolerances affect the resolution or performance of such devices, and what steps we can take to mitigate the degradation. Such design studies help us formulate critical requirements on the materials and fabrication process, and help understand what practical limits currently exist to the capabilities these devices can deliver today or over the next few years.
Erik Shirokoff, Peter S. Barry, Charles M. Bradford, Goutam Chattopadhyay, Peter Day, Simon Doyle, Steve Hailey-Dunsheath, Matthew I. Hollister, Attila Kovács, Christopher McKenney, Henry G. Leduc, Nuria Llombart, Daniel P. Marrone, Philip Mauskopf, Roger O'Brient, Stephen Padin, Theodore Reck, Loren J. Swenson, Jonas Zmuidzinas
SuperSpec is an ultra-compact spectrometer-on-a-chip for millimeter and submillimeter wavelength astronomy. Its very small size, wide spectral bandwidth, and highly multiplexed readout will enable construction of powerful multibeam spectrometers for high-redshift observations. The spectrometer consists of a horn-coupled microstrip feedline, a bank of narrow-band superconducting resonator filters that provide spectral selectivity, and Kinetic Inductance Detectors (KIDs) that detect the power admitted by each filter resonator. The design is realized using thin-film lithographic structures on a silicon wafer. The mm-wave microstrip feedline and spectral filters of the first prototype are designed to operate in the band from 195-310 GHz and are fabricated from niobium with at Tc of 9.2K. The KIDs are designed to operate at hundreds of MHz and are fabricated from titanium nitride with a Tc of 2K. Radiation incident on the horn travels along the mm-wave microstrip, passes through the frequency-selective filter, and is finally absorbed by the corresponding KID where it causes a measurable shift in the resonant frequency. In this proceedings, we present the design of the KIDs employed in SuperSpec and the results of initial laboratory testing of a prototype device. We will also briefly describe the ongoing development of a demonstration instrument that will consist of two 500-channel, R=700 spectrometers, one operating in the 1-mm atmospheric window and the other covering the 650 and 850 micron bands.
Zeeshan Ahmed, Yuri Alexeev, Giorgio Apollinari, Asimina Arvanitaki, David Awschalom, Karl K. Berggren, Karl Van Bibber, Przemyslaw Bienias, Geoffrey Bodwin, Malcolm Boshier, Daniel Bowring, Davide Braga, Karen Byrum, Gustavo Cancelo, Gianpaolo Carosi, Tom Cecil, Clarence Chang, Mattia Checchin, Sergei Chekanov, Aaron Chou, Aashish Clerk, Ian Cloet, Michael Crisler, Marcel Demarteau, Ranjan Dharmapalan, Matthew Dietrich, Junjia Ding, Zelimir Djurcic, John Doyle, James Fast, Michael Fazio, Peter Fierlinger, Hal Finkel, Patrick Fox, Gerald Gabrielse, Andrei Gaponenko, Maurice Garcia-Sciveres, Andrew Geraci, Jeffrey Guest, Supratik Guha, Salman Habib, Ron Harnik, Amr Helmy, Yuekun Heng, Jason Henning, Joseph Heremans, Phay Ho, Jason Hogan, Johannes Hubmayr, David Hume, Kent Irwin, Cynthia Jenks, Nick Karonis, Raj Kettimuthu, Derek Kimball, Jonathan King, Eve Kovacs, Richard Kriske, Donna Kubik, Akito Kusaka, Benjamin Lawrie, Konrad Lehnert, Paul Lett, Jonathan Lewis, Pavel Lougovski, Larry Lurio, Xuedan Ma, Edward May, Petra Merkel, Jessica Metcalfe, Antonino Miceli, Misun Min, Sandeep Miryala, John Mitchell, Vesna Mitrovic, Holger Mueller, Sae Woo Nam, Hogan Nguyen, Howard Nicholson, Andrei Nomerotski, Michael Norman, Kevin O'Brien, Roger O'Brient, Umeshkumar Patel, Bjoern Penning, Sergey Perverzev, Nicholas Peters, Raphael Pooser, Chrystian Posada, James Proudfoot, Tenzin Rabga, Tijana Rajh, Sergio Rescia, Alexander Romanenko, Roger Rusack, Monika Schleier-Smith, Keith Schwab, Julie Segal, Ian Shipsey, Erik Shirokoff, Andrew Sonnenschein, Valerie Taylor, Robert Tschirhart, Chris Tully, David Underwood, Vladan Vuletic, Robert Wagner, Gensheng Wang, Harry Weerts, Nathan Woollett, Junqi Xie, Volodymyr Yefremenko, John Zasadzinski, Jinlong Zhang, Xufeng Zhang, Vishnu Zutshi
Report of the first workshop to identify approaches and techniques in the domain of quantum sensing that can be utilized by future High Energy Physics applications to further the scientific goals of High Energy Physics.
CMB-S4 Collaboration, :, Kevork Abazajian, Graeme E. Addison, Peter Adshead, Zeeshan Ahmed, Daniel Akerib, Aamir Ali, Steven W. Allen, David Alonso, Marcelo Alvarez, Mustafa A. Amin, Adam Anderson, Kam S. Arnold, Peter Ashton, Carlo Baccigalupi, Debbie Bard, Denis Barkats, Darcy Barron, Peter S. Barry, James G. Bartlett, Ritoban Basu Thakur, Nicholas Battaglia, Rachel Bean, Chris Bebek, Amy N. Bender, Bradford A. Benson, Federico Bianchini, Colin A. Bischoff, Lindsey Bleem, James J. Bock, Sebastian Bocquet, Kimberly K. Boddy, J. Richard Bond, Julian Borrill, François R. Bouchet, Thejs Brinckmann, Michael L. Brown, Sean Bryan, Victor Buza, Karen Byrum, Carlos Hervias Caimapo, Erminia Calabrese, Victoria Calafut, Robert Caldwell, John E. Carlstrom, Julien Carron, Thomas Cecil, Anthony Challinor, Clarence L. Chang, Yuji Chinone, Hsiao-Mei Sherry Cho, Asantha Cooray, Will Coulton, Thomas M. Crawford, Abigail Crites, Ari Cukierman, Francis-Yan Cyr-Racine, Tijmen de Haan, Jacques Delabrouille, Mark Devlin, Eleonora Di Valentino, Marion Dierickx, Matt Dobbs, Shannon Duff, Jo Dunkley, Cora Dvorkin, Joseph Eimer, Tucker Elleflot, Josquin Errard, Thomas Essinger-Hileman, Giulio Fabbian, Chang Feng, Simone Ferraro, Jeffrey P. Filippini, Raphael Flauger, Brenna Flaugher, Aurelien A. Fraisse, Andrei Frolov, Nicholas Galitzki, Patricio A. Gallardo, Silvia Galli, Ken Ganga, Martina Gerbino, Vera Gluscevic, Neil Goeckner-Wald, Daniel Green, Daniel Grin, Evan Grohs, Riccardo Gualtieri, Jon E. Gudmundsson, Ian Gullett, Nikhel Gupta, Salman Habib, Mark Halpern, Nils W. Halverson, Shaul Hanany, Kathleen Harrington, Masaya Hasegawa, Matthew Hasselfield, Masashi Hazumi, Katrin Heitmann, Shawn Henderson, Brandon Hensley, Charles Hill, J. Colin Hill, Renée Hlozek, Shuay-Pwu Patty Ho, Thuong Hoang, Gil Holder, William Holzapfel, John Hood, Johannes Hubmayr, Kevin M. Huffenberger, Howard Hui, Kent Irwin, Oliver Jeong, Bradley R. Johnson, William C. Jones, Jae Hwan Kang, Kirit S. Karkare, Nobuhiko Katayama, Reijo Keskitalo, Theodore Kisner, Lloyd Knox, Brian J. Koopman, Arthur Kosowsky, John Kovac, Ely D. Kovetz, Steve Kuhlmann, Chao-lin Kuo, Akito Kusaka, Anne Lähteenmäki, Charles R. Lawrence, Adrian T. Lee, Antony Lewis, Dale Li, Eric Linder, Marilena Loverde, Amy Lowitz, Phil Lubin, Mathew S. Madhavacheril, Adam Mantz, Gabriela Marques, Frederick Matsuda, Philip Mauskopf, Heather McCarrick, Jeffrey McMahon, P. Daniel Meerburg, Jean-Baptiste Melin, Felipe Menanteau, Joel Meyers, Marius Millea, Joseph Mohr, Lorenzo Moncelsi, Maria Monzani, Tony Mroczkowski, Suvodip Mukherjee, Johanna Nagy, Toshiya Namikawa, Federico Nati, Tyler Natoli, Laura Newburgh, Michael D. Niemack, Haruki Nishino, Brian Nord, Valentine Novosad, Roger O'Brient, Stephen Padin, Steven Palladino, Bruce Partridge, Don Petravick, Elena Pierpaoli, Levon Pogosian, Karthik Prabhu, Clement Pryke, Giuseppe Puglisi, Benjamin Racine, Alexandra Rahlin, Mayuri Sathyanarayana Rao, Marco Raveri, Christian L. Reichardt, Mathieu Remazeilles, Graca Rocha, Natalie A. Roe, Anirban Roy, John E. Ruhl, Maria Salatino, Benjamin Saliwanchik, Emmanuel Schaan, Alessandro Schillaci, Benjamin Schmitt, Marcel M. Schmittfull, Douglas Scott, Neelima Sehgal, Sarah Shandera, Blake D. Sherwin, Erik Shirokoff, Sara M. Simon, Anze Slosar, David Spergel, Tyler St. Germaine, Suzanne T. Staggs, Antony Stark, Glenn D. Starkman, Radek Stompor, Chris Stoughton, Aritoki Suzuki, Osamu Tajima, Grant P. Teply, Keith Thompson, Ben Thorne, Peter Timbie, Maurizio Tomasi, Matthieu Tristram, Gregory Tucker, Caterina Umiltà, Alexander van Engelen, Eve M. Vavagiakis, Joaquin D. Vieira, Abigail G. Vieregg, Kasey Wagoner, Benjamin Wallisch, Gensheng Wang, Scott Watson, Ben Westbrook, Nathan Whitehorn, Edward J. Wollack, W. L. Kimmy Wu, Zhilei Xu, H. Y. Eric Yang, Siavash Yasini, Volodymyr G. Yefremenko, Ki Won Yoon, Edward Young, Cyndia Yu, Andrea Zonca
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, Silvia Zhang
We demonstrate a wide-band 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$\times$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 $\sim$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 are 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 $\sim$ 5% ellipticity and $\sim$10-15% peak-to-peak differences for A-B polarization pairs.
Kevork Abazajian, Arwa Abdulghafour, Graeme E. Addison, Peter Adshead, Zeeshan Ahmed, Marco Ajello, Daniel Akerib, Steven W. Allen, David Alonso, Marcelo Alvarez, Mustafa A. Amin, Mandana Amiri, Adam Anderson, Behzad Ansarinejad, Melanie Archipley, Kam S. Arnold, Matt Ashby, Han Aung, Carlo Baccigalupi, Carina Baker, Abhishek Bakshi, Debbie Bard, Denis Barkats, Darcy Barron, Peter S. Barry, James G. Bartlett, Paul Barton, Ritoban Basu Thakur, Nicholas Battaglia, Jim Beall, Rachel Bean, Dominic Beck, Sebastian Belkner, Karim Benabed, Amy N. Bender, Bradford A. Benson, Bobby Besuner, Matthieu Bethermin, Sanah Bhimani, Federico Bianchini, Simon Biquard, Ian Birdwell, Colin A. Bischoff, Lindsey Bleem, Paulina Bocaz, James J. Bock, Sebastian Bocquet, Kimberly K. Boddy, J. Richard Bond, Julian Borrill, Francois R. Bouchet, Thejs Brinckmann, Michael L. Brown, Sean Bryan, Victor Buza, Karen Byrum, Erminia Calabrese, Victoria Calafut, Robert Caldwell, John E. Carlstrom, Julien Carron, Thomas Cecil, Anthony Challinor, Victor Chan, Clarence L. Chang, Scott Chapman, Eric Charles, Eric Chauvin, Cheng Cheng, Grace Chesmore, Kolen Cheung, Yuji Chinone, Jens Chluba, Hsiao-Mei Sherry Cho, Steve Choi, Justin Clancy, Susan Clark, Asantha Cooray, Gabriele Coppi, John Corlett, Will Coulton, Thomas M. Crawford, Abigail Crites, Ari Cukierman, Francis-Yan Cyr-Racine, Wei-Ming Dai, Cail Daley, Eli Dart, Gregorg Daues, Tijmen de Haan, Cosmin Deaconu, Jacques Delabrouille, Greg Derylo, Mark Devlin, Eleonora Di Valentino, Marion Dierickx, Brad Dober, Randy Doriese, Shannon Duff, Daniel Dutcher, Cora Dvorkin, Rolando Dünner, Tarraneh Eftekhari, Joseph Eimer, Hamza El Bouhargani, Tucker Elleflot, Nick Emerson, Josquin Errard, Thomas Essinger-Hileman, Giulio Fabbian, Valentina Fanfani, Alessandro Fasano, Chang Feng, Simone Ferraro, Jeffrey P. Filippini, Raphael Flauger, Brenna Flaugher, Aurelien A. Fraisse, Josef Frisch, Andrei Frolov, Nicholas Galitzki, Patricio A. Gallardo, Silvia Galli, Ken Ganga, Martina Gerbino, Christos Giannakopoulos, Murdock Gilchriese, Vera Gluscevic, Neil Goeckner-Wald, David Goldfinger, Daniel Green, Paul Grimes, Daniel Grin, Evan Grohs, Riccardo Gualtieri, Vic Guarino, Jon E. Gudmundsson, Ian Gullett, Sam Guns, Salman Habib, Gunther Haller, Mark Halpern, Nils W. Halverson, Shaul Hanany, Emma Hand, Kathleen Harrington, Masaya Hasegawa, Matthew Hasselfield, Masashi Hazumi, Katrin Heitmann, Shawn Henderson, Brandon Hensley, Ryan Herbst, Carlos Hervias-Caimapo, J. Colin Hill, Richard Hills, Eric Hivon, Renée Hlozek, Anna Ho, Gil Holder, Matt Hollister, William Holzapfel, John Hood, Selim Hotinli, Alec Hryciuk, Johannes Hubmayr, Kevin M. Huffenberger, Howard Hui, Roberto Ibá nez, Ayodeji Ibitoye, Margaret Ikape, Kent Irwin, Cooper Jacobus, Oliver Jeong, Bradley R. Johnson, Doug Johnstone, William C. Jones, John Joseph, Baptiste Jost, Jae Hwan Kang, Ari Kaplan, Kirit S. Karkare, Nobuhiko Katayama, Reijo Keskitalo, Cesiley King, Theodore Kisner, Matthias Klein, Lloyd Knox, Brian J. Koopman, Arthur Kosowsky, John Kovac, Ely D. Kovetz, Alex Krolewski, Donna Kubik, Steve Kuhlmann, Chao-Lin Kuo, Akito Kusaka, Anne Lähteenmäki, Kenny Lau, Charles R. Lawrence, Adrian T. Lee, Louis Legrand, Matthaeus Leitner, Clément Leloup, Antony Lewis, Dale Li, Eric Linder, Ioannis Liodakis, Jia Liu, Kevin Long, Thibaut Louis, Marilena Loverde, Lindsay Lowry, Chunyu Lu, Phil Lubin, Yin-Zhe Ma, Thomas Maccarone, Mathew S. Madhavacheril, Felipe Maldonado, Adam Mantz, Gabriela Marques, Frederick Matsuda, Philip Mauskopf, Jared May, Heather McCarrick, Ken McCracken, Jeffrey McMahon, P. Daniel Meerburg, Jean-Baptiste Melin, Felipe Menanteau, Joel Meyers, Marius Millea, Vivian Miranda, Don Mitchell, Joseph Mohr, Lorenzo Moncelsi, Maria Elena Monzani, Magdy Moshed, Tony Mroczkowski, Suvodip Mukherjee, Moritz Münchmeyer, Daisuke Nagai, Chandan Nagarajappa, Johanna Nagy, Toshiya Namikawa, Federico Nati, Tyler Natoli, Simran Nerval, Laura Newburgh, Hogan Nguyen, Erik Nichols, Andrina Nicola, Michael D. Niemack, Brian Nord, Tim Norton, Valentine Novosad, Roger O'Brient, Yuuki Omori, Giorgio Orlando, Benjamin Osherson, Rachel Osten, Stephen Padin, Scott Paine, Bruce Partridge, Sanjaykumar Patil, Don Petravick, Matthew Petroff, Elena Pierpaoli, Mauricio Pilleux, Levon Pogosian, Karthik Prabhu, Clement Pryke, Giuseppe Puglisi, Benjamin Racine, Srinivasan Raghunathan, Alexandra Rahlin, Marco Raveri, Ben Reese, Christian L. Reichardt, Mathieu Remazeilles, Arianna Rizzieri, Graca Rocha, Natalie A. Roe, Kaja Rotermund, Anirban Roy, John E. Ruhl, Joe Saba, Noah Sailer, Maria Salatino, Benjamin Saliwanchik, Leonid Sapozhnikov, Mayuri Sathyanarayana Rao, Lauren Saunders, Emmanuel Schaan, Alessandro Schillaci, Benjamin Schmitt, Douglas Scott, Neelima Sehgal, Sarah Shandera, Blake D. Sherwin, Erik Shirokoff, Corwin Shiu, Sara M. Simon, Baibhav Singari, Anze Slosar, David Spergel, Tyler St. Germaine, Suzanne T. Staggs, Antony A. Stark, Glenn D. Starkman, Bryan Steinbach, Radek Stompor, Chris Stoughton, Aritoki Suzuki, Osamu Tajima, Chris Tandoi, Grant P. Teply, Gregg Thayer, Keith Thompson, Ben Thorne, Peter Timbie, Maurizio Tomasi, Cynthia Trendafilova, Matthieu Tristram, Carole Tucker, Gregory Tucker, Caterina Umiltà, Alexander van Engelen, Joshiwa van Marrewijk, Eve M. Vavagiakis, Clara Vergès, Joaquin D. Vieira, Abigail G. Vieregg, Kasey Wagoner, Benjamin Wallisch, Gensheng Wang, Guo-Jian Wang, Scott Watson, Duncan Watts, Chris Weaver, Lukas Wenzl, Ben Westbrook, Martin White, Nathan Whitehorn, Andrew Wiedlea, Paul Williams, Robert Wilson, Harrison Winch, Edward J. Wollack, W. L. Kimmy Wu, Zhilei Xu, Volodymyr G. Yefremenko, Cyndia Yu, David Zegeye, Jeff Zivick, Andrea Zonca
Shubh Agrawal, Bryan Steinbach, James J. Bock, Clifford Frez, Lorenzo Minutolo, Hien Nguyen, Roger O'Brient, Anthony Turner, Albert Wandui
We demonstrate strong negative electrothermal feedback accelerating and linearizing the response of a thermal kinetic inductance detector (TKID). TKIDs are a proposed highly multiplexable replacement to transition-edge sensors and measure power through the temperature-dependent resonant frequency of a superconducting microresonator bolometer. At high readout probe power and probe frequency detuned from the TKID resonant frequency, we observe electrothermal feedback loop gain up to $\mathcal L$ $\approx$ 16 through measuring the reduction of settling time. We also show that the detector response has no detectable non-linearity over a 38% range of incident power and that the noise-equivalent power is below the design photon noise.
Logan Foote, Michael D. Audley, Charles, Bradford, Gert de Lange, Pierre Echternach, Dale J. Fixsen, Howard Hui, Matthew Kenyon, Hien Nguyen, Roger O'Brient, Elmer H. Sharp, Johannes G. Staguhn, Jan van der Kuur, Jonas Zmuidzinas
We report on efforts to improve the speed of low-G far-infrared transition-edged-sensed bolometers. We use a fabrication process that does not require any dry etch steps to reduce heat capacity on the suspended device and measure a reduction in the detector time constant. However, we also measure an increase in the temperature-normalized thermal conductance (G), and a corresponding increase in the noise-equivalent power (NEP). We employ a new near-IR photon-noise technique using a near-IR laser to calibrate the frequency-domain multiplexed AC system and compare the results to a well-understood DC circuit. We measure an NEP white noise level of 0.8 aW/rtHz with a 1/f knee below 0.1 Hz and a time constant of 3.2 ms.
Christos Giannakopoulos, Clara Vergès, P. A. R. Ade, Zeeshan Ahmed, Mandana Amiri, Denis Barkats, Ritoban Basu Thakur, Colin A. Bischoff, Dominic Beck, James J. Bock, Hans Boenish, Victor Buza, James R. Cheshire, Jake Connors, James Cornelison, Michael Crumrine, Ari Jozef Cukierman, Edward Denison, Marion Dierickx, Lionel Duband, Miranda Eiben, Brodi D. Elwood, Sofia Fatigoni, Jeff P. Filippini, Antonio Fortes, Min Gao, Neil Goeckner-Wald, David C. Goldfinger, James A. Grayson, Paul K. Grimes, Grantland Hall, George Halal, Mark Halpern, Emma Hand, Sam A. Harrison, Shawn Henderson, Johannes Hubmayr, Howard Hui, Kent D. Irwin, Jae Hwan Kang, Kirit S. Karkare, Sinan Kefeli, J. M. Kovac, Chao-Lin Kuo, King Lau, Margaret Lautzenhiser, Amber Lennox, Tongtian Liu, Koko G. Megerian, Oliver Miller, Lorenzo Minutolo, Lorenzo Moncelsi, Yuka Nakato, H. T. Nguyen, Roger O'brient, Anika Patel, Matthew A. Petroff, Anna R. Polish, Nathan Precup, Thomas Prouve, Clement Pryke, Carl D. Reintsema, Thibault Romand, Maria Salatino, Alessandro Schillaci, Benjamin Schmitt, Baibhav Singari, Ahmed Soliman, Tyler St Germaine, Aaron Steiger, Bryan Steinbach, Rashmi Sudiwala, Keith L. Thompson, Calvin Tsai, Carole Tucker, Anthony D. Turner, Abigail G. Vieregg, Albert Wandui, Alexis C. Weber, Justin Willmert, Wai Ling K. Wu, Hung-I Yang, Cyndia Yu, Lingzhen Zeng, Cheng Zhang, Silvia Zhang
Sep 24, 2024·astro-ph.CO·PDF The BICEP3 and BICEP Array polarimeters are small-aperture refracting telescopes located at the South Pole designed to measure primordial gravitational wave signatures in the Cosmic Microwave Background (CMB) polarization, predicted by inflation. Constraining the inflationary signal requires not only excellent sensitivity, but also careful control of instrumental systematics. Both instruments use antenna-coupled orthogonally polarized detector pairs, and the polarized sky signal is reconstructed by taking the difference in each detector pair. As a result, the differential response between detectors within a pair becomes an important systematic effect we must control. Additionally, mapping the intensity and polarization response in regions away from the main beam can inform how sidelobe levels affect CMB measurements. Extensive calibration measurements are taken in situ every austral summer for control of instrumental systematics and instrument characterisation. In this work, we detail the set of beam calibration measurements that we conduct on the BICEP receivers, from deep measurements of main beam response to polarized beam response and sidelobe mapping. We discuss the impact of these measurements for instrumental systematics studies and design choices for future CMB receivers.
Gregor G. Taylor, Alexander B. Walter, Boris Korzh, Bruce Bumble, Sahil R. Patel, Jason P. Allmaras, Andrew D. Beyer, Roger O'Brient, Matthew D. Shaw, Emma E. Wollman
Aug 29, 2023·quant-ph·PDF We report on the extension of the spectral sensitivity of superconducting nanowire single-photon detectors to a wavelength of 29 $μ$m. This represents the first demonstration of a time correlated single-photon counting detector at these long infrared wavelengths. We achieve saturated internal detection efficiency from 10 to 29 $μ$m, whilst maintaining dark count rates below 0.1 counts per second. Extension of superconducting nanowire single-photon detectors to this spectral range provides low noise and high timing resolution photon counting detection, effectively providing a new class of single-photon sensitive detector for these wavelengths. These detectors are important for applications such as exoplanet spectroscopy, infrared astrophysics, physical chemistry, remote sensing and direct dark-matter detection.
Jamil A. Shariff, Peter A. R. Ade, Mandana Amiri, Steven J. Benton, Jamie J. Bock, J. Richard Bond, Sean A. Bryan, H. Cynthia Chiang, Carlo R. Contaldi, Brendan P. Crill, Olivier P. Doré, Marzieh Farhang, Jeffrey P. Filippini, Laura M. Fissel, Aurelien A. Fraisse, Anne E. Gambrel, Natalie N. Gandilo, Sunil R. Golwala, Jon E. Gudmundsson, Mark Halpern, Matthew Hasselfield, Gene C. Hilton, Warren A. Holmes, Viktor V. Hristov, Kent D. Irwin, William C. Jones, Zigmund D. Kermish, Chao-Lin Kuo, Carolyn J. MacTavish, Peter V. Mason, Krikor G. Megerian, Lorenzo Moncelsi, Tracy A. Morford, Johanna M. Nagy, C. Barth Netterfield, Roger O'Brient, Alexandra S. Rahlin, Carl D. Reintsema, John E. Ruhl, Marcus C. Runyan, Juan D. Soler, Amy Trangsrud, Carole E. Tucker, Rebecca S. Tucker, Anthony D. Turner, Alexis C. Weber, Donald V. Wiebe, Edward Y. Young
We present the technology and control methods developed for the pointing system of the SPIDER experiment. SPIDER is a balloon-borne polarimeter designed to detect the imprint of primordial gravitational waves in the polarization of the Cosmic Microwave Background radiation. We describe the two main components of the telescope's azimuth drive: the reaction wheel and the motorized pivot. A 13 kHz PI control loop runs on a digital signal processor, with feedback from fibre optic rate gyroscopes. This system can control azimuthal speed with < 0.02 deg/s RMS error. To control elevation, SPIDER uses stepper-motor-driven linear actuators to rotate the cryostat, which houses the optical instruments, relative to the outer frame. With the velocity in each axis controlled in this way, higher-level control loops on the onboard flight computers can implement the pointing and scanning observation modes required for the experiment. We have accomplished the non-trivial task of scanning a 5000 lb payload sinusoidally in azimuth at a peak acceleration of 0.8 deg/s$^2$, and a peak speed of 6 deg/s. We can do so while reliably achieving sub-arcminute pointing control accuracy.