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1. Erratum: 'The First CHIME/FRB Fast Radio Burst Catalog' (2021, ApJS, 257, 59)

Author: The CHIME/FRB Collaboration, Mandana Amiri, Bridget C. Andersen, Kevin Bandura, Sabrina Berger, Mohit Bhardwaj, Michelle M. Boyce, P. J. Boyle, Charanjot Brar, Daniela Breitman, Tomas Cassanelli, Pragya Chawla, Tianyue Chen, J.-F. Cliche, Amanda Cook, Davor Cubranic, Alice P. Curtin, Meiling Deng, Matt Dobbs, Fengqiu (Adam) Dong, Gwendolyn Eadie, Mateus Fandino, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Deborah C. Good, Mark Halpern, Alex S. Hill, Gary Hinshaw, Alexander Josephy, Jane F. Kaczmarek, Zarif Kader, Joseph W. Kania, Victoria M. Kaspi, T. L. Landecker, Dustin Lang, Calvin Leung, Dongzi Li, Hsiu-Hsien Lin, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Marcus Merryfield, Bradley W. Meyers, Daniele Michilli, Nikola Milutinovic, Arash Mirhosseini, Moritz Münchmeyer, Arun Naidu, Laura Newburgh, Cherry Ng, Chitrang Patel, Ue-Li Pen, Emily Petroff, Tristan Pinsonneault-Marotte, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott M. Ransom, Andre Renard, Pranav Sanghavi, Paul Scholz, J. Richard Shaw, Kaitlyn Shin, Seth R. Siegel, Andrew E. Sikora, Saurabh Singh, Kendrick M. Smith, Ingrid Stairs, Chia Min Tan, S. P. Tendulkar, Keith Vanderlinde, Haochen Wang, Dallas Wulf, and A. V. Zwaniga
Subjects: Astrophysics, QB460-466
Published: 2023
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2. A SQUID controller unit for space-based TES sensor readout

Author: M. Zannoni, A. Passerini, G. Signorelli, J.-F. Cliche, G. Coppi, P. Dal Bo, S. Della Torre, E. Di Giorgi, M. Dobbs, L. Galli, M. Gervasi, A. Limonta, M. Massa, A. Moggi, J. Montgomery, F. Nati, D. Nicolò, M. Pinchera, D. Poletti, G. Smecher, F. Spinella, A. Tartari, Zannoni, M, Passerini, A, Signorelli, G, Cliche, J, Coppi, G, Bo, P, Torre, S, Giorgi, E, Dobbs, M, Galli, L, Gervasi, M, Limonta, A, Massa, M, Moggi, A, Montgomery, J, Nati, F, Nicolo, D, Pinchera, M, Poletti, D, Smecher, G, Spinella, F, and Tartari, A
Subjects: FIS/05 - ASTRONOMIA E ASTROFISICA, Nuclear and High Energy Physics, TES readout, CMB, SQUID, Instrumentation
Abstract: We have developed a Superconducting Quantum Interference Device (SQUID) controller unit for Transition Edge Sensors (TES) readout, designed to be used in a space mission. The unit is made of 8 boards and each board can condition four SQUID array amplifiers. The board design is inspired by a similar one developed for ground based experiments, but specific changes have been made to adopt Components Off The Shelf (COTS) with space grade equivalents, to implement redundancy and cross-strapping capabilities. The design also includes the thermal path to lift the heat off the boards towards an in-house designed monolithic aluminum rack.
Published: 2023
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3. A clock stabilization system for CHIME/FRB Outriggers

Author: J. Mena-Parra, C. Leung, S. Cary, K. W. Masui, J. F. Kaczmarek, M. Amiri, K. Bandura, P. J. Boyle, T. Cassanelli, J.-F. Cliche, M. Dobbs, V. M. Kaspi, T. L. Landecker, A. Lanman, and J. L. Sievers
Subjects: Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The Canadian Hydrogen Intensity Mapping Experiment (CHIME) has emerged as the prime telescope for detecting fast radio bursts (FRBs). CHIME/FRB Outriggers will be a dedicated very-long-baseline interferometry (VLBI) instrument consisting of outrigger telescopes at continental baselines working with CHIME and its specialized real-time transient-search backend (CHIME/FRB) to detect and localize FRBs with 50 mas precision. In this paper we present a minimally invasive clock stabilization system that effectively transfers the CHIME digital backend reference clock from its original GPS-disciplined ovenized crystal oscillator to a passive hydrogen maser. This enables us to combine the long-term stability and absolute time tagging of the GPS clock with the short and intermediate-term stability of the maser to reduce the clock timing errors between VLBI calibration observations. We validate the system with VLBI-style observations of Cygnus A over a 400 m baseline between CHIME and the CHIME Pathfinder, demonstrating agreement between sky-based and maser-based timing measurements at the 30 ps rms level on timescales ranging from one minute to up to nine days, and meeting the stability requirements for CHIME/FRB Outriggers. In addition, we present an alternate reference clock solution for outrigger stations which lack the infrastructure to support a passive hydrogen maser., 15 pages, 7 figures, submitted to AJ
Published: 2021

4. On-Sky Performance of the SPT-3G Frequency-Domain Multiplexed Readout

Author: J. A. Sobrin, Thomas Cecil, E. V. Denison, S. S. Meyer, Kent D. Irwin, Peter A. R. Ade, W. L. Holzapfel, K. T. Story, K. Vanderlinde, A. E. Lowitz, V. Novosad, Donna Kubik, Aled Jones, John E. Carlstrom, G. I. Noble, Lincoln Bryant, Jason W. Henning, T. de Haan, Ki Won Yoon, Volodymyr Yefremenko, Nathan Whitehorn, Zeeshan Ahmed, T. Natoli, N. L. Harrington, Gene C. Hilton, Robert Gardner, Amy N. Bender, Carole Tucker, Jason Gallicchio, E. M. Leitch, C. L. Chang, A. E. Gambrel, W. B. Everett, A. Foster, Adrian T. Lee, D. Howe, D. Dutcher, Antony A. Stark, M. Jonas, Aritoki Suzuki, J. E. Ruhl, J. Stephen, Trupti Khaire, D. Riebel, Bradford Benson, J. F. Cliche, Joshua Montgomery, H. M. Cho, Ari Cukierman, Graeme Smecher, Z. Pan, Alexandra S. Rahlin, R. Basu Thakur, Matt Dobbs, K. R. Ferguson, Faustin Carter, Andrew Nadolski, Junjia Ding, Adam Anderson, M. R. Young, N. W. Halverson, Leila R. Vale, Oliver Jeong, Chao-Lin Kuo, Keith L. Thompson, John Groh, Karen Byrum, John E. Pearson, P. Paschos, N. Huang, A. Gilbert, J. Fu, A. M. Kofman, Jessica Avva, R. Guyser, Stephen Padin, C. M. Posada, Steve Kuhlmann, Joaquin Vieira, S. Guns, Daniel Michalik, Gensheng Wang, W. Quan, Erik Shirokoff, Peter S. Barry, A. H. Harke-Hosemann, H. T. Nguyen, M. Korman, and J. T. Sayre
Subjects: Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Multiplexing, Noise (electronics), 010305 fluids & plasmas, law.invention, Optics, law, 0103 physical sciences, General Materials Science, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, business.industry, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), White noise, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, South Pole Telescope, Frequency domain, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, business, Voltage
Abstract: Frequency-domain multiplexing (fMux) is an established technique for the readout of large arrays of transition edge sensor (TES) bolometers. Each TES in a multiplexing module has a unique AC voltage bias that is selected by a resonant filter. This scheme enables the operation and readout of multiple bolometers on a single pair of wires, reducing thermal loading onto sub-Kelvin stages. The current receiver on the South Pole Telescope, SPT-3G, uses a 68x fMux system to operate its large-format camera of $\sim$16,000 TES bolometers. We present here the successful implementation and performance of the SPT-3G readout as measured on-sky. Characterization of the noise reveals a median pair-differenced 1/f knee frequency of 33 mHz, indicating that low-frequency noise in the readout will not limit SPT-3G's measurements of sky power on large angular scales. Measurements also show that the median readout white noise level in each of the SPT-3G observing bands is below the expectation for photon noise, demonstrating that SPT-3G is operating in the photon-noise-dominated regime., Comment: 9 pages, 5 figures submitted to the Journal of Low Temperature Physics: LTD18 Special Edition
Published: 2019
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5. Performance of Al–Mn Transition-Edge Sensor Bolometers in SPT-3G

Author: M. Korman, Kent D. Irwin, W. L. Holzapfel, J. E. Ruhl, H. M. Cho, Ari Cukierman, V. Novosad, Donna Kubik, C. L. Chang, A. E. Gambrel, Alexandra S. Rahlin, Matt Dobbs, K. Vanderlinde, Keith L. Thompson, D. Howe, M. R. Young, Karen Byrum, Thomas Cecil, R. Basu Thakur, Erik Shirokoff, P. Paschos, Aled Jones, Peter A. R. Ade, Zeeshan Ahmed, Amy N. Bender, Ki Won Yoon, A. H. Harke-Hosemann, K. T. Story, A. E. Lowitz, H. T. Nguyen, D. Dutcher, Antony A. Stark, J. A. Sobrin, J. Stephen, Jason Gallicchio, Lincoln Bryant, Jason W. Henning, J. T. Sayre, S. S. Meyer, Volodymyr Yefremenko, Nathan Whitehorn, John E. Pearson, Peter S. Barry, N. L. Harrington, T. Natoli, Andrew Nadolski, Jessica Avva, G. I. Noble, Carole Tucker, R. Guyser, Stephen Padin, Trupti Khaire, N. Huang, A. Foster, Joshua Montgomery, A. Gilbert, C. M. Posada, Bradford Benson, Robert Gardner, J. F. Cliche, Steve Kuhlmann, Gene C. Hilton, Joaquin Vieira, Chao-Lin Kuo, S. Guns, Graeme Smecher, W. B. Everett, N. W. Halverson, Daniel Michalik, Gensheng Wang, John Groh, J. Fu, E. V. Denison, W. Quan, A. M. Kofman, M. Jonas, Leila R. Vale, Adrian T. Lee, Aritoki Suzuki, Faustin Carter, Junjia Ding, John E. Carlstrom, T. de Haan, E. M. Leitch, D. Riebel, Oliver Jeong, Z. Pan, K. R. Ferguson, and Adam Anderson
Subjects: Physics - Instrumentation and Detectors, Materials science, Physics::Instrumentation and Detectors, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Multiplexing, 010305 fluids & plasmas, law.invention, Optics, law, 0103 physical sciences, General Materials Science, Wafer, 010306 general physics, Anisotropy, Instrumentation and Methods for Astrophysics (astro-ph.IM), business.industry, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), Condensed Matter Physics, Atomic and Molecular Physics, and Optics, South Pole Telescope, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, business
Abstract: SPT-3G is a polarization-sensitive receiver, installed on the South Pole Telescope, that measures the anisotropy of the cosmic microwave background (CMB) from degree to arcminute scales. The receiver consists of ten 150~mm-diameter detector wafers, containing a total of 16,000 transition-edge sensor (TES) bolometers observing at 95, 150, and 220 GHz. During the 2018-2019 austral summer, one of these detector wafers was replaced by a new wafer fabricated with Al-Mn TESs instead of the Ti/Au design originally deployed for SPT-3G. We present the results of in-lab characterization and on-sky performance of this Al-Mn wafer, including electrical and thermal properties, optical efficiency measurements, and noise-equivalent temperature. In addition, we discuss and account for several calibration-related systematic errors that affect measurements made using frequency-domain multiplexing readout electronics., Comment: 9 pages, 5 figures, submitted to the Journal of Low Temperature Physics: LTD18 Special Edition
Published: 2019
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6. Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope

Author: P. M. Chichura, A. Foster, C. Patel, N. Ossa-Jaen, P. A. R. Ade, Z. Ahmed, A. J. Anderson, M. Archipley, J. E. Austermann, J. S. Avva, L. Balkenhol, P. S. Barry, R. Basu Thakur, J. A. Beall, K. Benabed, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, F. R. Bouchet, L. Bryant, K. Byrum, J. E. Carlstrom, F. W. Carter, T. W. Cecil, C. L. Chang, P. Chaubal, G. Chen, H. C. Chiang, H.-M. Cho, T-L. Chou, R. Citron, J.-F. Cliche, T. M. Crawford, A. T. Crites, A. Cukierman, C. M. Daley, E. V. Denison, K. Dibert, J. Ding, M. A. Dobbs, D. Dutcher, W. Everett, C. Feng, K. R. Ferguson, J. Fu, S. Galli, J. Gallicchio, A. E. Gambrel, R. W. Gardner, E. M. George, N. Goeckner-Wald, R. Gualtieri, S. Guns, N. Gupta, R. Guyser, T. de Haan, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, D. Howe, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, O. B. Jeong, M. Jonas, A. Jones, T. S. Khaire, L. Knox, A. M. Kofman, M. Korman, D. L. Kubik, S. Kuhlmann, C.-L. Kuo, A. T. Lee, E. M. Leitch, D. Li, A. Lowitz, C. Lu, D. P. Marrone, J. J. McMahon, S. S. Meyer, D. Michalik, M. Millea, L. M. Mocanu, J. Montgomery, C. Corbett Moran, A. Nadolski, T. Natoli, H. Nguyen, J. P. Nibarger, G. Noble, V. Novosad, Y. Omori, S. Padin, Z. Pan, P. Paschos, S. Patil, J. Pearson, K. A. Phadke, C. M. Posada, K. Prabhu, C. Pryke, W. Quan, A. Rahlin, C. L. Reichardt, D. Riebel, B. Riedel, M. Rouble, J. E. Ruhl, B. R. Saliwanchik, J. T. Sayre, K. K. Schaffer, E. Schiappucci, E. Shirokoff, C. Sievers, G. Smecher, J. A. Sobrin, A. Springmann, A. A. Stark, J. Stephen, K. T. Story, A. Suzuki, C. Tandoi, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, L. R. Vale, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, K. W. Yoon, and M. R. Young
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the first measurements of asteroids in millimeter wavelength (mm) data from the South Pole Telescope (SPT), which is used primarily to study the cosmic microwave background (CMB). We analyze maps of two $\sim270$ deg$^2$ sky regions near the ecliptic plane, each observed with the SPTpol camera $\sim100$ times over one month. We subtract the mean of all maps of a given field, removing static sky signal, and then average the mean-subtracted maps at known asteroid locations. We detect three asteroids$\text{ -- }$(324) Bamberga, (13) Egeria, and (22) Kalliope$\text{ -- }$with signal-to-noise ratios (S/N) of 11.2, 10.4, and 6.1, respectively, at 2.0 mm (150 GHz); we also detect (324) Bamberga with S/N of 4.1 at 3.2 mm (95 GHz). We place constraints on these asteroids' effective emissivities, brightness temperatures, and light curve modulation amplitude. Our flux density measurements of (324) Bamberga and (13) Egeria roughly agree with predictions, while our measurements of (22) Kalliope suggest lower flux, corresponding to effective emissivities of $0.66 \pm 0.11$ at 2.0 mm and $, 21 pages, 9 figures
Published: 2022
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7. Measurements of the E -mode polarization and temperature- E -mode correlation of the CMB from SPT-3G 2018 data

Author: Faustin Carter, S. E. Kuhlmann, Junjia Ding, Gene C. Hilton, J. C. Hood, A. T. Lee, M. Millea, Erik Shirokoff, Oliver Jeong, N. W. Halverson, Thomas Cecil, John E. Pearson, G. I. Noble, John E. Carlstrom, E. V. Denison, B. Thorne, K. Prabhu, C. L. Kuo, François R. Bouchet, M. Korman, Federico Bianchini, K. Dibert, S. Padin, Ethan Anderes, Neil Goeckner-Wald, D. Riebel, J. E. Ruhl, Jason W. Henning, Nikhel Gupta, N. Huang, M. Rouble, M. Jonas, RB Thakur, K. L. Thompson, J. T. Sayre, C. Tucker, A. A. Stark, A. Lowitz, M. A. Dobbs, N. L. Harrington, Z. Pan, Karen Byrum, A. H. Harke-Hosemann, C. Lu, Srinivasan Raghunathan, B. Riedel, C. L. Chang, A. Cukierman, Andreas Bender, Z. Ahmed, K. Aylor, E. M. Leitch, Alexandra S. Rahlin, S. Guns, J. A. Sobrin, K. W. Yoon, D. Howe, P. Chaubal, Young, Graeme Smecher, C. Umilta, J. F. Cliche, T. de Haan, Silvia Galli, H. Nguyen, Lloyd Knox, T. Natoli, K. Vanderlinde, T. M. Crawford, J. Fu, P. Paschos, S. S. Meyer, Christian L. Reichardt, H-M. Cho, L. R. Vale, A. Foster, K. T. Story, Karim Benabed, E. Hivon, E. Schiappucci, Anthony P. Jones, Andrew Nadolski, Lindsey Bleem, Jessica Avva, Peter S. Barry, L. Balkenhol, Bradford Benson, Yefremenko, R. Guyser, R. Gualtieri, C. M. Posada, Chang Feng, G. P. Holder, A. M. Kofman, Daniel Michalik, Novosad, J. D. Vieira, C. Daley, Gensheng Wang, W. L. Holzapfel, W. Quan, K. R. Ferguson, Adam Anderson, Gang Chen, Nathan Whitehorn, Robert Gardner, M. Archipley, Y. Omori, A. Suzuki, Lincoln Bryant, D. Dutcher, T.-L. Chou, Trupti Khaire, Joshua Montgomery, J. Stephen, A. E. Gambrel, Kent D. Irwin, W. L. K. Wu, Donna Kubik, P. A. R. Ade, and W. B. Everett
Subjects: Physics, 010308 nuclear & particles physics, Cosmic microwave background, Spectral density, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Parameter space, 01 natural sciences, 7. Clean energy, symbols.namesake, Amplitude, Gravitational lens, South Pole Telescope, 0103 physical sciences, symbols, Planck, Multipole expansion, 010303 astronomy & astrophysics
Abstract: We present measurements of the $E$-mode ($EE$) polarization power spectrum and temperature-$E$-mode ($TE$) cross-power spectrum of the cosmic microwave background using data collected by SPT-3G, the latest instrument installed on the South Pole Telescope. This analysis uses observations of a 1500 deg$^2$ region at 95, 150, and 220 GHz taken over a four month period in 2018. We report binned values of the $EE$ and $TE$ power spectra over the angular multipole range $300 \le \ell < 3000$, using the multifrequency data to construct six semi-independent estimates of each power spectrum and their minimum-variance combination. These measurements improve upon the previous results of SPTpol across the multipole ranges $300 \le \ell \le 1400$ for $EE$ and $300 \le \ell \le 1700$ for $TE$, resulting in constraints on cosmological parameters comparable to those from other current leading ground-based experiments. We find that the SPT-3G dataset is well-fit by a $\Lambda$CDM cosmological model with parameter constraints consistent with those from Planck and SPTpol data. From SPT-3G data alone, we find $H_0 = 68.8 \pm 1.5 \mathrm{km\,s^{-1}\,Mpc^{-1}}$ and $\sigma_8 = 0.789 \pm 0.016$, with a gravitational lensing amplitude consistent with the $\Lambda$CDM prediction ($A_L = 0.98 \pm 0.12$). We combine the SPT-3G and the Planck datasets and obtain joint constraints on the $\Lambda$CDM model. The volume of the 68% confidence region in six-dimensional $\Lambda$CDM parameter space is reduced by a factor of 1.5 compared to Planck-only constraints, with only slight shifts in central values. We note that the results presented here are obtained from data collected during just half of a typical observing season with only part of the focal plane operable, and that the active detector count has since nearly doubled for observations made with SPT-3G after 2018.
Published: 2021
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8. The Design and Integrated Performance of SPT-3G

Author: J. A. Sobrin, A. J. Anderson, A. N. Bender, B. A. Benson, D. Dutcher, A. Foster, N. Goeckner-Wald, J. Montgomery, A. Nadolski, A. Rahlin, P. A. R. Ade, Z. Ahmed, E. Anderes, M. Archipley, J. E. Austermann, J. S. Avva, K. Aylor, L. Balkenhol, P. S. Barry, R. Basu Thakur, K. Benabed, F. Bianchini, L. E. Bleem, F. R. Bouchet, L. Bryant, K. Byrum, J. E. Carlstrom, F. W. Carter, T. W. Cecil, C. L. Chang, P. Chaubal, G. Chen, H.-M. Cho, T.-L. Chou, J.-F. Cliche, T. M. Crawford, A. Cukierman, C. Daley, T. de Haan, E. V. Denison, K. Dibert, J. Ding, M. A. Dobbs, W. Everett, C. Feng, K. R. Ferguson, J. Fu, S. Galli, A. E. Gambrel, R. W. Gardner, R. Gualtieri, S. Guns, N. Gupta, R. Guyser, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, D. Howe, N. Huang, K. D. Irwin, O. B. Jeong, M. Jonas, A. Jones, T. S. Khaire, L. Knox, A. M. Kofman, M. Korman, D. L. Kubik, S. Kuhlmann, C.-L. Kuo, A. T. Lee, E. M. Leitch, A. E. Lowitz, C. Lu, S. S. Meyer, D. Michalik, M. Millea, T. Natoli, H. Nguyen, G. I. Noble, V. Novosad, Y. Omori, S. Padin, Z. Pan, P. Paschos, J. Pearson, C. M. Posada, K. Prabhu, W. Quan, C. L. Reichardt, D. Riebel, B. Riedel, M. Rouble, J. E. Ruhl, B. Saliwanchik, J. T. Sayre, E. Schiappucci, E. Shirokoff, G. Smecher, A. A. Stark, J. Stephen, K. T. Story, A. Suzuki, C. Tandoi, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, L. R. Vale, K. Vanderlinde, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, K. W. Yoon, M. R. Young, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and SPT-3G
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 7. Clean energy, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: SPT-3G is the third survey receiver operating on the South Pole Telescope dedicated to high-resolution observations of the cosmic microwave background (CMB). Sensitive measurements of the temperature and polarization anisotropies of the CMB provide a powerful dataset for constraining cosmology. Additionally, CMB surveys with arcminute-scale resolution are capable of detecting galaxy clusters, millimeter-wave bright galaxies, and a variety of transient phenomena. The SPT-3G instrument provides a significant improvement in mapping speed over its predecessors, SPT-SZ and SPTpol. The broadband optics design of the instrument achieves a 430 mm diameter image plane across observing bands of 95 GHz, 150 GHz, and 220 GHz, with 1.2 arcmin FWHM beam response at 150 GHz. In the receiver, this image plane is populated with 2690 dual-polarization, tri-chroic pixels (~16000 detectors) read out using a 68X digital frequency-domain multiplexing readout system. In 2018, SPT-3G began a multiyear survey of 1500 deg$^{2}$ of the southern sky. We summarize the unique optical, cryogenic, detector, and readout technologies employed in SPT-3G, and we report on the integrated performance of the instrument., Comment: 25 pages, 11 figures. Accepted for publication in ApJS
Published: 2021

9. A second source of repeating fast radio bursts

Author: P. J. Boyle, M. Fandino, J. Mena-Parra, Ue-Li Pen, P. Boubel, M. Rafiei-Ravandi, Laura Newburgh, Mohit Bhardwaj, C. Brar, Shriharsh P. Tendulkar, M. A. Dobbs, Deborah C. Good, Kiyoshi Masui, P. Chawla, C. Höfer, D. Michilli, Kevin Bandura, Emmanuel Fonseca, Ajay Gill, J. R. Shaw, M. Burhanpurkar, M. Deng, Mandana Amiri, C. Patel, A. Renard, M. M. Boyce, P. Yadav, C. Moatti, Bryan Gaensler, A. Josephy, A. Naidu, Scott M. Ransom, Gary Hinshaw, David Hanna, A. Gilbert, I. Tretyakov, Seth Siegel, Nolan Denman, Chime, Alex S. Hill, U. Giri, Keith Vanderlinde, Ziggy Pleunis, T. Cassanelli, Mubdi Rahman, M. Merryfield, Mark Halpern, Ingrid H. Stairs, R. Mckinven, Dustin Lang, D. Cubranic, T. Pinsonneault-Marotte, Hsiu-Hsien Lin, Kendrick M. Smith, J. F. Cliche, Paul Scholz, Victoria M. Kaspi, T. L. Landecker, Cherry Ng, and N. Milutinovic
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Multidisciplinary, 010308 nuclear & particles physics, Fast radio burst, Milky Way, Canadian Hydrogen Intensity Mapping Experiment, media_common.quotation_subject, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, Redshift, Radio telescope, Sky, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, education, Second source, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, media_common
Abstract: The discovery of a repeating Fast Radio Burst (FRB) source, FRB 121102, eliminated models involving cataclysmic events for this source. No other repeating FRB has yet been detected in spite of many recent FRB discoveries and follow-ups, suggesting repeaters may be rare in the FRB population. Here we report the detection of six repeat bursts from FRB 180814.J0422+73, one of the 13 FRBs detected by the Canadian Hydrogen Intensity Mapping Experiment (CHIME) FRB project during its pre-commissioning phase in July and August 2018. These repeat bursts are consistent with originating from a single position on the sky, with the same dispersion measure (DM), ~189 pc cm-3. This DM is approximately twice the expected Milky Way column density, and implies an upper limit on the source redshift of 0.1, at least a factor of ~2 closer than FRB 121102. In some of the repeat bursts, we observe sub-pulse frequency structure, drifting, and spectral variation reminiscent of that seen in FRB 121102, suggesting similar emission mechanisms and/or propagation effects. This second repeater, found among the first few CHIME/FRB discoveries, suggests that there exists -- and that CHIME/FRB and other wide-field, sensitive radio telescopes will find -- a substantial population of repeating FRBs., Comment: accepted by Nature
Published: 2019
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10. Thermal Links and Microstrip Transmission Lines in SPT-3G Bolometers

Author: Peter A. R. Ade, Faustin Carter, K. T. Story, J. S. Avva, Thomas Cecil, S. E. Kuhlmann, Junjia Ding, Gene C. Hilton, K. Vanderlinde, G. I. Noble, W. B. Everett, A. Cukierman, Q. Y. Tang, E. V. Denison, A. E. Lowitz, V. G. Yefremenko, R. N. Gannon, M. R. Young, Carole Tucker, K. L. Thompson, Alexandra S. Rahlin, R. Basu Thakur, Chihway Chang, N. W. Halverson, John E. Carlstrom, Amy N. Bender, J. A. Sobrin, Z. Pan, N. L. Harrington, Jason W. Henning, T. Natoli, Jason E. Austermann, S. S. Meyer, Kent D. Irwin, N. Whitehorn, D. Dutcher, Ralu Divan, Bradford Benson, K. W. Yoon, Graeme Smecher, A. Foster, Donna Kubik, J. F. Cliche, C. L. Kuo, Adrian T. Lee, Valentine Novosad, Andrew Nadolski, Zeeshan Ahmed, Trupti Khaire, Joshua Montgomery, T. de Haan, M. Jonas, A. J. Gilbert, A. A. Stark, W. Holzapfel, Adam Anderson, J. E. Ruhl, John E. Pearson, Leila R. Vale, C. S. Miller, M. A. Dobbs, N. Huang, J. C. Groh, Aritoki Suzuki, H. Nguyen, L. J. Saunders, C. M. Posada, A. M. Kofman, I. Shirley, Daniel Michalik, O. B. Jeong, Gensheng Wang, Joaquin Vieira, Liliana Stan, Erik Shirokoff, Stephen Padin, M. Korman, A. H. Harke-Hosemann, and J. T. Sayre
Subjects: 010302 applied physics, Physics, Physics::Instrumentation and Detectors, business.industry, Cosmic microwave background, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Condensed Matter Physics, 01 natural sciences, Atomic and Molecular Physics, and Optics, Microstrip, Computer Science::Other, law.invention, South Pole Telescope, Optics, law, 0103 physical sciences, Thermal, Dissipation factor, General Materials Science, Transition edge sensor, 010306 general physics, business
Abstract: In this work, we have measured the properties of membrane-suspended bolometer thermal links and microstrip transmission lines in the transition-edge sensor arrays for the third-generation camera for South Pole Telescope (SPT-3G). A promising technique for controlling the end point of the release etch that defines the thermal link has been developed. We have also evaluated the microstrip loss in our detectors by measuring the optical efficiency of detectors with different lengths of microstrip line. The loss tangent is sufficiently low for the use in multi-chronic pixels for cosmic microwave background instruments like SPT-3G.
Published: 2018
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11. Design and Assembly of SPT-3G Cold Readout Hardware

Author: Amy N. Bender, A. Cukierman, D. Dutcher, E. V. Denison, V. G. Yefremenko, C. M. Posada, W. B. Everett, Trupti Khaire, John E. Carlstrom, K. L. Thompson, Joaquin Vieira, Q. Y. Tang, Carole Tucker, Joshua Montgomery, A. E. Lowitz, Z. Pan, Alexandra S. Rahlin, Jason E. Austermann, K. W. Yoon, Graeme Smecher, R. Basu Thakur, Chihway Chang, Valentine Novosad, J. E. Ruhl, Faustin Carter, Leila R. Vale, Y. Hori, K. M. Rotermund, K. Vanderlinde, M. A. Dobbs, Peter A. R. Ade, S. E. Kuhlmann, Junjia Ding, K. T. Story, Oliver Jeong, J. F. Cliche, Kent D. Irwin, Gene C. Hilton, W. L. Holzapfel, M. Korman, A. A. Stark, R. N. Gannon, M. R. Young, Donna Kubik, John E. Pearson, Kaori Hattori, T. Natoli, Gensheng Wang, M. Jonas, Aritoki Suzuki, John Groh, A. J. Gilbert, Jason W. Henning, Tucker Elleflot, C. L. Kuo, A. Foster, Adam Anderson, Zeeshan Ahmed, Thomas Cecil, N. W. Halverson, T. de Haan, L. J. Saunders, J. A. Sobrin, H. Nguyen, Jessica Avva, Nathan Whitehorn, S. S. Meyer, Stephen Padin, Masaya Hasegawa, H. Nishino, A. M. Kofman, I. Shirley, Andrew Nadolski, A. H. Harke-Hosemann, G. I. Noble, Aaron Lee, Erik Shirokoff, N. Huang, J. T. Sayre, D. Barron, N. L. Harrington, and Bradford Benson
Subjects: 010302 applied physics, Physics, business.industry, Detector, Condensed Matter Physics, 01 natural sciences, Atomic and Molecular Physics, and Optics, Resonator, Upgrade, Thermal conductivity, South Pole Telescope, Planar, 0103 physical sciences, Optoelectronics, General Materials Science, 010306 general physics, business, Electrical impedance, Stripline
Abstract: The third-generation upgrade to the receiver on the South Pole Telescope, SPT-3G, was installed at the South Pole during the 2016–2017 austral summer to measure the polarization of the cosmic microwave background. Increasing the number of detectors by a factor of 10 to ∼16,000 \ud ∼16,000\ud required the multiplexing factor to increase to 68 and the bandwidth of the frequency-division readout electronics to span 1.6–5.2 MHz. This increase necessitates low-thermal conductance, low-inductance cryogenic wiring. Our cold readout system consists of planar thin-film aluminum inductive–capacitive resonators, wired in series with the detectors, summed together, and connected to 4K SQUIDs by 10−μm \ud 10−μm\ud -thick niobium–titanium (NbTi) broadside-coupled striplines. Here, we present an overview of the cold readout electronics for SPT-3G, including assembly details and characterization of electrical and thermal properties of the system. We report, for the NbTi striplines, values of R≤10 −4 Ω \ud R≤10−4Ω\ud , L=21±1 nH \ud L=21±1 nH\ud , and C=1.47±.02 nF \ud C=1.47±.02 nF\ud . Additionally, the striplines’ thermal conductivity is described by kA=6.0±0.3 T 0.92±0.04 μW mm K −1 \ud kA=6.0±0.3 T0.92±0.04 μW mm K−1\ud . Finally, we provide projections for cross talk induced by parasitic impedances from the stripline and find that the median value of percentage cross talk from leakage current is 0.22 and 0.09% \ud 0.09%\ud from wiring impedance.
Published: 2018
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12. Fabrication of Detector Arrays for the SPT-3G Receiver

Author: N. W. Halverson, K. Vanderlinde, J. E. Ruhl, Leila R. Vale, C. L. Kuo, M. A. Dobbs, K. L. Thompson, Zeeshan Ahmed, Z. Pan, T. Natoli, Aaron Lee, Peter A. R. Ade, C. M. Posada, Bradford Benson, Jason W. Henning, E. V. Denison, A. Foster, A. E. Lowitz, K. T. Story, Amy N. Bender, V. G. Yefremenko, A. Cukierman, D. Dutcher, T. de Haan, Thomas Cecil, Joaquin Vieira, G. I. Noble, Jason E. Austermann, A. H. Harke-Hosemann, Kent D. Irwin, J. F. Cliche, Valentine Novosad, W. L. Holzapfel, K. W. Yoon, R. N. Gannon, M. R. Young, A. J. Gilbert, Andrew Nadolski, Adam Anderson, N. Huang, Donna Kubik, Graeme Smecher, W. B. Everett, Nathan Whitehorn, Daniel Michalik, Gensheng Wang, John Groh, N. L. Harrington, Q. Y. Tang, M. Jonas, Aritoki Suzuki, J. A. Sobrin, Trupti Khaire, Liliana Stan, S. S. Meyer, Carole Tucker, J. T. Sayre, Joshua Montgomery, Erik Shirokoff, Jessica Avva, I. Shirley, C. S. Miller, Stephen Padin, M. Korman, H. Nguyen, A. M. Kofman, Ralu Divan, L. J. Saunders, John E. Pearson, Alexandra S. Rahlin, R. Basu Thakur, Chihway Chang, A. A. Stark, John E. Carlstrom, Oliver Jeong, Faustin Carter, S. E. Kuhlmann, Junjia Ding, and Gene C. Hilton
Subjects: 010302 applied physics, Physics, business.industry, Detector, Bolometer, Condensed Matter Physics, 01 natural sciences, Multiplexing, Signal, Atomic and Molecular Physics, and Optics, Radio spectrum, law.invention, Cardinal point, Optics, South Pole Telescope, law, 0103 physical sciences, General Materials Science, Antenna (radio), 010306 general physics, business
Abstract: The South Pole Telescope third-generation (SPT-3G) receiver was installed during the austral summer of 2016–2017. It is designed to measure the cosmic microwave background across three frequency bands centered at 95, 150, and 220 GHz. The SPT-3G receiver has ten focal plane modules, each with 269 pixels. Each pixel features a broadband sinuous antenna coupled to a niobium microstrip transmission line. In-line filters define the desired band-passes before the signal is coupled to six bolometers with Ti/Au/Ti/Au transition edge sensors (three bands × \ud ×\ud two polarizations). In total, the SPT-3G receiver is composed of 16,000 detectors, which are read out using a 68× \ud ×\ud frequency-domain multiplexing scheme. In this paper, we present the process employed in fabricating the detector arrays.
Published: 2018
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13. The CHIME Pulsar Project: System Overview

Author: A. Renard, Paul Demorest, Laura Newburgh, B. W. Meyers, J. R. Shaw, A. E. Sikora, Ingrid H. Stairs, T. L. Landecker, M. A. Dobbs, Mandana Amiri, N. T. Denman, Scott M. Ransom, Calvin Leung, Jing Luo, A. Naidu, Cherry Ng, C. Brar, Victoria M. Kaspi, C. M. Tan, K. Vanderlinde, J. W. McKee, I. Tretyakov, H. Wang, Xin Wang, M. Fandino, C. Patel, Hsiu-Hsien Lin, F. Q. Dong, Alex S. Hill, Kiyoshi Masui, C. Höfer, Emmanuel Fonseca, J. F. Cliche, P. J. Boyle, Mark Halpern, Kevin Bandura, D. Cubranic, Daniele Michilli, J. Mena-Parra, Shriharsh P. Tendulkar, P. Scholz, Deborah C. Good, T. Pinsonneault-Marotte, and Kathryn Crowter
Subjects: astronomy data analysis, Physics, astronomical instrumentation, pulsar timing method, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, radio astronomy, 01 natural sciences, Astronomical instrumentation, Pulsar, Space and Planetary Science, 0103 physical sciences, astronomy data acquisition, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), radio pulsars, Radio astronomy
Abstract: We present the design, implementation and performance of a digital backend constructed for the Canadian Hydrogen Intensity Mapping Experiment (CHIME) that uses accelerated computing to observe radio pulsars and transient radio sources. When operating, the CHIME correlator outputs 10 independent streams of beamformed data for the CHIME/Pulsar backend that digitally track specified celestial positions. Each of these independent streams are processed by the CHIME/Pulsar backend system which can coherently dedisperse, in real-time, up to dispersion measure values of 2500 pc/cm$^{-3}$ . The tracking beams and real-time analysis system are autonomously controlled by a priority-based algorithm that schedules both known sources and positions of interest for observation with observing cadences as small as one day. Given the distribution of known pulsars and radio-transient sources, the CHIME/Pulsar system can monitor up to 900 positions once per sidereal day and observe all sources with declinations greater than $-20^\circ$ once every $\sim$2 weeks. We also discuss the science program enabled through the current modes of data acquisition for CHIME/Pulsar that centers on timing and searching experiments., Comment: 18 pages, 9 figures, 1 table. Submitted to ApJS
Published: 2020
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14. Updated design of the CMB polarization experiment satellite LiteBIRD

Author: H. Sugai, P. A. R. Ade, Y. Akiba, D. Alonso, K. Arnold, J. Aumont, J. Austermann, C. Baccigalupi, A. J. Banday, R. Banerji, R. B. Barreiro, S. Basak, J. Beall, S. Beckman, M. Bersanelli, J. Borrill, F. Boulanger, M. L. Brown, M. Bucher, A. Buzzelli, E. Calabrese, F. J. Casas, A. Challinor, V. Chan, Y. Chinone, J.-F. Cliche, F. Columbro, A. Cukierman, D. Curtis, P. Danto, P. de Bernardis, T. de Haan, M. De Petris, C. Dickinson, M. Dobbs, T. Dotani, L. Duband, A. Ducout, S. Duff, A. Duivenvoorden, J.-M. Duval, K. Ebisawa, T. Elleflot, H. Enokida, H. K. Eriksen, J. Errard, T. Essinger-Hileman, F. Finelli, R. Flauger, C. Franceschet, U. Fuskeland, K. Ganga, J.-R. Gao, R. Génova-Santos, T. Ghigna, A. Gomez, M. L. Gradziel, J. Grain, F. Grupp, A. Gruppuso, J. E. Gudmundsson, N. W. Halverson, P. Hargrave, T. Hasebe, M. Hasegawa, M. Hattori, M. Hazumi, S. Henrot-Versille, D. Herranz, C. Hill, G. Hilton, Y. Hirota, E. Hivon, R. Hlozek, D.-T. Hoang, J. Hubmayr, K. Ichiki, T. Iida, H. Imada, K. Ishimura, H. Ishino, G. C. Jaehnig, M. Jones, T. Kaga, S. Kashima, Y. Kataoka, N. Katayama, T. Kawasaki, R. Keskitalo, A. Kibayashi, T. Kikuchi, K. Kimura, T. Kisner, Y. Kobayashi, N. Kogiso, A. Kogut, K. Kohri, E. Komatsu, K. Komatsu, K. Konishi, N. Krachmalnicoff, C. L. Kuo, N. Kurinsky, A. Kushino, M. Kuwata-Gonokami, L. Lamagna, M. Lattanzi, A. T. Lee, E. Linder, B. Maffei, D. Maino, M. Maki, A. Mangilli, E. Martínez-González, S. Masi, R. Mathon, T. Matsumura, A. Mennella, M. Migliaccio, Y. Minami, K. Mistuda, D. Molinari, L. Montier, G. Morgante, B. Mot, Y. Murata, J. A. Murphy, M. Nagai, R. Nagata, S. Nakamura, T. Namikawa, P. Natoli, S. Nerval, T. Nishibori, H. Nishino, Y. Nomura, F. Noviello, C. O’Sullivan, H. Ochi, H. Ogawa, H. Ohsaki, I. Ohta, N. Okada, L. Pagano, A. Paiella, D. Paoletti, G. Patanchon, F. Piacentini, G. Pisano, G. Polenta, D. Poletti, T. Prouvé, G. Puglisi, D. Rambaud, C. Raum, S. Realini, M. Remazeilles, G. Roudil, J. A. Rubiño-Martín, M. Russell, H. Sakurai, Y. Sakurai, M. Sandri, G. Savini, D. Scott, Y. Sekimoto, B. D. Sherwin, K. Shinozaki, M. Shiraishi, P. Shirron, G. Signorelli, G. Smecher, P. Spizzi, S. L. Stever, R. Stompor, S. Sugiyama, A. Suzuki, J. Suzuki, E. Switzer, R. Takaku, H. Takakura, S. Takakura, Y. Takeda, A. Taylor, E. Taylor, Y. Terao, K. L. Thompson, B. Thorne, M. Tomasi, H. Tomida, N. Trappe, M. Tristram, M. Tsuji, M. Tsujimoto, C. Tucker, J. Ullom, S. Uozumi, S. Utsunomiya, J. Van Lanen, G. Vermeulen, P. Vielva, F. Villa, M. Vissers, N. Vittorio, F. Voisin, I. Walker, N. Watanabe, I. Wehus, J. Weller, B. Westbrook, B. Winter, E. Wollack, R. Yamamoto, N. Y. Yamasaki, M. Yanagisawa, T. Yoshida, J. Yumoto, M. Zannoni, A. Zonca, Sugai, H, Ade, P, Akiba, Y, Alonso, D, Arnold, K, Aumont, J, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beckman, S, Bersanelli, M, Borrill, J, Boulanger, F, Brown, M, Bucher, M, Buzzelli, A, Calabrese, E, Casas, F, Challinor, A, Chan, V, Chinone, Y, Cliche, J, Columbro, F, Cukierman, A, Curtis, D, Danto, P, de Bernardis, P, de Haan, T, De Petris, M, Dickinson, C, Dobbs, M, Dotani, T, Duband, L, Ducout, A, Duff, S, Duivenvoorden, A, Duval, J, Ebisawa, K, Elleflot, T, Enokida, H, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Ganga, K, Gao, J, Génova-Santos, R, Ghigna, T, Gomez, A, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, J, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Henrot-Versille, S, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoang, D, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Jones, M, Kaga, T, Kashima, S, Kataoka, Y, Katayama, N, Kawasaki, T, Keskitalo, R, Kibayashi, A, Kikuchi, T, Kimura, K, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kuo, C, Kurinsky, N, Kushino, A, Kuwata-Gonokami, M, Lamagna, L, Lattanzi, M, Lee, A, Linder, E, Maffei, B, Maino, D, Maki, M, Mangilli, A, Martínez-González, E, Masi, S, Mathon, R, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mistuda, K, Molinari, D, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, Nomura, Y, Noviello, F, O’Sullivan, C, Ochi, H, Ogawa, H, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Piacentini, F, Pisano, G, Polenta, G, Poletti, D, Prouvé, T, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Remazeilles, M, Roudil, G, Rubiño-Martín, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Savini, G, Scott, D, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Spizzi, P, Stever, S, Stompor, R, Sugiyama, S, Suzuki, A, Suzuki, J, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takeda, Y, Taylor, A, Taylor, E, Terao, Y, Thompson, K, Thorne, B, Tomasi, M, Tomida, H, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Uozumi, S, Utsunomiya, S, Van Lanen, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Voisin, F, Walker, I, Watanabe, N, Wehus, I, Weller, J, Westbrook, B, Winter, B, Wollack, E, Yamamoto, R, Yamasaki, N, Yanagisawa, M, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, World Premier International Research Center (Japan), Japan Society for the Promotion of Science, Ministry of Education, Culture, Sports, Science and Technology (Japan), Agenzia Spaziale Italiana, Istituto Nazionale di Fisica Nucleare, Centre National D'Etudes Spatiales (France), Centre National de la Recherche Scientifique (France), Commissariat à l'Ènergie Atomique et aux Ènergies Alternatives (France), European Space Agency, Canadian Space Agency, National Aeronautics and Space Administration (US), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Sugai, H. [0000-0001-6501-3871], and Apollo - University of Cambridge Repository
Subjects: Passive cooling, Cosmic Microwave Background, Cosmology, Polarimetry, Instrumentation, Inflation, Cosmic microwave background, cosmic background radiation: polarization, 7. Clean energy, 01 natural sciences, Polarization, General Materials Science, 010303 astronomy & astrophysics, media_common, Physics, Settore FIS/01, Settore FIS/05, Astrophysics::Instrumentation and Methods for Astrophysics, suppression, Condensed Matter Physics, Polarization (waves), Atomic and Molecular Physics, and Optics, Infation, adiabatic, Astrophysics - Instrumentation and Methods for Astrophysics, signature, Astrophysics and Astronomy, media_common.quotation_subject, Lagrangian point, Inflation, Primordial gravitational wave, Satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Noise (electronics), Article, NO, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, noise: thermal, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010308 nuclear & particles physics, Gravitational wave, PE9_14, beam: width, gravitational radiation: primordial, Astronomy, 13. Climate action, Sky, spectral, galaxy, astro-ph.IM
Abstract: H. Sugai, et al., Recent developments of transition-edge sensors (TESs), based on extensive experience in ground-based experiments, have been making the sensor techniques mature enough for their application on future satellite cosmic microwave background (CMB) polarization experiments. LiteBIRD is in the most advanced phase among such future satellites, targeting its launch in Japanese Fiscal Year 2027 (2027FY) with JAXA’s H3 rocket. It will accommodate more than 4000 TESs in focal planes of reflective low-frequency and refractive medium-and-high-frequency telescopes in order to detect a signature imprinted on the CMB by the primordial gravitational waves predicted in cosmic inflation. The total wide frequency coverage between 34 and 448 GHz enables us to extract such weak spiral polarization patterns through the precise subtraction of our Galaxy’s foreground emission by using spectral differences among CMB and foreground signals. Telescopes are cooled down to 5 K for suppressing thermal noise and contain polarization modulators with transmissive half-wave plates at individual apertures for separating sky polarization signals from artificial polarization and for mitigating from instrumental 1/f noise. Passive cooling by using V-grooves supports active cooling with mechanical coolers as well as adiabatic demagnetization refrigerators. Sky observations from the second Sun–Earth Lagrangian point, L2, are planned for 3 years. An international collaboration between Japan, the USA, Canada, and Europe is sharing various roles. In May 2019, the Institute of Space and Astronautical Science, JAXA, selected LiteBIRD as the strategic large mission No. 2., This work was supported by World Premier International Research Center Initiative (WPI), MEXT, Japan, by JSPS Core-to-Core Program, A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian contribution to the LiteBIRD phase A is supported by the Italian Space Agency (ASI Grant No. 2016-24- H.1-2018) and the National Institute for Nuclear Physics (INFN). The French contribution to the LiteBIRD phase A is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifque (CNRS), and by the Commissariat à l’Energie Atomique (CEA). A Concurrent Design Facility study focused on the MHFT and Sub-Kelvin coolers has been led by the European Space Agency (ESA). The Canadian contribution to LiteBIRD is supported by the Canadian Space Agency. The US contribution is supported by NASA Grant no. 80NSSC18K0132
Published: 2020
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15. Concept design of low frequency telescope for CMB B-mode polarization satellite LiteBIRD

Author: Mario G. Lattanzi, Carlo Baccigalupi, François Levrier, J. M. Duval, J. Austermann, M. Brilenkov, B. Thorne, Eiichiro Komatsu, D. Rambaud, T. Nagasaki, Peter Shirron, H. Imada, Nozomu Kogiso, Jeff Van Lanen, H. Takakura, T. Kawasaki, Lionel Duband, Ingunn Kathrine Wehus, Y. Hoshino, Tadayasu Dotani, Enrique Martinez-Gonzalez, Tucker Elleflot, S. Beckman, T. Kaga, Shogo Nakamura, A. Kato, Giorgio Savini, S. Bounissou, S. Mandelli, Peter Charles Hargrave, Francois Boulanger, Julien Grain, S. Realini, Reijo Keskitalo, Bruno Maffei, Y. Nagano, Davide Maino, D. Herman, Michael R. Vissers, B. Mot, R. Banerji, N. Katayama, James A. Beall, Johannes Hubmayr, Tomotake Matsumura, Shugo Oguri, G. Patanchon, S. Basak, S. Takakura, Créidhe O'Sullivan, Massimo Gervasi, Y. Takase, S. Stever, A. Carones, Raphael Flauger, F. J. Casas, T. de Haan, Yasuhiro Murata, T. Prouvé, Douglas Scott, P. Vielva, Toshiya Namikawa, Mayu Tominaga, Yuki Sakurai, Luca Lamagna, Eric Hivon, S. Nerval, Ken Ebisawa, Noriko Y. Yamasaki, Julian Borrill, Shingo Kashima, Hajime Sugai, M. De Petris, R. Nagata, Ted Kisner, D. W. Curtis, A. Mennella, P. de Bernardis, Alexandre E. Adler, Misao Sasaki, Jiansong Gao, Kam Arnold, K. Ganga, T. Ghigna, Kazunori Kohri, Ben Westbrook, R. Aurlien, T. Toda, Yasuhiro Takeda, U. Fuskeland, Alessandro Gruppuso, Giuseppe Puglisi, A. Ritacco, I. Kreykenbohm, C. Leloup, M. A. Dobbs, Jochen Weller, Joel N. Ullom, Chao-Lin Kuo, M. Migliaccio, Charles A. Hill, E. Allys, Nicola Vittorio, T. Yoshida, R. Takaku, Thomas Essinger-Hileman, Alessandro Paiella, J. Aumont, Berend Winter, Junji Yumoto, Yutaka Terao, Aritoki Suzuki, T. Hasebe, Toshiyuki Nishibori, A. Cukierman, P. Campeti, Y. Hirota, Alan J. Kogut, Josquin Errard, S. Sugiyama, L. P. L. Colombo, Anthony Challinor, Yohei Kobayashi, A. Kushino, Gemma Luzzi, Makoto Nagai, M. Sandri, Christopher Raum, Giuseppe D'Alessandro, Masashi Hazumi, Masaya Hasegawa, Renée Hlozek, Silvia Masi, Joseph Seibert, F. Piacentini, J. A. Murphy, Greg Jaehnig, Jose Alberto Rubino-Martin, Davide Poletti, Michael L. Brown, Blake D. Sherwin, Daniela Paoletti, Joshua Montgomery, F. Columbro, Gianluca Morgante, J. Bermejo, M. Tomasi, Haruki Nishino, P. Diego-Palazuelos, Hirokazu Ishino, T. Iida, Kazuhisa Mitsuda, Haruyuki Sakurai, Keith L. Thompson, Javier Cubas, Neil Trappe, Keisuke Shinozaki, Adrian T. Lee, Hiroyuki Ohsaki, Martina Gerbino, D. Herranz, M. Tsuji, Marco Bersanelli, Nadia Dachlythra, M. Russell, E. Gjerløw, Maresuke Shiraishi, E. de la Hoz, Eric V. Linder, Graeme Smecher, Eric R. Switzer, Erminia Calabrese, G. Roudil, Mario Zannoni, T. Maciaszek, L. Pagano, D. Auguste, Frank Grupp, Kosei Ishimura, Fabrizio Villa, Kuniaki Konishi, I. S. Ohta, G. Signorelli, J. Bonis, A. Tartari, Jun-ichi Suzuki, R. B. Barreiro, J. F. Cliche, M. Maki, Douglas H Beck, Ricardo Genova-Santos, A. J. Banday, M. Galloway, T. L. Svalheim, Fabio Finelli, L. A. Montier, H. K. Eriksen, Nicoletta Krachmalnicoff, Karen C. Cheung, Cristian Franceschet, Matthieu Tristram, V. Chan, G. Polenta, Clive Dickinson, N. W. Halverson, Kiyotomo Ichiki, Yuji Chinone, Mathieu Remazeilles, Giampaolo Pisano, Jon E. Gudmundsson, J. Peloton, M. Reinecke, Shannon M. Duff, Carole Tucker, Y. Minanmi, Gene C. Hilton, Martin Bucher, P. A. R. Ade, G. Vermeulen, K. Komatsu, Norio Okada, Thibaut Louis, Sophie Henrot-Versille, Edward J. Wollack, Paolo Natoli, Hideo Ogawa, Jörn Wilms, E. Taylor, Andrea Zonca, Makoto Hattori, Radek Stompor, Masahiro Tsujimoto, Yutaro Sekimoto, Marcin Gradziel, H. Thommesen, Zmuidzinas, Jonas, Sekimoto, Y, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, de Bernardis, P, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Columbro, F, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, J, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Henrot-Versillé, S, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lamagna, L, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minanmi, Y, Mitsuda, K, Montgomery, J, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, O'Sullivan, C, Ogawa, H, Oguri, S, Osaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Pisano, G, Polenta, G, Poletti, D, Prouvé, T, Puglisi, G, Tambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Savini, G, Scott, D, Seibert, J, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stever, S, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Westbrook, B, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique de l'ENS (LPTENS), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Hautes Energies (LPTHE), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National d’Études Spatiales [Paris] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), LiteBIRD, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Laboratoire de Physique Théorique de l'ENS [École Normale Supérieure] (LPTENS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), and Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Aperture, FOS: Physical sciences, 7. Clean energy, cryogenic telescope, law.invention, Cosmic microwave background, Entrance pupil, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Optics, millimeter-wave polarization, space program, Settore FIS/05 - Astronomia e Astrofisica, law, Angular resolution, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Stray light, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Lens (optics), Cardinal point, Astrophysics - Instrumentation and Methods for Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: LiteBIRD has been selected as JAXA's strategic large mission in the 2020s, to observe the cosmic microwave background (CMB) $B$-mode polarization over the full sky at large angular scales. The challenges of LiteBIRD are the wide field-of-view (FoV) and broadband capabilities of millimeter-wave polarization measurements, which are derived from the system requirements. The possible paths of stray light increase with a wider FoV and the far sidelobe knowledge of $-56$ dB is a challenging optical requirement. A crossed-Dragone configuration was chosen for the low frequency telescope (LFT : 34--161 GHz), one of LiteBIRD's onboard telescopes. It has a wide field-of-view ($18^\circ \times 9^\circ$) with an aperture of 400 mm in diameter, corresponding to an angular resolution of about 30 arcminutes around 100 GHz. The focal ratio f/3.0 and the crossing angle of the optical axes of 90$^\circ$ are chosen after an extensive study of the stray light. The primary and secondary reflectors have rectangular shapes with serrations to reduce the diffraction pattern from the edges of the mirrors. The reflectors and structure are made of aluminum to proportionally contract from warm down to the operating temperature at $5\,$K. A 1/4 scaled model of the LFT has been developed to validate the wide field-of-view design and to demonstrate the reduced far sidelobes. A polarization modulation unit (PMU), realized with a half-wave plate (HWP) is placed in front of the aperture stop, the entrance pupil of this system. A large focal plane with approximately 1000 AlMn TES detectors and frequency multiplexing SQUID amplifiers is cooled to 100 mK. The lens and sinuous antennas have broadband capability. Performance specifications of the LFT and an outline of the proposed verification plan are presented., Comment: 21 pages, 14 figures
Published: 2020
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16. A bright millisecond-duration radio burst from a Galactic magnetar

Author: A. Josephy, B. W. Meyers, J. W. Kania, M. Rafiei-Ravandi, Laura Newburgh, Kyung-Hoon Shin, T. Chen, Gary Hinshaw, Hsiu-Hsien Lin, C. Brar, Dallas Wulf, A. V. Zwaniga, J. R. Shaw, T. L. Landecker, B. C. Andersen, A. Cook, Saranjit Singh, Kiyoshi Masui, C. Höfer, D. Michilli, Emmanuel Fonseca, M. M. Boyce, M. Fandino, Rick Smegal, C. Patel, Keith Vanderlinde, Bryan Gaensler, Mubdi Rahman, U. Giri, A. P. Curtin, F. Q. Dong, Ue-Li Pen, Scott M. Ransom, P. Chawla, M. Merryfield, Akanksha Bij, J. Mena-Parra, Kendrick M. Smith, A. Mirhosseini, T. Pinsonneault-Marotte, Kevin Bandura, Calvin Leung, Mohit Bhardwaj, D. Cubranic, M. A. Dobbs, V. M. Kaspi, Brendan M. Quine, J. F. Cliche, Cherry Ng, A. Naidu, Chime, Nolan Denman, T. Cassanelli, N. Milutinovic, Alex S. Hill, A. Renard, C. M. Tan, Mark Halpern, Ziggy Pleunis, Seth Siegel, Paul Scholz, I. Tretyakov, R. Mckinven, D. Z. Li, P. J. Boyle, Pranav Sanghavi, Shriharsh P. Tendulkar, Moritz Münchmeyer, Deborah C. Good, Ingrid H. Stairs, and H. Wang
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Multidisciplinary, 010308 nuclear & particles physics, Fast radio burst, Canadian Hydrogen Intensity Mapping Experiment, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Magnetar, 01 natural sciences, Galaxy, Neutron star, Orders of magnitude (time), 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Radio wave
Abstract: Magnetars are highly magnetized young neutron stars that occasionally produce enormous bursts and flares of X-rays and gamma-rays. Of the approximately thirty magnetars currently known in our Galaxy and Magellanic Clouds, five have exhibited transient radio pulsations. Fast radio bursts (FRBs) are millisecond-duration bursts of radio waves arriving from cosmological distances. Some have been seen to repeat. A leading model for repeating FRBs is that they are extragalactic magnetars, powered by their intense magnetic fields. However, a challenge to this model has been that FRBs must have radio luminosities many orders of magnitude larger than those seen from known Galactic magnetars. Here we report the detection of an extremely intense radio burst from the Galactic magnetar SGR 1935+2154 using the Canadian Hydrogen Intensity Mapping Experiment (CHIME) FRB project. The fluence of this two-component bright radio burst and the estimated distance to SGR 1935+2154 together imply a 400-800 MHz burst energy of $\sim 3 \times 10^{34}$ erg, which is three orders of magnitude brighter than those of any radio-emitting magnetar detected thus far. Such a burst coming from a nearby galaxy would be indistinguishable from a typical FRB. This event thus bridges a large fraction of the radio energy gap between the population of Galactic magnetars and FRBs, strongly supporting the notion that magnetars are the origin of at least some FRBs., Comment: Submitted to Nature. This version: Geocentric arrival time corrected
Published: 2020
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17. Design and Bolometer Characterization of the SPT-3G First-year Focal Plane

Author: Volodymyr Yefremenko, Thomas Cecil, A. E. Lowitz, Jason W. Henning, Ki Won Yoon, Nathan Whitehorn, Valentine Novosad, W. B. Everett, A. M. Kofman, Peter A. R. Ade, K. T. Story, Jason E. Austermann, T. Natoli, M. Korman, Graeme Smecher, Kent D. Irwin, A. Cukierman, N. W. Halverson, W. L. Holzapfel, A. Foster, Donna Kubik, A. H. Harke-Hosemann, Trupti Khaire, H. T. Nguyen, Joshua Montgomery, Q. Y. Tang, Gene C. Hilton, Chao-Lin Kuo, Carole Tucker, J. T. Sayre, N. Huang, Faustin Carter, Erik Shirokoff, A. Gilbert, C. L. Chang, Junjia Ding, J. E. Ruhl, John Groh, Daniel Michalik, Zeeshan Ahmed, Adam Anderson, Gensheng Wang, M. A. Dobbs, Leila R. Vale, Alexandra S. Rahlin, Lauren J. Saunders, Z. Pan, R. Basu Thakur, Amy N. Bender, J. A. Sobrin, C. M. Posada, Steve Kuhlmann, Joaquin Vieira, S. S. Meyer, Aaron Lee, D. Dutcher, I. Shirley, E. V. Denison, Jessica Avva, Keith Vanderlinde, Stephen Padin, John E. Carlstrom, G. I. Noble, John E. Pearson, T. de Haan, R. N. Gannon, Bradford Benson, J. F. Cliche, M. R. Young, Keith L. Thompson, M. Jonas, A. Nadolski, Aritoki Suzuki, N. L. Harrington, Antony A. Stark, and Oliver Jeong
Subjects: Physics::Instrumentation and Detectors, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Multiplexing, law.invention, Optics, law, 0103 physical sciences, General Materials Science, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010302 applied physics, Physics, Pixel, business.industry, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Polarization (waves), Atomic and Molecular Physics, and Optics, Cardinal point, South Pole Telescope, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: During the austral summer of 2016-17, the third-generation camera, SPT-3G, was installed on the South Pole Telescope, increasing the detector count in the focal plane by an order of magnitude relative to the previous generation. Designed to map the polarization of the cosmic microwave background, SPT-3G contains ten 6-in-hexagonal modules of detectors, each with 269 trichroic and dual-polarization pixels, read out using 68x frequency-domain multiplexing. Here we discuss design, assembly, and layout of the modules, as well as early performance characterization of the first-year array, including yield and detector properties., Conference proceeding for Low Temperature Detectors 2017. Accepted for publication: 27 August 2018
Published: 2019

18. Broadband, millimeter-wave antireflection coatings for large-format, cryogenic aluminum oxide optics

Author: N. Huang, W. L. Holzapfel, W. B. Everett, Jason Gallicchio, Z. Ahmed, A. E. Gambrel, Marion Dierickx, J. A. Sobrin, Jason W. Henning, T. de Haan, S. S. Meyer, A. Suzuki, Joaquin Vieira, D. Dutcher, S. Guns, K. W. Yoon, J. Stephen, Graeme Smecher, K. Vanderlinde, Andrew Nadolski, Aled Jones, Lincoln Bryant, Valentine Novosad, J. C. Groh, D. Howe, C. M. Po sada, H. Nguyen, J. Fu, A. H. Harke-Hosemann, T. Natoli, Faustin Carter, L. Florez, John M Kovac, A. Foster, J. T. Sayre, Thomas Cecil, Erik Shirokoff, A. Lowitz, Antony A. Stark, P. Paschos, S. E. Kuhlmann, Junjia Ding, C. L. Kuo, Kent D. Irwin, J. E. Ruhl, A. M. Kofman, Daniel Michalik, K. R. Ferguson, C. Tucker, J. Cheshire, Adam Anderson, M. R. Young, Grace E. Chesmore, Gensheng Wang, M. Korman, Donna Kubik, V. G. Yefremenko, W. Quan, S. Padin, J. F. Cliche, Jeff McMahon, John E. Pearson, J. Meier, Jessica Avva, A. Cukierman, R. Guyser, Andreas Bender, G. I. Noble, M. Jonas, C. Tandoi, N. W. Halverson, Peter A. R. Ade, R. J. Harris, K. T. Story, Bradford Benson, Nathan Whitehorn, N. L. Harrington, Joshua Montgomery, D. Riebel, K. L. Thompson, Z. Pan, Oliver Jeong, Robert Gardner, John E. Carlstrom, J. Farwick, Adrian T. Lee, Alexandra S. Rahlin, R. Basu Thakur, and Chihway Chang
Subjects: Physics - Instrumentation and Detectors, Materials science, Fabrication, Oxide, FOS: Physical sciences, Dielectric, Substrate (electronics), Lenslet, engineering.material, 01 natural sciences, 010309 optics, chemistry.chemical_compound, Optics, Coating, 0103 physical sciences, Transmittance, Electrical and Electronic Engineering, Engineering (miscellaneous), Instrumentation and Methods for Astrophysics (astro-ph.IM), business.industry, Instrumentation and Detectors (physics.ins-det), Atomic and Molecular Physics, and Optics, chemistry, engineering, Astrophysics - Instrumentation and Methods for Astrophysics, business, Refractive index
Abstract: We present two prescriptions for broadband (~77 - 252 GHz), millimeter-wave antireflection coatings for cryogenic, sintered polycrystalline aluminum oxide optics: one for large-format (700 mm diameter) planar and plano-convex elements, the other for densely packed arrays of quasi-optical elements, in our case 5 mm diameter half-spheres (called "lenslets"). The coatings comprise three layers of commercially-available, polytetrafluoroethylene-based, dielectric sheet material. The lenslet coating is molded to fit the 150 mm diameter arrays directly while the large-diameter lenses are coated using a tiled approach. We review the fabrication processes for both prescriptions then discuss laboratory measurements of their transmittance and reflectance. In addition, we present the inferred refractive indices and loss tangents for the coating materials and the aluminum oxide substrate. We find that at 150 GHz and 300 K the large-format coating sample achieves (97 +/- 2)% transmittance and the lenslet coating sample achieves (94 +/- 3)% transmittance., Comment: 19 pages, 11 figures; submitted 05 Dec 2019, accepted 26 Feb 2020
Published: 2019
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19. Tuning SPT-3G transition-edge-sensor electrical properties with a four-ayer Ti–Au–Ti–Au thin-film stack

Author: T. de Haan, A. Cukierman, P. A. R. Ade, Daniel Michalik, W. B. Everett, Gensheng Wang, Trupti Khaire, C. L. Kuo, Joshua Montgomery, Andrew Nadolski, Zeeshan Ahmed, Amy N. Bender, V. Kutepova, C. S. Miller, Q. Y. Tang, K. T. Story, N. L. Harrington, Liliana Stan, D. Dutcher, A. J. Gilbert, Adam Anderson, John E. Pearson, Jessica Avva, Carole Tucker, Bradford Benson, Erik Shirokoff, Stephen Padin, N. W. Halverson, Nathan Whitehorn, Kent D. Irwin, C. M. Posada, W. L. Holzapfel, J. F. Cliche, Aaron Lee, Joaquin Vieira, J. A. Sobrin, Donna Kubik, H. Nguyen, Jason E. Austermann, S. S. Meyer, A. H. Harke-Hosemann, A. E. Lowitz, I. Shirley, J. T. Sayre, L. J. Saunders, K. W. Yoon, A. M. Kofman, Graeme Smecher, N. Huang, G. I. Noble, M. Jonas, Aritoki Suzuki, M. Korman, Alexandra S. Rahlin, R. Basu Thakur, Chihway Chang, K. Vanderlinde, Jason W. Henning, R. N. Gannon, M. R. Young, John E. Carlstrom, Oliver Jeong, A. A. Stark, Thomas Cecil, T. Natoli, A. Foster, V. Novosad, John Groh, J. E. Ruhl, Leila R. Vale, M. A. Dobbs, K. L. Thompson, Z. Pan, Faustin Carter, S. E. Kuhlmann, Junjia Ding, Gene C. Hilton, E. V. Denison, V. G. Yefremenko, and Ralu Divan
Subjects: Superconductivity, Materials science, business.industry, Transition temperature, 02 engineering and technology, Substrate (electronics), 021001 nanoscience & nanotechnology, Condensed Matter Physics, 01 natural sciences, Atomic and Molecular Physics, and Optics, Stack (abstract data type), 0103 physical sciences, Proximity effect (audio), Optoelectronics, General Materials Science, Thin film, Transition edge sensor, 010306 general physics, 0210 nano-technology, business, Layer (electronics)
Abstract: We have developed superconducting Ti transition-edge sensors with Au protection layers on the top and bottom for the South Pole Telescope’s third-generation receiver (a cosmic microwave background polarimeter, due to be upgraded this austral summer of 2017/2018). The base Au layer (deposited on a thin Ti glue layer) isolates the Ti from any substrate effects; the top Au layer protects the Ti from oxidation during processing and subsequent use of the sensors. We control the transition temperature and normal resistance of the sensors by varying the sensor width and the relative thicknesses of the Ti and Au layers. The transition temperature is roughly six times more sensitive to the thickness of the base Au layer than to that of the top Au layer. The normal resistance is inversely proportional to sensor width for any given film configuration. For widths greater than five micrometers, the critical temperature is independent of width.
Published: 2018

20. SPT-3G: a multichroic receiver for the South Pole Telescope

Author: N. Kuklev, H. M. Cho, Faustin Carter, Junjia Ding, Gene C. Hilton, E. V. Denison, N. Huang, V. G. Yefremenko, Christian L. Reichardt, Peter S. Barry, K. L. Thompson, Alexandra S. Rahlin, Z. Pan, Gilbert Holder, A. A. Stark, N. W. Halverson, T. de Haan, R. Basu Thakur, Chihway Chang, Kent D. Irwin, N. L. Harrington, John Groh, W. L. Holzapfel, Q. Y. Tang, Jessica Avva, A. Cukierman, John E. Carlstrom, Donna Kubik, T. Natoli, A. E. Lowitz, John E. Pearson, Stephen Padin, Bradford Benson, J. E. Ruhl, Jason W. Henning, W. B. Everett, Carole Tucker, Leila R. Vale, A. Foster, Daniel Michalik, Thomas Cecil, Gensheng Wang, Jason E. Austermann, Valentine Novosad, J. A. Sobrin, K. W. Yoon, Oliver Jeong, H. Nguyen, Graeme Smecher, Lindsey Bleem, Amy N. Bender, S. S. Meyer, R. N. Gannon, Karen Byrum, L. J. Saunders, J. F. Cliche, D. Dutcher, C. M. Posada, M. R. Young, K. Vanderlinde, I. Shirley, Steve Kuhlmann, Matt Dobbs, Joaquin Vieira, Lloyd Knox, G. I. Noble, A. M. Kofman, C. L. Kuo, T. M. Crawford, M. Jonas, Aritoki Suzuki, Zeeshan Ahmed, Peter A. R. Ade, K. T. Story, Nathan Whitehorn, Trupti Khaire, Joshua Montgomery, A. J. Gilbert, Adam Anderson, J. T. Sayre, A. H. Harke-Hosemann, E. M. Leitch, M. Korman, Erik Shirokoff, Aaron Lee, and Andrew Nadolski
Subjects: Physics, Gravitational wave, Cosmic microwave background, Detector, Polarimetry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Condensed Matter Physics, 01 natural sciences, Multiplexing, Atomic and Molecular Physics, and Optics, South Pole Telescope, Gravitational lens, 0103 physical sciences, General Materials Science, 010306 general physics, 010303 astronomy & astrophysics, Galaxy cluster
Abstract: A new receiver for the South Pole Telescope, SPT-3G, was deployed in early 2017 to map the cosmic microwave background at 95, 150, and 220 GHz with ∼ \ud ∼\ud 16,000 detectors, 10 times more than its predecessor SPTpol. The increase in detector count is made possible by lenslet-coupled trichroic polarization-sensitive pixels fabricated at Argonne National Laboratory, new 68× \ud ×\ud frequency-domain multiplexing readout electronics, and a higher-throughput optical design. The enhanced sensitivity of SPT-3G will enable a wide range of results including constraints on primordial B-mode polarization, measurements of gravitational lensing of the CMB, and a galaxy cluster survey. Here we present an overview of the instrument and its science objectives, highlighting its measured performance and plans for the upcoming 2018 observing season.
Published: 2018

21. Optical characterization of the SPT-3G camera

Author: J. A. Sobrin, Leila R. Vale, S. S. Meyer, Matt Dobbs, Volodymyr Yefremenko, Ki Won Yoon, V. Novosad, I. Shirley, Faustin Carter, N. Huang, M. Jonas, Aritoki Suzuki, Erik Shirokoff, John E. Pearson, S. E. Kuhlmann, Junjia Ding, Daniel Michalik, Gene C. Hilton, E. V. Denison, Jason W. Henning, J. F. Cliche, Gensheng Wang, Alexandra S. Rahlin, T. Natoli, J. E. Ruhl, R. Basu Thakur, Chihway Chang, Zeeshan Ahmed, A. E. Lowitz, Kent D. Irwin, W. L. Holzapfel, T. de Haan, A. Foster, N. W. Halverson, Chao-Lin Kuo, A. H. Harke-Hosemann, H. Nguyen, K. Vanderlinde, Donna Kubik, W. B. Everett, Keith L. Thompson, Thomas Cecil, Jessica Avva, L. J. Saunders, Stephen Padin, Oliver Jeong, A. M. Kofman, John E. Carlstrom, C. M. Posada, Ari Cukierman, Joaquin Vieira, Q. Y. Tang, M. Korman, John Groh, Z. Pan, Carole Tucker, R. N. Gannon, M. R. Young, Amy N. Bender, Andrew Nadolski, Jason E. Austermann, Graeme Smecher, D. Dutcher, J. T. Sayre, G. I. Noble, N. L. Harrington, Antony A. Stark, Bradford Benson, A. J. Gilbert, Adam Anderson, Trupti Khaire, Joshua Montgomery, Peter A. R. Ade, K. T. Story, Nathan Whitehorn, and Adrian T. Lee
Subjects: Physics, business.industry, Frequency band, Physics::Instrumentation and Detectors, Cosmic microwave background, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Polarization (waves), 01 natural sciences, 7. Clean energy, Atomic and Molecular Physics, and Optics, Fourier transform spectroscopy, law.invention, 010309 optics, Optics, South Pole Telescope, law, 0103 physical sciences, General Materials Science, Transition edge sensor, 010306 general physics, business
Abstract: The third-generation South Pole Telescope camera is designed to measure the cosmic microwave background across three frequency bands (centered at 95, 150 and 220 GHz) with ∼ \ud ∼\ud 16,000 transition-edge sensor (TES) bolometers. Each multichroic array element on a detector wafer has a broadband sinuous antenna that couples power to six TESs, one for each of the three observing bands and both polarizations, via lumped element filters. Ten detector wafers populate the detector array, which is coupled to the sky via a large-aperture optical system. Here we present the frequency band characterization with Fourier transform spectroscopy, measurements of optical time constants, beam properties, and optical and polarization efficiencies of the detector array. The detectors have frequency bands consistent with our simulations and have high average optical efficiency which is 86, 77 and 66% for the 95, 150 and 220 GHz detectors. The time constants of the detectors are mostly between 0.5 and 5 ms. The beam is round with the correct size, and the polarization efficiency is more than 90% for most of the bolometers.
Published: 2018

22. Design and characterization of the SPT-3G receiver

Author: A. E. Lowitz, Adrian T. Lee, T. de Haan, Carole Tucker, Keith L. Thompson, Kent D. Irwin, T. Natoli, J. E. Ruhl, W. B. Everett, Antony A. Stark, W. L. Holzapfel, K. Vanderlinde, Andrew Nadolski, V. Novosad, Matt Dobbs, A. J. Gilbert, Adam Anderson, Donna Kubik, Bradford Benson, Peter A. R. Ade, A. Foster, J. T. Sayre, K. T. Story, J. F. Cliche, Amy N. Bender, G. I. Noble, Volodymyr Yefremenko, Ari Cukierman, A. M. Kofman, D. Dutcher, M. Jonas, Ki Won Yoon, Nathan Whitehorn, Thomas Cecil, Aritoki Suzuki, Graeme Smecher, N. W. Halverson, C. L. Chang, Jason W. Henning, Zeeshan Ahmed, Erik Shirokoff, Trupti Khaire, N. Huang, Joshua Montgomery, M. R. Young, A. H. Harke-Hosemann, N. L. Harrington, H. T. Nguyen, M. Korman, J. A. Sobrin, Chao-Lin Kuo, Alexandra S. Rahlin, John Groh, R. Basu Thakur, S. S. Meyer, Z. Pan, Faustin Carter, Junjia Ding, Oliver Jeong, John E. Carlstrom, Daniel Michalik, Gensheng Wang, J. Gallichio, John E. Pearson, W. Quan, Jessica Avva, Stephen Padin, C. M. Posada, Steve Kuhlmann, Joaquin Vieira, and S. Guns
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics - Instrumentation and Detectors, Computer science, Physics::Instrumentation and Detectors, Cosmic microwave background, FOS: Physical sciences, Design elements and principles, 02 engineering and technology, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Electronic engineering, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Throughput (business), Astroparticle physics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), 021001 nanoscience & nanotechnology, Characterization (materials science), South Pole Telescope, 0210 nano-technology, Astrophysics - Instrumentation and Methods for Astrophysics, Sensitivity (electronics), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The SPT-3G receiver was commissioned in early 2017 on the 10-meter South Pole Telescope (SPT) to map anisotropies in the cosmic microwave background (CMB). New optics, detector, and readout technologies have yielded a multichroic, high-resolution, low-noise camera with impressive throughput and sensitivity, offering the potential to improve our understanding of inflationary physics, astroparticle physics, and growth of structure. We highlight several key features and design principles of the new receiver, and summarize its performance to date., Conference Presentation at SPIE Astronomical Telescopes + Instrumentation 2018, conference 10708
Published: 2018

23. Year two instrument status of the SPT-3G cosmic microwave background receiver

Author: J. C. Groh, Chao-Lin Kuo, Christian L. Reichardt, V. Novosad, N. W. Halverson, Thomas Cecil, A. E. Lowitz, C. M. Posada, A. J. Gilbert, Aled Jones, Adam Anderson, Joaquin Vieira, S. Guns, Ki Won Yoon, N. Huang, Jason Gallicchio, K. Aylor, John E. Carlstrom, Matt Dobbs, Faustin Carter, Erik Shirokoff, H. Nguyen, S. E. Kuhlmann, T. M. Crawford, Srinivasan Raghunathan, Jessica Avva, Junjia Ding, Gene C. Hilton, Kent D. Irwin, Stephen Padin, A. H. Harke-Hosemann, T. de Haan, T. Natoli, G. I. Noble, W. L. Holzapfel, A. M. Kofman, Daniel Michalik, Volodymyr Yefremenko, W. L. K. Wu, W. B. Everett, H-M. Cho, Donna Kubik, Gensheng Wang, E. M. Leitch, L. S. Bleem, A. Foster, J. E. Ruhl, Jason W. Henning, M. Korman, Keith L. Thompson, W. Quan, J. A. Sobrin, Karen Byrum, S. S. Meyer, Amy N. Bender, Ari Cukierman, Andrew Nadolski, D. Dutcher, E. V. Denison, Peter S. Barry, J. F. Cliche, Zeeshan Ahmed, Antony A. Stark, K. Vanderlinde, N. L. Harrington, L. R. Vale, John E. Pearson, Z. Pan, Peter A. R. Ade, Sebastian Bocquet, M. Jonas, Bradford Benson, K. T. Story, Aritoki Suzuki, Oliver Jeong, Alexandra S. Rahlin, Scott Dodelson, Nathan Whitehorn, R. Basu Thakur, Chihway Chang, Carole Tucker, Trupti Khaire, Joshua Montgomery, Graeme Smecher, Adrian T. Lee, Lloyd Knox, Gilbert Holder, M. R. Young, and J. T. Sayre
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, High Energy Physics - Experiment, Telescope, High Energy Physics - Experiment (hep-ex), law, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Physics, Gravitational wave, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Polarization (waves), South Pole Telescope, 13. Climate action, Sky, Neutrino, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The South Pole Telescope (SPT) is a millimeter-wavelength telescope designed for high-precision measurements of the cosmic microwave background (CMB). The SPT measures both the temperature and polarization of the CMB with a large aperture, resulting in high resolution maps sensitive to signals across a wide range of angular scales on the sky. With these data, the SPT has the potential to make a broad range of cosmological measurements. These include constraining the effect of massive neutrinos on large-scale structure formation as well as cleaning galactic and cosmological foregrounds from CMB polarization data in future searches for inflationary gravitational waves. The SPT began observing in January 2017 with a new receiver (SPT-3G) containing $\sim$16,000 polarization-sensitive transition-edge sensor bolometers. Several key technology developments have enabled this large-format focal plane, including advances in detectors, readout electronics, and large millimeter-wavelength optics. We discuss the implementation of these technologies in the SPT-3G receiver as well as the challenges they presented. In late 2017 the implementations of all three of these technologies were modified to optimize total performance. Here, we present the current instrument status of the SPT-3G receiver., 21 pages, 9 Figures, Presented at SPIE Astronomical Telescopes + Instrumentation 2018
Published: 2018

24. Characterization and performance of the second-year SPT-3G focal plane

Author: Thomas Cecil, John E. Carlstrom, M. Korman, J. A. Sobrin, A. J. Gilbert, N. Huang, T. de Haan, Oliver Jeong, Adam Anderson, Ki Won Yoon, S. S. Meyer, N. L. Harrington, J. T. Sayre, Keith L. Thompson, Jason W. Henning, Carole Tucker, Trupti Khaire, Joshua Montgomery, John E. Pearson, A. E. Lowitz, M. Jonas, Bradford Benson, Andrew Nadolski, Ari Cukierman, Aritoki Suzuki, Erik Shirokoff, Peter A. R. Ade, Amy N. Bender, Chao-Lin Kuo, K. T. Story, Jason Gallicchio, D. Dutcher, M. R. Young, A. H. Harke-Hosemann, T. Natoli, Z. Pan, W. B. Everett, Kent D. Irwin, W. L. Holzapfel, J. E. Ruhl, John Groh, K. Vanderlinde, Nathan Whitehorn, A. Foster, Donna Kubik, Graeme Smecher, V. Novosad, J. F. Cliche, Alexandra S. Rahlin, R. Basu Thakur, Chihway Chang, Zeeshan Ahmed, Faustin Carter, H. Nguyen, Adrian T. Lee, S. E. Kuhlmann, Junjia Ding, A. M. Kofman, C. M. Posada, Joaquin Vieira, S. Guns, Volodymyr Yefremenko, N. W. Halverson, Jessica Avva, Stephen Padin, Daniel Michalik, Gensheng Wang, W. Quan, Matt Dobbs, Antony A. Stark, and G. I. Noble
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics::Instrumentation and Detectors, FOS: Physical sciences, 02 engineering and technology, 01 natural sciences, Microstrip, law.invention, Telescope, Optics, law, 0103 physical sciences, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Pixel, Linear polarization, business.industry, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, South Pole Telescope, Cardinal point, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, business, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The third-generation instrument for the 10-meter South Pole Telescope, SPT-3G, was first installed in January 2017. In addition to completely new cryostats, secondary telescope optics, and readout electronics, the number of detectors in the focal plane has increased by an order of magnitude from previous instruments to ~16,000. The SPT-3G focal plane consists of ten detector modules, each with an array of 269 trichroic, polarization-sensitive pixels on a six-inch silicon wafer. Within each pixel is a broadband, dual-polarization sinuous antenna; the signal from each orthogonal linear polarization is divided into three frequency bands centered at 95, 150, and 220 GHz by in-line lumped element filters and transmitted via superconducting microstrip to Ti/Au transition-edge sensor (TES) bolometers. Properties of the TES film, microstrip filters, and bolometer island must be tightly controlled to achieve optimal performance. For the second year of SPT-3G operation, we have replaced all ten wafers in the focal plane with new detector arrays tuned to increase mapping speed and improve overall performance. Here we discuss the TES superconducting transition temperature and normal resistance, detector saturation power, bandpasses, optical efficiency, and full array yield for the 2018 focal plane., Comment: 13 pages, 11 figures
Published: 2018
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25. Low Loss Superconducting Microstrip Development at Argonne National Lab

Author: A. Cukierman, Benjamin Saliwanchik, Gilbert Holder, V. Yefremenko, Steven W. Allen, Aritoki Suzuki, Jason E. Austermann, Erik Shirokoff, Graeme Smecher, C. Tucker, Kam Arnold, Lloyd Knox, Kent D. Irwin, Alexey Vikhlinin, W. L. Holzapfel, Michael McDonald, Ryan Keisler, Jason W. Henning, C. Posada Arbelaez, Donna Kubik, Bradford Benson, N. W. Halverson, M. J. Myers, D. Hanson, P. A. R. Ade, W. B. Everett, Ki Won Yoon, A. J. Gilbert, Amy N. Bender, D. Dutcher, E. M. Leitch, N. L. Harrington, J. F. Cliche, H. Nguyen, Dale Li, K. Vanderlinde, H. M. Cho, Joshua Montgomery, T. M. Crawford, K. T. Story, T. Natoli, J. T. Sayre, G. Simard, Chihway Chang, Lindsey Bleem, C. L. Kuo, Zeeshan Ahmed, Christian L. Reichardt, S. S. Meyer, Kaori Hattori, V. Novosad, Aaron Lee, A. A. Stark, John E. Carlstrom, T. de Haan, J. E. Ruhl, S. T. Ciocys, M. A. Dobbs, Junjia Ding, Gene C. Hilton, K. L. Thompson, Z. Pan, G. Wang, John E. Pearson, Stephen Padin, Joaquin Vieira, and J. Hubmayr
Subjects: Physics, Fabrication, Condensed matter physics, Physics::Instrumentation and Detectors, business.industry, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Microstrip, Computer Science::Other, Electronic, Optical and Magnetic Materials, law.invention, Resonator, law, Dissipation factor, Optoelectronics, Dielectric loss, Electrical and Electronic Engineering, Transition edge sensor, business
Abstract: Low loss superconducting microstrip is an essential component in realizing 100 kilo-pixel multichroic cosmic microwave background detector arrays. We have been developing a low loss microstrip by understanding and controlling the loss mechanisms. We present the fabrication of the superconducting microstrip, the loss measurements at a few GHz frequencies using half-wavelength resonators, and the loss measurements at 220 GHz frequencies with the superconducting microstrip coupled to slot antennas at one end and to TES detectors at the other end. The measured loss tangent of the microstrip made of sputtered Nb and SiOx is 1-2e-3.
Published: 2015
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26. The CHIME Fast Radio Burst Project: System Overview

Author: A. Josephy, Bryan Gaensler, T. L. Landecker, Scott M. Ransom, M. Fandino, E. Fonseca, Laura Newburgh, A. Naidu, M. M. Boyce, K. Vanderlinde, S. R. Siegel, P. J. Boyle, S. P. Tendulkar, Cherry Ng, D. V. Wiebe, Charanjot Brar, Ziggy Pleunis, H. Liao, Kendrick M. Smith, A. Renard, M. Dobbs, Kris Sigurdson, Victoria M. Kaspi, Ingrid H. Stairs, C. Höfer, M. Rafiei Ravandi, M. Amiri, Ue-Li Pen, Philippe Berger, M. Burhanpurkar, Gary Hinshaw, J. Mena-Parra, S. Guliani, T. Pinsonneault-Marotte, Mohit Bhardwaj, J. F. Cliche, A. J. Gilbert, J. Chowdhury, M. Deng, Kevin Bandura, Mark Halpern, D. Cubranic, D. Lang, Miles Cranmer, P. Scholz, Kiyoshi Masui, N. Denman, P. Chawla, C. Patel, Utkarsh Giri, and Deborah C. Good
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Fast radio burst, Canadian Hydrogen Intensity Mapping Experiment, Real-time computing, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Methods observational, Space and Planetary Science, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is a novel transit radio telescope operating across the 400-800-MHz band. CHIME is comprised of four 20-m x 100-m semi-cylindrical paraboloid reflectors, each of which has 256 dual-polarization feeds suspended along its axis, giving it a >200 square degree field-of-view. This, combined with wide bandwidth, high sensitivity, and a powerful correlator makes CHIME an excellent instrument for the detection of Fast Radio Bursts (FRBs). The CHIME Fast Radio Burst Project (CHIME/FRB) will search beam-formed, high time-and frequency-resolution data in real time for FRBs in the CHIME field-of-view. Here we describe the CHIME/FRB backend, including the real-time FRB search and detection software pipeline as well as the planned offline analyses. We estimate a CHIME/FRB detection rate of 2-42 FRBs/sky/day normalizing to the rate estimated at 1.4-GHz by Vander Wiel et al. (2016). Likely science outcomes of CHIME/FRB are also discussed. CHIME/FRB is currently operational in a commissioning phase, with science operations expected to commence in the latter half of 2018., 27 pages, submitted to ApJ
Published: 2018
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27. Broadband anti-reflective coatings for cosmic microwave background experiments

Author: J. Gallichio, Amy N. Bender, John E. Pearson, D. Dutcher, C. M. Posada, Volodymyr Yefremenko, Joaquin Vieira, S. Guns, V. Novosad, Ki Won Yoon, W. B. Everett, Daniel Michalik, Antony A. Stark, Gensheng Wang, Carole Tucker, G. I. Noble, W. Quan, K. Vanderlinde, Aled Jones, A. E. Lowitz, Kent D. Irwin, Z. Pan, W. L. Holzapfel, John E. Carlstrom, T. de Haan, Peter A. R. Ade, Donna Kubik, Matt Dobbs, Jason W. Henning, T. Natoli, Chao-Lin Kuo, A. J. Gilbert, K. T. Story, Jessica Avva, Adam Anderson, R. Guyser, Stephen Padin, Faustin Carter, John Groh, Alexandra S. Rahlin, S. E. Kuhlmann, Junjia Ding, N. W. Halverson, R. Basu Thakur, Chihway Chang, Keith L. Thompson, Oliver Jeong, Graeme Smecher, A. Foster, Thomas Cecil, M. Jonas, Aritoki Suzuki, Andrew Nadolski, J. F. Cliche, N. Huang, Nathan Whitehorn, Ari Cukierman, M. R. Young, J. A. Sobrin, S. S. Meyer, Trupti Khaire, Joshua Montgomery, J. E. Ruhl, J. T. Sayre, Zeeshan Ahmed, Adrian T. Lee, Erik Shirokoff, H. Nguyen, J. Fu, A. M. Kofman, A. H. Harke-Hosemann, N. L. Harrington, M. Korman, and Bradford Benson
Subjects: Physics - Instrumentation and Detectors, Materials science, Cosmic microwave background, FOS: Physical sciences, 02 engineering and technology, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, engineering.material, 01 natural sciences, law.invention, Optics, Coating, law, 0103 physical sciences, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), 021001 nanoscience & nanotechnology, Cardinal point, South Pole Telescope, Anti-reflective coating, Extremely high frequency, engineering, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, business
Abstract: The desire for higher sensitivity has driven ground-based cosmic microwave background (CMB) experiments to employ ever larger focal planes, which in turn require larger reimaging optics. Practical limits to the maximum size of these optics motivates the development of quasi-optically-coupled (lenslet-coupled), multi-chroic detectors. These detectors can be sensitive across a broader bandwidth compared to waveguide-coupled detectors. However, the increase in bandwidth comes at a cost: the lenses (up to $\sim$700 mm diameter) and lenslets ($\sim$5 mm diameter, hemispherical lenses on the focal plane) used in these systems are made from high-refractive-index materials (such as silicon or amorphous aluminum oxide) that reflect nearly a third of the incident radiation. In order to maximize the faint CMB signal that reaches the detectors, the lenses and lenslets must be coated with an anti-reflective (AR) material. The AR coating must maximize radiation transmission in scientifically interesting bands and be cryogenically stable. Such a coating was developed for the third generation camera, SPT-3G, of the South Pole Telescope (SPT) experiment, but the materials and techniques used in the development are general to AR coatings for mm-wave optics. The three-layer polytetrafluoroethylene-based AR coating is broadband, inexpensive, and can be manufactured with simple tools. The coating is field tested; AR coated focal plane elements were deployed in the 2016-2017 austral summer and AR coated reimaging optics were deployed in 2017-2018., Comment: 13 pages, 5 figures
Published: 2018
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28. Limits on the Ultra-bright Fast Radio Burst Population from the CHIME Pathfinder

Author: Peter Klages, Emilie Storer, Liam Connor, Meiling Deng, R. S. Domagalski, Keith Vanderlinde, S. R. Siegel, T. L. Landecker, M. A. Dobbs, Mandana Amiri, A. Renard, Laura Newburgh, Kris Sigurdson, Philippe Berger, Kiyoshi Masui, A. J. Gilbert, C. Höfer, D. S. Hanna, Deborah C. Good, Mark Halpern, Jeffrey B. Peterson, T. Pinsonneault-Marotte, J. Mena-Parra, Kendrick M. Smith, J. R. Bond, J. F. Cliche, J. R. Shaw, Niels Oppermann, I. Tretyakov, Kevin Bandura, M. Fandino, G. Hsyu, Adam D. Hincks, Ue-Li Pen, Nolan Denman, Gary Hinshaw, D. V. Wiebe, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Fast radio burst, media_common.quotation_subject, Canadian Hydrogen Intensity Mapping Experiment, Population, FOS: Physical sciences, Astronomy and Astrophysics, Field of view, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Power law, Pathfinder, Space and Planetary Science, Sky, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, education, 010303 astronomy & astrophysics, media_common
Abstract: We present results from a new incoherent-beam Fast Radio Burst (FRB) search on the Canadian Hydrogen Intensity Mapping Experiment (CHIME) Pathfinder. Its large instantaneous field of view (FoV) and relative thermal insensitivity allow us to probe the ultra-bright tail of the FRB distribution, and to test a recent claim that this distribution's slope, $\alpha\equiv-\frac{\partial \log N}{\partial \log S}$, is quite small. A 256-input incoherent beamformer was deployed on the CHIME Pathfinder for this purpose. If the FRB distribution were described by a single power-law with $\alpha=0.7$, we would expect an FRB detection every few days, making this the fastest survey on sky at present. We collected 1268 hours of data, amounting to one of the largest exposures of any FRB survey, with over 2.4\,$\times$\,10$^5$\,deg$^2$\,hrs. Having seen no bursts, we have constrained the rate of extremely bright events to $
Published: 2017

29. Optimization of transition edge sensor arrays for cosmic microwave background observations with the South Pole Telescope

Author: Faustin Carter, Junjia Ding, Gene C. Hilton, Jason W. Henning, H. M. Cho, C. S. Miller, Chihway Chang, V. G. Yefremenko, RB Thakur, K. L. Thompson, Z. Pan, E. M. Leitch, A. S. Rahlin, H. Nguyen, K. Vanderlinde, R. N. Gannon, Trupti Khaire, Liliana Stan, J. A. Sobrin, Joshua Montgomery, David A. Czaplewski, Andreas Bender, John E. Carlstrom, Johannes Hubmayr, W. L. K. Wu, Kam Arnold, D. Dutcher, T. Natoli, Erik Shirokoff, Jessica Avva, S. S. Meyer, R. Guyser, Kent D. Irwin, Valentine Novosad, Q. Y. Tang, Stephen Padin, A. J. Gilbert, Christian L. Reichardt, Adam Anderson, A. Cukierman, T. de Haan, Lindsey Bleem, Aritoki Suzuki, W. L. Holzapfel, I. Shirley, Gensheng Wang, Donna Kubik, W. B. Everett, Kaori Hattori, J. T. Sayre, Peter A. R. Ade, A. A. Stark, Carole Tucker, Ki Won Yoon, K. T. Story, N. W. Halverson, J. E. Ruhl, C. L. Kuo, C. M. Posada, Andrew Nadolski, M. A. Dobbs, Zeeshan Ahmed, J. F. Cliche, Joaquin Vieira, Nathan Whitehorn, Jason E. Austermann, John E. Pearson, Benjamin Saliwanchik, Oliver Jeong, Graeme Smecher, Ralu Divan, Karen Byrum, N. L. Harrington, Bradford Benson, N. Huang, Jamil A. Shariff, and Aaron Lee
Subjects: cosmic microwave background, General Physics, Physics::Instrumentation and Detectors, Cosmic microwave background, 02 engineering and technology, Dielectric, 01 natural sciences, 7. Clean energy, law.invention, Optics, Thermal conductivity, superconducting detectors, law, 0103 physical sciences, Electrical and Electronic Engineering, 010306 general physics, QB, Physics, Transition edge sensors, business.industry, Detector, Bolometer, South Pole telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Materials Engineering, 021001 nanoscience & nanotechnology, Condensed Matter Physics, Polarization (waves), Electronic, Optical and Magnetic Materials, South Pole Telescope, Transition edge sensor, 0210 nano-technology, business, bolometers
Abstract: © 2002-2011 IEEE. In this paper, we describe the optimization of transition-edge-sensor (TES) detector arrays for the third-generation camera for the South Pole Telescope. The camera, which contains ~ 16 000 detectors, will make high-angular-resolution maps of the temperature and polarization of the cosmic microwave background. Our key results are scatter in the transition temperature of Ti/Au TESs is reduced by fabricating the TESs on a thin Ti(5 nm)/Au(5 nm) buffer layer and the thermal conductivity of the legs that support our detector islands is dominated by the SiOx dielectric in the microstrip transmission lines that run along the legs.
Published: 2017
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30. ICE-Based Custom Full-Mesh Network for the CHIME High Bandwidth Radio Astronomy Correlator

Author: D. Ittah, Kevin Bandura, M. A. Dobbs, J. F. Cliche, Graeme Smecher, A. J. Gilbert, and J. Mena Parra
Subjects: Ethernet, 010308 nuclear & particles physics, business.industry, Computer science, Canadian Hydrogen Intensity Mapping Experiment, Mesh networking, Bandwidth (signal processing), Graphics processing unit, Astronomy and Astrophysics, 01 natural sciences, Data link, 0103 physical sciences, Transceiver, business, Field-programmable gate array, 010303 astronomy & astrophysics, Instrumentation, Computer hardware
Abstract: New generation radio interferometers encode signals from thousands of antenna feeds across large bandwidth. Channelizing and correlating this data requires networking capabilities that can handle unprecedented data rates with reasonable cost. The Canadian Hydrogen Intensity Mapping Experiment (CHIME) correlator processes 8-bits from [Formula: see text] digitizer inputs across 400[Formula: see text]MHz of bandwidth. Measured in [Formula: see text] bandwidth, it is the largest radio correlator that is currently commissioning. Its digital back-end must exchange and reorganize the 6.6[Formula: see text]terabit/s produced by its 128 digitizing and channelizing nodes, and feed it to the 256 graphics processing unit (GPU) node spatial correlator in a way that each node obtains data from all digitizer inputs but across a small fraction of the bandwidth (i.e. ‘corner-turn’). In order to maximize performance and reliability of the corner-turn system while minimizing cost, a custom networking solution has been implemented. The system makes use of Field Programmable Gate Array (FPGA) transceivers to implement direct, passive copper, full-mesh, high speed serial connections between sixteen circuit boards in a crate, to exchange data between crates, and to offload the data to a cluster of 256 GPU nodes using standard 10[Formula: see text]Gbit/s Ethernet links. The GPU nodes complete the corner-turn by combining data from all crates and then computing visibilities. Eye diagrams and frame error counters confirm error-free operation of the corner-turn network in both the currently operating CHIME Pathfinder telescope (a prototype for the full CHIME telescope) and a representative fraction of the full CHIME hardware providing an end-to-end system validation. An analysis of an equivalent corner-turn system built with Ethernet switches instead of custom passive data links is provided.
Published: 2016
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31. ICE: A Scalable, Low-Cost FPGA-Based Telescope Signal Processing and Networking System

Author: J. F. Cliche, Matt Dobbs, T. de Haan, Keith Vanderlinde, Joshua Montgomery, Sinéad M. Griffin, Nathan Whitehorn, D. Ittah, J. Mena Parra, Seth Siegel, Amy N. Bender, G. Hsyu, Graeme Smecher, Q. Y. Tang, Kevin Bandura, T. Pinsonneault-Marotte, and A. Gilbert
Subjects: Signal processing, 010308 nuclear & particles physics, Computer science, business.industry, Emphasis (telecommunications), Astronomy and Astrophysics, Terabyte, 01 natural sciences, Multiplexing, Data acquisition, Gate array, 0103 physical sciences, business, Field-programmable gate array, 010303 astronomy & astrophysics, Instrumentation, Computer hardware, Digital signal processing
Abstract: We present an overview of the ‘ICE’ hardware and software framework that implements large arrays of interconnected field-programmable gate array (FPGA)-based data acquisition, signal processing and networking nodes economically. The system was conceived for application to radio, millimeter and sub-millimeter telescope readout systems that have requirements beyond typical off-the-shelf processing systems, such as careful control of interference signals produced by the digital electronics, and clocking of all elements in the system from a single precise observatory-derived oscillator. A new generation of telescopes operating at these frequency bands and designed with a vastly increased emphasis on digital signal processing to support their detector multiplexing technology or high-bandwidth correlators — data rates exceeding a terabyte per second — are becoming common. The ICE system is built around a custom FPGA motherboard that makes use of an Xilinx Kintex-7 FPGA and ARM-based co-processor. The system is specialized for specific applications through software, firmware and custom mezzanine daughter boards that interface to the FPGA through the industry-standard FPGA mezzanine card (FMC) specifications. For high density applications, the motherboards are packaged in 16-slot crates with ICE backplanes that implement a low-cost passive full-mesh network between the motherboards in a crate, allow high bandwidth interconnection between crates and enable data offload to a computer cluster. A Python-based control software library automatically detects and operates the hardware in the array. Examples of specific telescope applications of the ICE framework are presented, namely the frequency-multiplexed bolometer readout systems used for the South Pole Telescope (SPT) and Simons Array and the digitizer, F-engine, and networking engine for the Canadian Hydrogen Intensity Mapping Experiment (CHIME) and Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX) radio interferometers.
Published: 2016
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32. Integrated performance of a frequency domain multiplexing readout in the SPT-3G receiver

Author: J. T. Sayre, Zeeshan Ahmed, Matt Dobbs, C. L. Chang, W. B. Everett, Trupti Khaire, Joshua Montgomery, V. Novosad, T. M. Crawford, H. Nguyen, Karen Byrum, Jason W. Henning, Peter A. R. Ade, K. T. Story, H. M. Cho, A. J. Gilbert, Alexandra S. Rahlin, J. E. Ruhl, G. Smecher, T. de Haan, Adam Anderson, N. W. Halverson, R. Basu Thakur, Nathan Whitehorn, Kent D. Irwin, J. A. Sobrin, Oliver Jeong, W. L. Holzapfel, David A. Czaplewski, S. S. Meyer, John E. Carlstrom, N. Huang, Erik Shirokoff, Keith L. Thompson, Z. Pan, Volodymyr Yefremenko, Donna Kubik, I. Shirley, Ki Won Yoon, John E. Pearson, Chao-Lin Kuo, Christian L. Reichardt, Ari Cukierman, Faustin Carter, K. Vanderlinde, Kaori Hattori, Amy N. Bender, Andrew Nadolski, Junjia Ding, T. Natoli, M. Korman, Kam Arnold, Gene C. Hilton, John Groh, Antony A. Stark, Sergi Lendinez, J. A. Shariff, D. Dutcher, B. R. Saliwanchik, Lindsey Bleem, N. L. Harrington, Ralu Divan, A. H. Harke-Hosemann, Adrian T. Lee, Bradford Benson, C. S. Miller, E. M. Leitch, C. M. Posada, Joaquin Vieira, J. F. Cliche, Liliana Stan, Jessica Avva, R. Guyser, Stephen Padin, Gensheng Wang, Aritoki Suzuki, Q. Y. Tang, Carole Tucker, and Jason E. Austermann
Subjects: Physics, business.industry, Cosmic microwave background, Bolometer, Bandwidth (signal processing), Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Multiplexing, law.invention, Cardinal point, Optics, South Pole Telescope, Interference (communication), law, 0103 physical sciences, 010306 general physics, business, 010303 astronomy & astrophysics
Abstract: The third generation receiver for the South Pole Telescope, SPT-3G, will make extremely deep, arcminuteresolution maps of the temperature and polarization of the cosmic microwave background. The SPT-3G maps will enable studies of the B-mode polarization signature, constraining primordial gravitational waves as well as the effect of massive neutrinos on structure formation in the late universe. The SPT-3G receiver will achieve exceptional sensitivity through a focal plane of ~16,000 transition-edge sensor bolometers, an order of magnitude more than the current SPTpol receiver. SPT-3G uses a frequency domain multiplexing (fMux) scheme to read out the focal plane, combining the signals from 64 bolometers onto a single pair of wires. The fMux readout facilitates the large number of detectors in the SPT-3G focal plane by limiting the thermal load due to readout wiring on the 250 millikelvin cryogenic stage. A second advantage of the fMux system is that the operation of each bolometer can be optimized. In addition to these benefits, the fMux readout introduces new challenges into the design and operation of the receiver. The bolometers are operated at a range of frequencies up to 5 MHz, requiring control of stray reactances over a large bandwidth. Additionally, crosstalk between multiplexed detectors will inject large false signals into the data if not adequately mitigated. SPT-3G is scheduled to deploy to the South Pole Telescope in late 2016. Here, we present the pre-deployment performance of the fMux readout system with the SPT-3G focal plane.
Published: 2016
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33. Holographic Beam Mapping of the CHIME Pathfinder Array

Author: J. Richard Shaw, Liam Connor, Meiling Deng, Gary Hinshaw, David Hanna, A. Gilbert, Adam D. Hincks, T. L. Landecker, Niels Oppermann, Laura Newburgh, Matt Dobbs, Donald Wiebe, I. Tretyakov, M. Fandino, Juan Mena Parra, Andre M. Johnson, Kiyoshi Masui, Jeffrey B. Peterson, C. Höfer, Kevin Bandura, Philippe Berger, Keith Vanderlinde, Mandana Amiri, Emilie Storer, Nolan Denman, Timothy Robishaw, Ue-Li Pen, Kwinten Van Gassen, Deborah C. Good, Andre Recnik, Kris Sigurdson, Seth Siegel, J. F. Cliche, Kendrick M. Smith, and Mark Halpern
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Phased array, Astrophysics::High Energy Astrophysical Phenomena, Holography, FOS: Physical sciences, 02 engineering and technology, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Radio telescope, Telescope, Optics, law, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, business.industry, Canadian Hydrogen Intensity Mapping Experiment, Astrophysics::Instrumentation and Methods for Astrophysics, 020206 networking & telecommunications, Interferometry, Pathfinder, Hydrogen line, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Canadian Hydrogen Intensity Mapping Experiment (CHIME) Pathfinder radio telescope is currently surveying the northern hemisphere between 400 and 800 MHz. By mapping the large scale structure of neutral hydrogen through its redshifted 21 cm line emission between $z \sim 0.8-2.5$ CHIME will contribute to our understanding of Dark Energy. Bright astrophysical foregrounds must be separated from the neutral hydrogen signal, a task which requires precise characterization of the polarized telescope beams. Using the DRAO John A. Galt 26 m telescope, we have developed a holography instrument and technique for mapping the CHIME Pathfinder beams. We report the status of the instrument and initial results of this effort., 16 pages, 9 figures. Submitted to Proc. SPIE, Astronomical Telescopes + Instrumentation (2016)
Published: 2016

34. HIRAX: A Probe of Dark Energy and Radio Transients

Author: Juan Mena Parra, Kavilan Moodley, Laura Newburgh, H. C. Chiang, Jeffrey B. Peterson, P. Stronkhorst, Aris Karastergiou, Amadeus Witzemann, G. Van Vuuren, Keith Vanderlinde, Martin Bucher, S. Macpherson, M. Mdlalose, O. Recnik, Chris Clarkson, Tzu-Ching Chang, Kevin Bandura, D. Lokhorst, B. Johnstone, Russ Taylor, Matt Hilton, Jonathan Sievers, Mario G. Santos, J. F. Cliche, Amanda Weltman, L. Ngwenya, N. Gupta, M. A. Dobbs, Ken Ganga, Roy Maartens, R. Dave, A. Gumba, T. Gogo, Martin Kunz, Oleg Smirnov, Benjamin Saliwanchik, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Marshall, Heather K., Hall, Helen J., Gilmozzi, Roberto, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie ( APC - UMR 7164 ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Milky Way, FOS: Physical sciences, Intensity mapping, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Cosmology, Large-scale structure, Pulsar, 0103 physical sciences, Dark energy, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 21cm, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Baryon acoustic oscillations, Equipment and services, 010308 nuclear & particles physics, Interferometers, Astronomy, Galaxy, Redshift, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Hydrogen
Abstract: The Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX) is a new 400-800MHz radio interferometer under development for deployment in South Africa. HIRAX will comprise 1024 six meter parabolic dishes on a compact grid and will map most of the southern sky over the course of four years. HIRAX has two primary science goals: to constrain Dark Energy and measure structure at high redshift, and to study radio transients and pulsars. HIRAX will observe unresolved sources of neutral hydrogen via their redshifted 21-cm emission line (`hydrogen intensity mapping'). The resulting maps of large-scale structure at redshifts 0.8-2.5 will be used to measure Baryon Acoustic Oscillations (BAO). HIRAX will improve upon current BAO measurements from galaxy surveys by observing a larger cosmological volume (larger in both survey area and redshift range) and by measuring BAO at higher redshift when the expansion of the universe transitioned to Dark Energy domination. HIRAX will complement CHIME, a hydrogen intensity mapping experiment in the Northern Hemisphere, by completing the sky coverage in the same redshift range. HIRAX's location in the Southern Hemisphere also allows a variety of cross-correlation measurements with large-scale structure surveys at many wavelengths. Daily maps of a few thousand square degrees of the Southern Hemisphere, encompassing much of the Milky Way galaxy, will also open new opportunities for discovering and monitoring radio transients. The HIRAX correlator will have the ability to rapidly and eXperimentciently detect transient events. This new data will shed light on the poorly understood nature of fast radio bursts (FRBs), enable pulsar monitoring to enhance long-wavelength gravitational wave searches, and provide a rich data set for new radio transient phenomena searches. This paper discusses the HIRAX instrument, science goals, and current status., Comment: 11 pages, 5 figures
Published: 2016
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35. A GPU-based Correlator X-engine Implemented on the CHIME Pathfinder

Author: Kris Sigurdson, Mark Halpern, Kevin Bandura, J. Richard Shaw, Laura Newburgh, Liam Connor, Nolan Denman, Juan Mena Parra, Adam D. Hincks, Gary Hinshaw, Kiyoshi Masui, C. Höfer, M. Fandino, Mandana Amiri, Keith Vanderlinde, Peter Klages, Andre Recnik, Matt Dobbs, J. F. Cliche, and Kendrick M. Smith
Subjects: business.industry, Computer science, Bandwidth (signal processing), FOS: Physical sciences, 020206 networking & telecommunications, 02 engineering and technology, 01 natural sciences, Radio telescope, Pathfinder, Stack (abstract data type), 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Computer hardware, Integer (computer science)
Abstract: We present the design and implementation of a custom GPU-based compute cluster that provides the correlation X-engine of the CHIME Pathfinder radio telescope. It is among the largest such systems in operation, correlating 32,896 baselines (256 inputs) over 400MHz of radio bandwidth. Making heavy use of consumer-grade parts and a custom software stack, the system was developed at a small fraction of the cost of comparable installations. Unlike existing GPU backends, this system is built around OpenCL kernels running on consumer-level AMD GPUs, taking advantage of low-cost hardware and leveraging packed integer operations to double algorithmic efficiency. The system achieves the required 105TOPS in a 10kW power envelope, making it among the most power-efficient X-engines in use today., 6 pages, 5 figures. Accepted by IEEE ASAP 2015
Published: 2015

36. Applications of control Precision timing control for radioastronomy maintaining femtosecond synchronization in the atacama large millimeter array

Author: J.-F. Cliche and B. Shillue
Subjects: Physics, Laser noise, business.industry, Ultrafast optics, Atacama Large Millimeter Array, law.invention, Optics, Control and Systems Engineering, law, Modeling and Simulation, Control system, Femtosecond, Synchronization (computer science), Phase noise, Electronic engineering, Electrical and Electronic Engineering, Radio control, business
Published: 2006
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37. SPT-3G: A Next-Generation Cosmic Microwave Background Polarization Experiment on the South Pole Telescope

Author: Matt Dobbs, Andreas Bender, Adrian T. Lee, Lloyd Knox, Benjamin Saliwanchik, Gilbert Holder, Joaquin Vieira, Dale Li, K. L. Thompson, W. B. Everett, T. M. Crawford, Z. Pan, K. Vanderlinde, Ki Won Yoon, Valentyn Novosad, Gene C. Hilton, H. Nguyen, D. Hanson, Mike McDonald, John E. Pearson, Stephen Padin, T. de Haan, T. Natoli, Jason W. Henning, Kent D. Irwin, A. Cukierman, Hsiao-Mei Cho, W. L. Holzapfel, Gensheng Wang, Chao-Lin Kuo, Alexey Vikhlinin, Christian L. Reichardt, Lindsey Bleem, Carole Tucker, Donna Kubik, G. Simard, John E. Carlstrom, Kaori Hattori, Jason E. Austermann, A. J. Gilbert, Graeme Smecher, J. E. Ruhl, A. Suzuki, Antony A. Stark, N. W. Halverson, M. J. Myers, D. Dutcher, J. F. Cliche, Steven W. Allen, Erik Shirokoff, Kam Arnold, V. G. Yefremenko, S. S. Meyer, E. M. Leitch, Samuel T. Ciocys, Bradford Benson, Peter A. R. Ade, J. T. Sayre, K. T. Story, N. L. Harrington, C. L. Chang, Z. Ahmed, Joshua Montgomery, Ryan Keisler, Holland, Wayne S., and Zmuidzinas, Jonas
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, Galaxy, Amplitude, South Pole Telescope, Dark energy, Neutrino, Astrophysics - Instrumentation and Methods for Astrophysics, Reionization, Instrumentation and Methods for Astrophysics (astro-ph.IM), Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We describe the design of a new polarization sensitive receiver, SPT-3G, for the 10-meter South Pole Telescope (SPT). The SPT-3G receiver will deliver a factor of ~20 improvement in mapping speed over the current receiver, SPTpol. The sensitivity of the SPT-3G receiver will enable the advance from statistical detection of B-mode polarization anisotropy power to high signal-to-noise measurements of the individual modes, i.e., maps. This will lead to precise (~0.06 eV) constraints on the sum of neutrino masses with the potential to directly address the neutrino mass hierarchy. It will allow a separation of the lensing and inflationary B-mode power spectra, improving constraints on the amplitude and shape of the primordial signal, either through SPT-3G data alone or in combination with BICEP-2/KECK, which is observing the same area of sky. The measurement of small-scale temperature anisotropy will provide new constraints on the epoch of reionization. Additional science from the SPT-3G survey will be significantly enhanced by the synergy with the ongoing optical Dark Energy Survey (DES), including: a 1% constraint on the bias of optical tracers of large-scale structure, a measurement of the differential Doppler signal from pairs of galaxy clusters that will test General Relativity on ~200 Mpc scales, and improved cosmological constraints from the abundance of clusters of galaxies., Comment: 21 pages, 9 figures. To be published in Proceedings of SPIE Volume 9153. Presented at SPIE Astronomical Telescopes + Instrumentation 2014, conference 9153
Published: 2014

38. Digital frequency domain multiplexing readout electronics for the next generation of millimeter telescopes

Author: A. Gilbert, Matt Dobbs, Tijmen de Haan, Neil Rowlands, Ken Smith, Andrew Wilson, Amy N. Bender, Graeme Smecher, Joshua Montgomery, and J. F. Cliche
Subjects: Computer science, business.industry, Dynamic range, Physics::Instrumentation and Detectors, Frequency domain multiplexing, Amplifier, Detector, Bandwidth (signal processing), Electrical engineering, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, 01 natural sciences, Multiplexing, 0103 physical sciences, Polyphase system, Electronics, 010306 general physics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Communication channel
Abstract: Frequency domain multiplexing (fMux) is an established technique for the readout of transition-edge sensor (TES) bolometers in millimeter-wavelength astrophysical instrumentation. In fMux, the signals from multiple detectors are read out on a single pair of wires reducing the total cryogenic thermal loading as well as the cold component complexity and cost of a system. The current digital fMux system, in use by POLARBEAR, EBEX, and the South Pole Telescope, is limited to a multiplexing factor of 16 by the dynamic range of the Superconducting Quantum Interference Device pre-amplifier and the total system bandwidth. Increased multiplexing is key for the next generation of large format TES cameras, such as SPT-3G and POLARBEAR2, which plan to have on the of order 15,000 detectors. Here, we present the next generation fMux readout, focusing on the warm electronics. In this system, the multiplexing factor increases to 64 channels per module (2 wires) while maintaining low noise levels and detector stability. This is achieved by increasing the system bandwidth, reducing the dynamic range requirements though active feedback, and digital synthesis of voltage biases with a novel polyphase filter algorithm. In addition, a version of the new fMux readout includes features such as low power consumption and radiation-hard components making it viable for future space-based millimeter telescopes such as the LiteBIRD satellite., 15 pages, 10 figures. To be published in Proceedings of SPIE Volume 9153. Presented at SPIE Astronomical Telescopes + Instrumentation 2014, conference 9153
Published: 2014

39. Calibrating CHIME, A New Radio Interferometer to Probe Dark Energy

Author: Ue-Li Pen, Gary Hinshaw, Adam D. Hincks, G. Davis, Rick Smegal, Kenneth Gibbs, Jeffrey B. Peterson, Kiyoshi Masui, C. Höfer, J. F. Cliche, J. Richard Bond, David Hanna, Laura Newburgh, A. Gilbert, Graeme Smecher, Kris Sigurdson, Keith Vanderlinde, T. L. Landecker, J. Richard Shaw, Mandana Amiri, Heather Fong, Peter Klages, Nolan Denman, Juan Mena Parra, Kevin Bandura, Andre Recnik, Graeme E. Addison, Matt Dobbs, Elizabeth Griffin, M. Fandino, D. V. Wiebe, Liam Connor, Meiling Deng, Mark Halpern, and Michael Sitwell
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radio interferometers, media_common.quotation_subject, FOS: Physical sciences, Intensity mapping, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, Acoustic oscillation, Astrophysical observatory, Observatory, Dark energy, 0103 physical sciences, Astronomical interferometer, 21cm, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, media_common, Physics, Interferometers, 010308 nuclear & particles physics, Canadian Hydrogen Intensity Mapping Experiment, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Spectral density, Cosmology, Interferometry, Sky, Calibration schemes, Calibration, Probes, Airborne telescopes, Baryon acoustic oscillations, Astrophysics - Instrumentation and Methods for Astrophysics, Frequency ranges, Hydrogen, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is a transit interferometer currently being built at the Dominion Radio Astrophysical Observatory (DRAO) in Penticton, BC, Canada. We will use CHIME to map neutral hydrogen in the frequency range 400 - 800MHz over half of the sky, producing a measurement of baryon acoustic oscillations (BAO) at redshifts between 0.8 - 2.5 to probe dark energy. We have deployed a pathfinder version of CHIME that will yield constraints on the BAO power spectrum and provide a test-bed for our calibration scheme. I will discuss the CHIME calibration requirements and describe instrumentation we are developing to meet these requirements., Ground-Based and Airborne Telescopes V, June 22-27, 2014, Series: Proceedings of SPIE; no. 9145
Published: 2014

40. Canadian Hydrogen Intensity Mapping Experiment (CHIME) Pathfinder

Author: Graeme E. Addison, Duncan Campbell-Wilson, Kris Sigurdson, Laura Newburgh, Meiling Deng, Liam Connor, Nolan Denman, J. Richard Bond, Kiyoshi Masui, C. Höfer, T. L. Landecker, Kevin Bandura, Gary Hinshaw, Mark Halpern, Graeme Smecher, Kenneth Gibbs, J. Richard Shaw, Matt Dobbs, David Hanna, Keith Vanderlinde, A. Gilbert, J. F. Cliche, Jeffrey B. Peterson, Ue-Li Pen, Adam D. Hincks, Mike Sitwell, Rick Smegal, M. Fandino, Mandana Amiri, G. Davis, Juan Mena Parra, Andre Recnik, Peter Klages, and D. V. Wiebe
Subjects: Frequency band, Acoustics, FOS: Physical sciences, Field of view, Intensity mapping, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, Acoustic oscillation, Power spectrum, Astrophysical observatory, Polarization, Astronomical interferometer, Frequency bands, Radio astronomy, Correlation matrix, Instrumentation and Methods for Astrophysics (astro-ph.IM), Wide-field surveys, Physics, BAO, Canadian Hydrogen Intensity Mapping Experiment, Low noise amplifiers, Astrophysics::Instrumentation and Methods for Astrophysics, Program processors, Cosmology, Pathfinder, Mapping, CHIME, Baryon acoustic oscillations, Airborne telescopes, Astrophysics - Instrumentation and Methods for Astrophysics, Hydrogen
Abstract: A pathfinder version of CHIME (the Canadian Hydrogen Intensity Mapping Experiment) is currently being commissioned at the Dominion Radio Astrophysical Observatory (DRAO) in Penticton, BC. The instrument is a hybrid cylindrical interferometer designed to measure the large scale neutral hydrogen power spectrum across the redshift range 0.8 to 2.5. The power spectrum will be used to measure the baryon acoustic oscillation (BAO) scale across this poorly probed redshift range where dark energy becomes a significant contributor to the evolution of the Universe. The instrument revives the cylinder design in radio astronomy with a wide field survey as a primary goal. Modern low-noise amplifiers and digital processing remove the necessity for the analog beam forming that characterized previous designs. The Pathfinder consists of two cylinders 37m long by 20m wide oriented north-south for a total collecting area of 1,500 square meters. The cylinders are stationary with no moving parts, and form a transit instrument with an instantaneous field of view of ∼100 degrees by 1-2 degrees. Each CHIME Pathfinder cylinder has a feedline with 64 dual polarization feeds placed every ∼30 cm which Nyquist sample the north-south sky over much of the frequency band. The signals from each dual-polarization feed are independently amplified, filtered to 400-800 MHz, and directly sampled at 800 MSps using 8 bits. The correlator is an FX design, where the Fourier transform channelization is performed in FPGAs, which are interfaced to a set of GPUs that compute the correlation matrix. The CHIME Pathfinder is a 1/10th scale prototype version of CHIME and is designed to detect the BAO feature and constrain the distance-redshift relation. The lessons learned from its implementation will be used to inform and improve the final CHIME design., Ground-Based and Airborne Telescopes V, June 22-27, 2014, Series: Proceedings of SPIE; no. 9145
Published: 2014
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41. The ALMA photonic local oscillator system

Author: R. Treacy, Christophe Jacques, Yoshihiro Masui, J. F. Cliche, Jason J. Castro, Bill Shillue, Wes Grammer, Rodrigo Brito, and Jack Meadows
Subjects: Physics, Heterodyne, business.industry, media_common.quotation_subject, Local oscillator, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Atacama Large Millimeter Array, Synchronization, Radio telescope, Optics, Sky, Femtosecond, Astrophysics::Earth and Planetary Astrophysics, Photonics, business, Astrophysics::Galaxy Astrophysics, media_common
Abstract: The Atacama Large Millimeter Array (ALMA) Photonic Local Oscillator (PLO) is an advanced photonics system that generates and distributes all of the Local Oscillator (LO) and timing references for the ALMA radio telescope array. These LO and timing references are used by the receivers and electronics at the antennas, and by the Correlator in the central building. Due to the unprecedented combination of high sky frequencies (up to 950 GHz) and long baseline lengths of up to 15 kilometers, the ALMA 1 st LO requirement is particularly stringent, with extremely precise timing and synchronization needed down to the ~10 femtosecond level.
Published: 2012
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42. Évaluation du Fonds d'initiatives autochtones, Québec Canada

Author: M-È Moktar Lamari, L Poulin, and J-F Cliche
Published: 2012
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43. All-fiber devices for chromatic dispersion compensation based on chirped distributed resonant coupling

Author: Francois Ouellette, S. Gagnon, and J.-F. Cliche
Subjects: Coupling, Physics, Optical fiber, business.industry, Physics::Optics, Atomic and Molecular Physics, and Optics, law.invention, Compensation (engineering), Optics, Fiber Bragg grating, law, Chirp, Physics::Accelerator Physics, Figure of merit, Optical filter, business, Nonlinear Sciences::Pattern Formation and Solitons, Diffraction grating
Abstract: We review the principle of operation and characteristics of all-fiber devices for dispersion compensation based on chirped distributed resonant coupling. These devices are the chirped Bragg grating, the chirped intermodal coupler, and the tapered two-dissimilar-core fiber. We discuss the use of a figure of merit to characterize equalizing filters. Based on a specific example, filter responses are computed and their performance is evaluated with a numerical simulation of an optical fiber link. Finally, design constraints are discussed. >
Published: 1994
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44. Low noise semiconductor laser for optical fiber sensing

Author: J.-F. Cliche, Michel Poulin, S. Ayotte, C. Latrasse, M. Aube, and A. Babin
Subjects: Optical fiber, Materials science, business.industry, Noise reduction, Physics::Optics, Laser, Semiconductor laser theory, law.invention, Laser linewidth, Optics, Fiber Bragg grating, law, Phase noise, Optoelectronics, Physics::Atomic Physics, business, Phase modulation
Abstract: Semiconductor lasers are of great interest in high performance optical fiber sensing systems because of their high reliability, lifetime, low cost and size. However, their linewidth and phase noise are often a limitation. Using frequency discrimination based on a specially designed fiber Bragg grating, we decrease the linewidth of a semiconductor laser to the kHz level, with phase noise reduction up to 1 MHz. Using a phase modulator in a second feedback loop to correct fast phase fluctuations, we demonstrate that the bandwidth can be pushed above 10 MHz.
Published: 2009
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45. Narrow linewidth lasers and their use in the generation and distribution of microwave signals

Author: Michel Tetu, M. Poulin, and J.-F. Cliche
Subjects: Materials science, business.industry, Microwave signals, Astrophysics::Instrumentation and Methods for Astrophysics, Physics::Optics, Astrophysics::Cosmology and Extragalactic Astrophysics, Laser, law.invention, Laser linewidth, law, Extremely high frequency, Phase noise, Optoelectronics, Photonics, business, Astrophysics::Galaxy Astrophysics, Microwave, Coherence (physics)
Abstract: The relationship between the spectral properties of lasers (phase/frequency noise, coherence, linewidth) and the quality of microwave signals generated by optical heterodyning is described. A 27-142 GHz photonic microwave and millimeter wave synthesizer is presented as an application of these concepts.
Published: 2007
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46. Fabrication of large dual-polarized multichroic TES bolometer arrays for CMB measurements with the SPT-3G camera

Author: V. G. Yefremenko, S. T. Ciocys, Kam Arnold, Benjamin Saliwanchik, Kent D. Irwin, W. L. Holzapfel, Ralu Divan, T. Natoli, Donna Kubik, N. W. Halverson, K. L. Thompson, M. J. Myers, Andrew Nadolski, W. B. Everett, Aritoki Suzuki, Antony A. Stark, Z. Pan, Ki Won Yoon, Carole Tucker, J. E. Ruhl, H. M. Cho, N. L. Harrington, Oliver Jeong, C. L. Kuo, Amy N. Bender, John E. Pearson, A. J. Gilbert, Valentine Novosad, John E. Carlstrom, Jason E. Austermann, Zeeshan Ahmed, Junjia Ding, Gene C. Hilton, J. F. Cliche, D. Dutcher, T. de Haan, Ryan Keisler, Kaori Hattori, Bradford Benson, Adrian T. Lee, E. M. Leitch, J. A. Sobrin, Graeme Smecher, Matt Dobbs, David A. Czaplewski, S. S. Meyer, K. E. Ziegler, C. L. Chang, Karen Byrum, A. Cukierman, T. M. Crawford, Lindsey Bleem, Erik Shirokoff, J. T. Sayre, Johannes Hubmayr, Joshua Montgomery, C. S. Miller, Peter A. R. Ade, K. T. Story, Nathan Whitehorn, H. Nguyen, K. Vanderlinde, Sergi Lendinez, Jason W. Henning, C. M. Posada, Joaquin Vieira, Liliana Stan, Stephen Padin, and Gensheng Wang
Subjects: Physics, business.industry, Bolometer, Detector, Metals and Alloys, Condensed Matter Physics, Isotropic etching, Microstrip, law.invention, Optics, South Pole Telescope, Etching (microfabrication), law, Materials Chemistry, Ceramics and Composites, Electrical and Electronic Engineering, Reactive-ion etching, business, Microfabrication
Abstract: This work presents the procedures used at Argonne National Laboratory to fabricate large arrays of multichroic transition-edge sensor (TES) bolometers for cosmic microwave background (CMB) measurements. These detectors will be assembled into the focal plane for the SPT-3G camera, the third generation CMB camera to be installed in the South Pole Telescope. The complete SPT-3G camera will have approximately 2690 pixels, for a total of 16 140 TES bolometric detectors. Each pixel is comprised of a broad-band sinuous antenna coupled to a Nb microstrip line. In-line filters are used to define the different bands before the millimeter-wavelength signal is fed to the respective Ti/Au TES bolometers. There are six TES bolometer detectors per pixel, which allow for measurements of three band-passes (95, 150 and 220 GHz) and two polarizations. The steps involved in the monolithic fabrication of these detector arrays are presented here in detail. Patterns are defined using a combination of stepper and contact lithography. The misalignment between layers is kept below 200 nm. The overall fabrication involves a total of 16 processes, including reactive and magnetron sputtering, reactive ion etching, inductively coupled plasma etching and chemical etching.
Published: 2015
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47. Effect of laser linewidth reduction systems on coherence length and interferometer noise

Author: J.-F. Cliche and M. Tetu
Subjects: Physics, Coherence time, Interferometric visibility, business.industry, Noise spectral density, Astrophysics::Instrumentation and Methods for Astrophysics, Physics::Optics, Degree of coherence, Coherence length, Laser linewidth, Interferometry, Optics, Optoelectronics, Physics::Atomic Physics, business, Coherence (physics)
Abstract: We analyze the effect of linewidth reduction systems on the degree of coherence of a laser and the noise levels measured at the output of an interferometer. We show results computed from the power spectral density of frequency noise measured on a DFB fiber laser and a DFB semiconductor laser narrowed with electrical feedback. Results show that the increase of coherence and interferometer noise is significant only over specific range of interferometer length, and that the improvement of interferometer noise might be proportionally much less important than the improvement in linewidth and coherence length.
Published: 2005
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48. Measurement of Laser Linewidths and Coherence Lengths using a Frequency Counter

Author: J.-F. Cliche and M. Tetu
Subjects: Physics, Coherence time, White light interferometry, business.industry, Physics::Optics, Laser, Coherence length, law.invention, Length measurement, Laser linewidth, Optics, law, Frequency counter, business, Coherence (physics)
Abstract: We describe how the linewidth and coherence length of high purity lasers can be estimated using a frequency counter to replace an optical interferometer of variable length. We also show theoretically and experimentally how such measurements are affected by the finite measurement time
Published: 2004
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49. Automatic absolute frequency calibration of tunable optical sources

Author: J.-F. Cliche and M. Tetu
Subjects: Materials science, Temperature control, business.industry, Physics::Optics, Laser, Semiconductor laser theory, law.invention, Optics, Semiconductor, law, Wavelength-division multiplexing, Calibration, business, Absorption (electromagnetic radiation), Optical filter
Abstract: We demonstrate a procedure that can be used to automatically calibrate the optical frequency of DFB MQW tunable semiconductor laser optical sources by measuring and recognizing the absorption pattern of a reference optical filter such as a gas cell.
Published: 2002
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50. A Radio-Frequency-over-Fiber link for large-array radio astronomy applications

Author: Matt Dobbs, Juan Mena, J. F. Cliche, Qing Yang Tang, A. Gilbert, and Kevin Bandura
Subjects: FOS: Physical sciences, 02 engineering and technology, 01 natural sciences, law.invention, Telescope, law, Observatory, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Instrumentation, Mathematical Physics, Physics, business.industry, Canadian Hydrogen Intensity Mapping Experiment, Astrophysics::Instrumentation and Methods for Astrophysics, Electrical engineering, 020206 networking & telecommunications, Laser, Interferometry, Analog signal, Radio frequency, Astrophysics - Instrumentation and Methods for Astrophysics, business, Radio astronomy
Abstract: A prototype 425-850 MHz Radio-Frequency-over-Fiber (RFoF) link for the Canadian Hydrogen Intensity Mapping Experiment (CHIME) is presented. The design is based on a directly modulated Fabry-Perot (FP) laser, operating at ambient temperature, and a single-mode fiber. The dynamic performance, gain stability, and phase stability of the RFoF link are characterized. Tests on a two-element interferometer built at the Dominion Radio Astrophysical Observatory for CHIME prototyping demonstrate that RFoF can be successfully used as a cost-effective solution for analog signal transport on the CHIME telescope and other large-array radio astronomy applications, 17 pages, 13 figures; submitted to Journal of Instrumentation (JINST). This preprint is under review
Published: 2013
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