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1. System performance of a cryogenic test-bed for the time-division multiplexing readout for NewAthena X-IFU

Author

Vaccaro, Davide, van der Kuur, Jan, van der Hulst, Paul, Vos, Tobias, de Wit, Martin, Gottardi, Luciano, Ravensberg, Kevin, Taralli, Emanuele, Adams, Joseph, Bandler, Simon, Bennet, Douglas, Chervenak, James, Doriese, Bertrand, Durkin, Malcolm, Gard, Johnathon, Reintsema, Carl, Sakai, Kazuhiro, Smith, Steven, Ullom, Joel, Wakeham, Nicholas, Herder, Jan-Willem den, jackson, Brian, Khosropanah, Pourya, Gao, Jian-Rong, Roelfsema, Peter, and Simionescu, Aurora

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The X-ray Integral Field Unit (X-IFU) is an instrument of ESA's future NewAthena space observatory, with the goal to provide high-energy resolution ($<$ 4 eV at X-ray energies up to 7 keV) and high-spatial resolution (9") spectroscopic imaging over the X-ray energy range from 200 eV to 12 keV, by means of an array of about 1500 transition-edge sensors (TES) read out via SQUID time-division multiplexing (TDM). In 2022, to aid in the transfer of TDM readout technology from the laboratory toward flight hardware, our team commissioned a new TDM-based laboratory test-bed at SRON. This setup hosts an array of $75\times 75\ \mu$m$^2$ TESs that are read out via 2-column $\times$ 32-row TDM. A system component that is critical to high-performance operation is the wiring harness that connects the room-temperature electronics to the cryogenic readout componentry. In November 2023, we implemented a re-designed flex harness, which in the SRON test-bed has a length close to what is envisioned for the X-IFU flight harness. We report here on our characterization of the TDM system with the new flex harness, which allowed the system to achieve a co-added energy resolution at a level of 2.7~eV FWHM at 6~keV via 32-row readout. In addition, we provide an outlook on the upcoming integration of TDM readout into the X-IFU Focal-Plane Assembly Development Model., Comment: Submitted for publication to Journal of Astronomical Telescopes, Instrumentation and Systems. arXiv admin note: text overlap with arXiv:2403.02978

Published
2024

2. Single Aperture Large Telescope for Universe Studies (SALTUS): Science Overview

Author

Chin, Gordon, Anderson, Carrie M., Bergner, Jennifer, Biver, Nicolas, Bjoraker, Gordon L., Cavalie, Thibault, DiSanti, Michael, Gao, Jian-Rong, Hartogh, Paul, Harding, Leon K., Hu, Qing, Kim, Daewook, Kulesa, Craig, de Lange, Gert, Leisawitz, David T., Levy, Rebecca C., Lichtenberger, Arthur, Marronh, Daniel P., Najita, Joan, Newswander, Trent, Rieke, George H., Rigopoulou, Dimitra, Roefsema, Peter, Roth, Nathan X., Schwarz, Kamber, Shirley, Yancy, Spilker, Justin, Stark, Antony A., van der Tak, Floris, Takashima, Yuzuru, Tielens, Alexander, Willner, David J., Wollack, Edward J., Yates, Stephen, Young, Erick, and Walker, Christopher K.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The SALTUS Probe mission will provide a powerful far-infrared (far-IR) pointed space observatory to explore our cosmic origins and the possibility of life elsewhere. The observatory employs an innovative deployable 14-m aperture, with a sunshield that will radiatively cool the off-axis primary to <45K. This cooled primary reflector works in tandem with cryogenic coherent and incoherent instruments that span the 34 to 660 micron far-IR range at both high and moderate spectral resolutions., Comment: 49 pages, 10 figures, 3 tables, submitted to SPIE JATIS

Published
2024

3. 4x2 Hot electron bolometer mixer arrays for detection at 1.46, 1.9 and 4.7 THz for a balloon borne terahertz observatory

Author

Silva, José R. G., Laauwen, Wouter M., Mirzaei, Behnam, Vercruyssen, Nathan, Finkel, Matvey, Westerveld, Menno, More, Nikhil, Silva, Vitor, Young, Abram, Kulesa, Craig, Walker, Christopher, van der Tak, Floris, and Gao, Jian Rong

Subjects
Physics - Instrumentation and Detectors
Abstract

We have demonstrated three 4x2 hot electron bolometer (HEB) mixer arrays for operation at local oscillator (LO) frequencies of 1.46, 1.9 and 4.7 THz, respectively. They consist of spiral antenna coupled NbN HEB mixers combined with elliptical lenses. These are to date the highest pixel count arrays using a quasi-optical coupling scheme at supra-THz frequencies. At 1.4 THz, we measured an average double sideband mixer noise temperature of 330 K, a mixer conversion loss of 5.7 dB, and an optimum LO power of 210 nW. The array at 1.9 THz has an average mixer noise temperature of 420K, a conversion loss of 6.9 dB, and an optimum LO power of 190 nW. For the array at 4.7 THz, we obtained an average mixer noise temperature of 700 K, a conversion loss of 9.7 dB, and an optimum LO power of 240 nW. We found the arrays to be uniform regarding the mixer noise temperature with a standard deviation of 3-4%, the conversion loss with a standard deviation of 7-10%, and optimum LO power with a standard deviation of 5-6%. The noise bandwidth was also measured, being 3.5 GHz for the three arrays. These performances are comparable to previously reported values in the literature for single pixels and also other detector arrays. Our arrays meet the requirements of the Galactic/Extra-Galactic ULDB Spectroscopic Terahertz Observatory (GUSTO), a NASA balloon borne observatory, and are therefore scheduled to fly as part of the payload, which is expected to be launched in December 2023.

Published
2023

4. Compact Metasurface Terahertz Spectrometer

Author

Ji, Wenye, Chang, Jin, Mirzaei, Behnam, Ridder, Marcel, Jellema, Willem, Kao, Wilt, Lee, Alan, Gao, Jian Rong, Urbach, Paul, and Adam, Aurele J. L.

Subjects
Physics - Optics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The electromagnetic spectrum in the terahertz frequency region is of significant importance for understanding the formation and evolution of galaxies and stars throughout the history of the universe and the process of planet formation. Within the star forming clouds the constituent atoms and molecules are excited to produce characteristic emission and absorption lines, many of which happen at the terahertz frequencies. Thus, detecting the spectral signatures as unique fingerprints of molecules and atoms require terahertz spectrometers, which need to be operated in a space observatory because of the water vapor absorption in the earth atmosphere. However, current terahertz spectrometers face several challenges that limit their performances and applications, including a low resolution, limited bandwidth, large volume, and complexity. In this paper, we address the last two issues by demonstrating a concept of a compact terahertz spectrometer using metasurface. We start by modelling, designing, and fabricating a metasurface, aiming to optimize its performance within a band from 1.7 to 2.5 THz. Next, we make use of an array of quantum cascade lasers that operate at slightly different frequencies around 2.1 THz to validate the performance of the spectrometer. Finally, we apply the spectrum inversion method to analyse the measured data to confirm a resolution R of at least 273. Our results demonstrated a miniaturized terahertz spectrometer concept successfully.

Published
2023

5. Recent Advances in Metasurface Design and Quantum Optics Applications with Machine Learning, Physics-Informed Neural Networks, and Topology Optimization Methods

Author

Ji, Wenye, Chang2, Jin, Xu, He-Xiu, Gao, Jian Rong, Gröblacher, Simon, Urbach, Paul, and Adam, Aurèle J. L.

Subjects
Physics - Optics, Physics - Applied Physics
Abstract

As a two-dimensional planar material with low depth profile, a metasurface can generate non-classical phase distributions for the transmitted and reflected electromagnetic waves at its interface. Thus, it offers more flexibility to control the wave front. A traditional metasurface design process mainly adopts the forward prediction algorithm, such as Finite Difference Time Domain, combined with manual parameter optimization. However, such methods are time-consuming, and it is difficult to keep the practical meta-atom spectrum being consistent with the ideal one. In addition, since the periodic boundary condition is used in the meta-atom design process, while the aperiodic condition is used in the array simulation, the coupling between neighboring meta-atoms leads to inevitable inaccuracy. In this review, representative intelligent methods for metasurface design are introduced and discussed, including machine learning, physics-information neural network, and topology optimization method. We elaborate on the principle of each approach, analyze their advantages and limitations, and discuss their potential applications. We also summarise recent advances in enabled metasurfaces for quantum optics applications. In short, this paper highlights a promising direction for intelligent metasurface designs and applications for future quantum optics research and serves as an up-to-date reference for researchers in the metasurface and metamaterial fields.

Published
2023

6. The Athena X-ray Integral Field Unit: a consolidated design for the system requirement review of the preliminary definition phase

Author

Barret, Didier, Albouys, Vincent, Herder, Jan-Willem den, Piro, Luigi, Cappi, Massimo, Huovelin, Juhani, Kelley, Richard, Mas-Hesse, J. Miguel, Paltani, Stéphane, Rauw, Gregor, Rozanska, Agata, Svoboda, Jiri, Wilms, Joern, Yamasaki, Noriko, Audard, Marc, Bandler, Simon, Barbera, Marco, Barcons, Xavier, Bozzo, Enrico, Ceballos, Maria Teresa, Charles, Ivan, Costantini, Elisa, Dauser, Thomas, Decourchelle, Anne, Duband, Lionel, Duval, Jean-Marc, Fiore, Fabrizio, Gatti, Flavio, Goldwurm, Andrea, Hartog, Roland den, Jackson, Brian, Jonker, Peter, Kilbourne, Caroline, Korpela, Seppo, Macculi, Claudio, Mendez, Mariano, Mitsuda, Kazuhisa, Molendi, Silvano, Pajot, François, Pointecouteau, Etienne, Porter, Frederick, Pratt, Gabriel W., Prêle, Damien, Ravera, Laurent, Sato, Kosuke, Schaye, Joop, Shinozaki, Keisuke, Skup, Konrad, Soucek, Jan, Thibert, Tanguy, Vink, Jacco, Webb, Natalie, Chaoul, Laurence, Raulin, Desi, Simionescu, Aurora, Torrejon, Jose Miguel, Acero, Fabio, Branduardi-Raymont, Graziella, Ettori, Stefano, Finoguenov, Alexis, Grosso, Nicolas, Kaastra, Jelle, Mazzotta, Pasquale, Miller, Jon, Miniutti, Giovanni, Nicastro, Fabrizio, Sciortino, Salvatore, Yamaguchi, Hiroya, Beaumont, Sophie, Cucchetti, Edoardo, D'Andrea, Matteo, Eckart, Megan, Ferrando, Philippe, Kammoun, Elias, Lotti, Simone, Mesnager, Jean-Michel, Natalucci, Lorenzo, Peille, Philippe, de Plaa, Jelle, Ardellier, Florence, Argan, Andrea, Bellouard, Elise, Carron, Jérôme, Cavazzuti, Elisabetta, Fiorini, Mauro, Khosropanah, Pourya, Martin, Sylvain, Perry, James, Pinsard, Frederic, Pradines, Alice, Rigano, Manuela, Roelfsema, Peter, Schwander, Denis, Torrioli, Guido, Ullom, Joel, Vera, Isabel, Villegas, Eduardo Medinaceli, Zuchniak, Monika, Brachet, Frank, Cicero, Ugo Lo, Doriese, William, Durkin, Malcom, Fioretti, Valentina, Geoffray, Hervé, Jacques, Lionel, Kirsch, Christian, Smith, Stephen, Adams, Joseph, Gloaguen, Emilie, Hoogeveen, Ruud, van der Hulst, Paul, Kiviranta, Mikko, van der Kuur, Jan, Ledot, Aurélien, van Leeuwen, Bert-Joost, van Loon, Dennis, Lyautey, Bertrand, Parot, Yann, Sakai, Kazuhiro, van Weers, Henk, Abdoelkariem, Shariefa, Adam, Thomas, Adami, Christophe, Aicardi, Corinne, Akamatsu, Hiroki, Alonso, Pablo Eleazar Merino, Amato, Roberta, André, Jérôme, Angelinelli, Matteo, Anon-Cancela, Manuel, Anvar, Shebli, Atienza, Ricardo, Attard, Anthony, Auricchio, Natalia, Balado, Ana, Bancel, Florian, Barusso, Lorenzo Ferrari, Bernard, Vivian, Berrocal, Alicia, Blin, Sylvie, Bonino, Donata, Bonnet, François, Bonny, Patrick, Boorman, Peter, Boreux, Charles, Bounab, Ayoub, Boutelier, Martin, Boyce, Kevin, Brienza, Daniele, Bruijn, Marcel, Bulgarelli, Andrea, Calarco, Simona, Callanan, Paul, Camus, Thierry, Canourgues, Florent, Capobianco, Vito, Cardiel, Nicolas, Castellani, Florent, Cheatom, Oscar, Chervenak, James, Chiarello, Fabio, Clerc, Nicolas, Clerc, Laurent, Cobo, Beatriz, Coeur-Joly, Odile, Coleiro, Alexis, Colonges, Stéphane, Corcione, Leonardo, Coriat, Mickael, Coynel, Alexandre, Cuttaia, Francesco, D'Ai, Antonino, D'anca, Fabio, Dadina, Mauro, Daniel, Christophe, DeNigris, Natalie, Dercksen, Johannes, DiPirro, Michael, Doumayrou, Eric, Dubbeldam, Luc, Dupieux, Michel, Dupourqué, Simon, Durand, Jean Louis, Eckert, Dominique, Eiriz, Valvanera, Ercolani, Eric, Etcheverry, Christophe, Finkbeiner, Fred, Fiocchi, Mariateresa, Fossecave, Hervé, Franssen, Philippe, Frericks, Martin, Gabici, Stefano, Gant, Florent, Gao, Jian-Rong, Gastaldello, Fabio, Genolet, Ludovic, Ghizzardi, Simona, Gil, M Angeles Alcacera, Giovannini, Elisa, Godet, Olivier, Gomez-Elvira, Javier, Gonzalez, Manuel, Gonzalez, Raoul, Gottardi, Luciano, Granat, Dolorès, Gros, Michel, Guignard, Nicolas, Hieltjes, Paul, Hurtado, Adolfo Jesus, Irwin, Kent, Jacquey, Christian, Janiuk, Agnieszka, Jaubert, Jean, Jiménez, Maria, Jolly, Antoine, Jourdan, Thierry, Julien, Sabine, Kedziora, Bartosz, Korb, Andrew, Kreykenbohm, Ingo, König, Ole, Langer, Mathieu, Laudet, Philippe, Laurent, Philippe, Laurenza, Monica, Lesrel, Jean, Ligori, Sebastiano, Lorenz, Maximilian, Luminari, Alfredo, Maffei, Bruno, Maisonnave, Océane, Marelli, Lorenzo, Massonet, Didier, Maussang, Irwin, Melchor, Alejandro Gonzalo, Mer, Isabelle Le, Michalski, Lea, Millerioux, Jean-Pierre, Mineo, Teresa, Minervini, Gabriele, Molin, Alexeï, Monestes, David, Montinaro, Nicola, Mot, Baptiste, Murat, David, Nagayoshi, Kenichiro, Nazé, Yaël, Noguès, Loïc, Pailot, Damien, Panessa, Francesca, Parodi, Luigi, Petit, Pascal, Piconcelli, Enrico, Pinto, Ciro, Plaza, Jose Miguel Encinas, Poyatos, David, Prouvé, Thomas, Ptak, Andy, Puccetti, Simonetta, Puccio, Elena, Ramon, Pascale, Reina, Manuel, Rioland, Guillaume, Rodriguez, Louis, Roig, Anton, Rollet, Bertrand, Roncarelli, Mauro, Roudil, Gilles, Rudnicki, Tomasz, Sanisidro, Julien, Sciortino, Luisa, Silva, Vitor, Sordet, Michael, Soto-Aguilar, Javier, Spizzi, Pierre, Surace, Christian, Sánchez, Miguel Fernández, Taralli, Emanuele, Terrasa, Guilhem, Terrier, Régis, Todaro, Michela, Ubertini, Pietro, Uslenghi, Michela, de Vaate, Jan Geralt Bij, Vaccaro, Davide, Varisco, Salvatore, Varnière, Peggy, Vibert, Laurent, Vidriales, María, Villa, Fabrizio, Vodopivec, Boris Martin, Volpe, Angela, de Vries, Cor, Wakeham, Nicholas, Walmsley, Gavin, Wise, Michael, de Wit, Martin, and Woźniak, Grzegorz

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

The Athena X-ray Integral Unit (X-IFU) is the high resolution X-ray spectrometer, studied since 2015 for flying in the mid-30s on the Athena space X-ray Observatory, a versatile observatory designed to address the Hot and Energetic Universe science theme, selected in November 2013 by the Survey Science Committee. Based on a large format array of Transition Edge Sensors (TES), it aims to provide spatially resolved X-ray spectroscopy, with a spectral resolution of 2.5 eV (up to 7 keV) over an hexagonal field of view of 5 arc minutes (equivalent diameter). The X-IFU entered its System Requirement Review (SRR) in June 2022, at about the same time when ESA called for an overall X-IFU redesign (including the X-IFU cryostat and the cooling chain), due to an unanticipated cost overrun of Athena. In this paper, after illustrating the breakthrough capabilities of the X-IFU, we describe the instrument as presented at its SRR, browsing through all the subsystems and associated requirements. We then show the instrument budgets, with a particular emphasis on the anticipated budgets of some of its key performance parameters. Finally we briefly discuss on the ongoing key technology demonstration activities, the calibration and the activities foreseen in the X-IFU Instrument Science Center, and touch on communication and outreach activities, the consortium organisation, and finally on the life cycle assessment of X-IFU aiming at minimising the environmental footprint, associated with the development of the instrument. Thanks to the studies conducted so far on X-IFU, it is expected that along the design-to-cost exercise requested by ESA, the X-IFU will maintain flagship capabilities in spatially resolved high resolution X-ray spectroscopy, enabling most of the original X-IFU related scientific objectives of the Athena mission to be retained. (abridged)., Comment: 48 pages, 29 figures, Accepted for publication in Experimental Astronomy with minor editing

Published
2022
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7. Frequency domain multiplexing readout for large arrays of transition-edge sensors

Author

Vaccaro, Davide, Akamatsu, Hiroki, Gottardi, Luciano, van der Kuur, Jan, Nagayoshi, Kenichiro, Taralli, Emanuele, de Wit, Martin, Bruijn, Marcel P., van der Linden, Anton J., van Leeuwen, Bert-Joost, van der Hulst, Paul, Ravensberg, Kevin, de Vries, Cor P., Kiviranta, Mikko, Gao, Jian-Rong, and Herder, Jan-Willem A. den

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract

We report our most recent progress and demonstration of a frequency domain multiplexing (FDM) readout technology for transition-edge sensor (TES) arrays, both of which we have been developing, in the framework of the X-IFU instrument on board the future Athena X-ray telescope. Using Ti/Au TES micro-calorimeters, high-Q LC filters and analog/digital electronics developed at SRON and low-noise two-stage SQUID amplifiers from VTT Finland, we demonstrated feasibility of our FDM readout technology, with the simultaneous readout of 37 pixels with an energy resolution at of 2.23 eV at an energy of 6 keV. We finally outline our plans for further scaling up and improving our technology., Comment: Version submitted to Nuclear Instruments and Methods A for the proceedings of the Pisa Meeting 2021 conference

Published
2022
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8. Performance of the SRON Ti/Au Transition Edge Sensor X-ray Calorimeters

Author

de Wit, Martin, Gottardi, Luciano, Nagayoshi, Kenichiro, Akamatsu, Hiroki, Bruijn, Marcel P., Ridder, Marcel L., Taralli, Emanuele, Vaccaro, Davide, Gao, Jian-Rong, and Herder, Jan-Willem A. den

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

In the early 2030s, ESAs new X-ray observatory, Athena, is scheduled to be launched. It will carry two main instruments, one of which is the X-ray Integral Field Unit (X-IFU), an X-ray imaging spectrometer, which will consist of an array of several thousand transition-edge sensors (TESs) with a proposed energy resolution of 2.5 eV for photon energies up to 7 keV. At SRON we develop the backup TES array based on Ti/Au bilayers with a transition temperature just below 100 mK. In this contribution we will give a broad overview of the properties and capabilities of these state-of-the-art detectors. Over the years we have fabricated and studied a large number of detectors with various geometries, providing us with a good understanding of how to precisely control the properties of our detectors. We are able to accurately vary the most important detector properties, such as the normal resistance, thermal conductance and critical temperature. This allows us to finely tune our detectors to meet the demands of various applications. The detectors have demonstrated excellent energy resolutions of below 1.8 eV for 5.9 keV X-rays. By tuning the properties of the devices, they can be optimally matched to various read-out schemes using both AC and DC biasing. The next step is to increase the size of our TES arrays from our current kilo-pixel arrays towards the full-sized array for X-IFU., Comment: Submitted as a conference proceeding for SPIE Astronomical Telescopes + Instrumentation 2022

Published
2022
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9. Susceptibility study of TES micro-calorimeters for X-ray spectroscopy under FDM readout

Author

Vaccaro, Davide, Akamatsu, Hiroki, Gottardi, Luciano, van der Kuur, Jan, Taralli, Emanuele, de Wit, Martin, Bruijn, Marcel P., Hartog, Roland den, Kiviranta, Mikko, van der Linden, Anton J., Nagayoshi, Kenichiro, Ravensberg, Kevin, Ridder, Marcel L., Visser, Sven, Jackson, Brian D., Gao, Jian-Rong, Hoogeveen, Ruud W. M., and Herder, Jan-Willem A. den

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present a characterization of the sensitivity of TES X-ray micro-calorimeters to environmental conditions under frequency-domain multiplexing (FDM) readout. In the FDM scheme, each TES in a readout chain is in series with a LC band-pass filter and AC biased with an independent carrier at MHz range. Using TES arrays, cold readout circuitry and warm electronics fabricated at SRON and SQUIDs produced at VTT Finland, we characterize the sensitivity of the detectors to bias voltage, bath temperature and magnetic field. We compare our results with the requirements for the Athena X-IFU instrument, showing the compliance of the measured sensitivities. We find in particular that FDM is intrinsically insensitive to the magnetic field because of TES design and AC readout., Comment: This paper has been accepted for publication in Journal of Low Temperature Physics

Published
2022
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10. Mitigation of the Magnetic Field Susceptibility of Transition Edge Sensors using a Superconducting Groundplane

Author

de Wit, Martin, Gottardi, Luciano, Ridder, Marcel L., Nagayoshi, Kenichiro, Taralli, Emanuele, Akamatsu, Hiroki, Vaccaro, Davide, Herder, Jan-Willem A. den, Bruijn, Marcel P., and Gao, Jian-Rong

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract

Transition edge sensor (TES) microcalorimeters and bolometers are used for a variety of applications. The sensors are based on the steep temperature-dependent resistance of the normal-to-superconducting transition, and are thus intrinsically sensitive to magnetic fields. Conventionally the detectors are shielded from stray magnetic fields using external magnetic shields. However, in particular for applications with strict limits on the available space and mass of an instrument, external magnetic shields might not be enough to obtain the required shielding factors or field homogeneity. Additionally, these shields are only effective for magnetic fields generated external to the TES array, and are ineffective to mitigate the impact of internally generated magnetic fields. Here we present an alternative shielding method based on a superconducting groundplane deposited directly on the backside of the silicon nitride membrane on which the TESs are located. We demonstrate that this local shielding for external magnetic fields has a shielding factor of at the least ~ 75, and is also effective at reducing internal self-induced magnetic fields, as demonstrated by measurements and simulation of the eddy current losses in our AC biased detectors. Measurements of 5.9 keV X-ray photons show that our shielded detectors have a high resilience to external magnetic fields, showing no degradation of the energy resolution or shifts of the energy scale calibration for fields of several microTesla, values higher than expected in typical real-world applications., Comment: 11 pages, 8 figures

Published
2022
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11. Thermal crosstalk of X-ray transition-edge sensor micro-calorimeters under frequency domain multiplexing readout

Author

Vaccaro, Davide, Akamatsu, Hiroki, Bruijn, Marcel P., Gottardi, Luciano, Hartog, Roland den, van der Kuur, Jan, van der Linden, A. J., Nagayoshi, Kenichiro, Ravensberg, Kevin, Ridder, Marcel L., Taralli, Emanuele, de Wit, Martin, Gao, Jian-Rong, Hoogeveen, Ruud W. M., and Herder, Jan-Willem A. den

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract

We have measured and characterized the thermal crosstalk in two different arrays of transition-edge sensor (TES) X-ray micro-calorimeters with frequency-domain multiplexing (FDM) readout. The TES arrays are fabricated at SRON and are a 8$\times$8 and a 32$\times$32 "kilo-pixel" uniform array. The amount of crosstalk is evaluated as the ratio between the averaged crosstalk signal and the X-ray pulse amplitudes. The crosstalk ratios (CR) for our detectors are compliant with the requirements for future X-ray space missions, such as Athena X-IFU (CR$< 10^{-3}$ for first-neighbour pixels): we measured a nearest-neighbour thermal crosstalk ratio at a level of $10^{-4}$, with a highest crosstalk ratio of $4\times 10^{-4}$ for the kilo-pixel array (worst case, center of array) and $1\times 10^{-4}$ for the 8$\times$8 array, with a margin of improvement achievable by optimizing the Cu metallization and the width of the Si supporting structures (muntins) in the backside of the TES array chip. Based on the measured crosstalk ratios, we have estimated the impact on the spectral resolution by means of noise equivalent power (NEP) considerations and a Monte Carlo simulation, finding an average degradation in quadrature of less than 40~meV, compliant with the < 0.2~eV requirement for Athena X-IFU.

Published
2021
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12. Single pixel performance of a 32$\times$32 Ti/Au TES array with broadband X-ray spectra

Author

D'Andrea, Matteo, Taralli, Emanuele, Akamatsu, Hiroki, Gottardi, Luciano, Nagayoshi, Kenichiro, Ravensberg, Kevin, Ridder, Marcel L., Vaccaro, Davide, de Vries, Cor P., de Wit, Martin, Bruijn, Marcel P., Hoogeveen, Ruud W. M., and Gao, Jian-Rong

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract

We are developing a kilo-pixels Ti/Au TES array as a backup option for Athena X-IFU. Here we report on single-pixel performance of a 32$\times$32 array operated in a Frequency Division Multiplexing (FDM) readout system, with bias frequencies in the range 1-5 MHz. We have tested the pixels response at several photon energies, by means of a $^{55}$Fe radioactive source (emitting Mn-K$\alpha$ at 5.9 keV) and a Modulated X-ray Source (MXS, providing Cr-K$\alpha$ at 5.4 keV and Cu-K$\alpha$ at 8.0 keV). First, we report the procedure used to perform the detector energy scale calibration, usually achieving a calibration accuracy better than $\sim$ 0.5 eV in the 5.4 - 8.9 keV energy range. Then, we present the measured energy resolution at the different energies (best single pixel performance: $\Delta$E$_{FWHM}$ = 2.40 $\pm$ 0.09 eV @ 5.4 keV; 2.53 $\pm$ 0.10 eV @ 5.9 keV; 2.78 $\pm$ 0.16 eV @ 8.0 keV), investigating also the performance dependency from the pixel bias frequency and the count rate. Thanks to long background measurements ($\sim$ 1 day), we finally detected also the Al-K$\alpha$ line at 1.5 keV, generated by fluorescence inside the experimental setup. We analyzed this line to obtain a first assessment of the single-pixel performance also at low energy ($\Delta$E$_{FWHM}$ = 1.91 eV $\pm$ 0.21 eV @ 1.5 keV), and to evaluate the linearity of the detector response in a large energy band (1.5 - 8.9 keV)., Comment: Accepted for publication in IEEE Transactions on Applied Superconductivity for ASC2020 special issue

Published
2021
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13. Probing ISM Structure in Trumpler 14 & Carina I Using The Stratospheric Terahertz Observatory 2

Author

Seo, Young Min, Goldsmith, Paul F., Walker, Chris, Hollenbach, David J., Wolfire, Mark G., Kulesa, Craig, Tolls, Volker, Bernasconi, Pietro N., Kavak, Umit, van der Tak, Floris F. S., Shipman, Russ, Gao, Jian Rong, Tielens, Alexander, Burton, Michael G., Yorke, Harold, Young, Erick, Peters, William L., Young, Abram, Groppi, Christopher, Davis, Kristina, Pineda, Jorge L., Langer, William D., Kawamura, Jonathan H., Stark, Antony, Melnick, Gary, Rebolledo, David, Wong, Graeme F., Horiuchi, Shinji, and Kuiper, Thomas B.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present observations of the Trumpler 14/Carina I region carried out using the Stratospheric Terahertz Observatory 2 (STO2). The Trumpler 14/Carina I region is in the west part of the Carina Nebula Complex, which is one of the most extreme star-forming regions in the Milky Way. We observed Trumpler 14/Carina I in the 158 $\mu$m transition of [C\,{\sc ii}] with a spatial resolution of 48$''$ and a velocity resolution of 0.17 km s$^{-1}$. The observations cover a 0.25$^\circ$ by 0.28$^\circ$ area with central position {\it l} = 297.34$^\circ$, {\it b} = -0.60$^\circ$. The kinematics show that bright [C\,{\sc ii}] structures are spatially and spectrally correlated with the surfaces of CO clouds, tracing the photodissociation region and ionization front of each molecular cloud. Along 7 lines of sight that traverse Tr 14 into the dark ridge to the southwest, we find that the [C\,{\sc ii}] luminosity from the HII region is 3.7 times that from the PDR. In same los we find in the PDRs an average ratio of 1:4.1:5.6 for the mass in atomic gas:dark-CO gas: molecular gas traced by CO. Comparing multiple gas tracers including HI 21cm, [C\,{\sc ii}], CO, and radio recombination lines, we find that the HII regions of the Carina Nebula Complex are well-described as HII regions with one-side freely expanding towards us, consistent with the champagne model of ionized gas evolution. The dispersal of the GMC in this region is dominated by EUV photoevaporation; the dispersal timescale is 20-30 Myr., Comment: ApJ accepted

Published
2019
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14. The SAFARI Detector System

Author

Audley, Michael D., de Lange, Gert, Gao, Jian-Rong, Jackson, Brian D., Hijmering, Richard A., Ridder, Marcel L., Bruijn, Marcel P., Roelfsema, Peter R., Ade, Peter A. R., Withington, Stafford, Bradford, Charles M., and Trappe, Neal A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We give an overview of the baseline detector system for SAFARI, the prime focal-plane instrument on board the proposed space infrared observatory, SPICA. SAFARI's detectors are based on superconducting Transition Edge Sensors (TES) to provide the extreme sensitivity (dark NEP$\le2\times10^{-19}\rm\ W/\sqrt Hz$) needed to take advantage of SPICA's cold (<8 K) telescope. In order to read out the total of ~3500 detectors we use frequency domain multiplexing (FDM) with baseband feedback. In each multiplexing channel, a two-stage SQUID preamplifier reads out 160 detectors. We describe the detector system and discuss some of the considerations that informed its design., Comment: 7 pages, 3 figures, Proc. SPIE 10708, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX, 107080K (9 July 2018); (fixed typo in abstract)

Published
2018
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15. Optical performance of prototype horn-coupled TES bolometer arrays for SAFARI

Author

Audley, Michael D., de Lange, Gert, Gao, Jian-Rong, Khosropanah, Pourya, Hijmering, Richard, and Ridder, Marcel L

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The SAFARI Detector Test Facility is an ultra-low background optical testbed for characterizing ultra-sensitive prototype horn-coupled TES bolmeters for SAFARI, the grating spectrometer on board the proposed SPICA satellite. The testbed contains internal cold and hot black-body illuminators and a light-pipe for illumination with an external source. We have added reimaging optics to facilitate array optical measurements. The system is now being used for optical testing of prototype detector arrays read out with frequency-domain multiplexing. We present our latest optical measurements of prototype arrays and discuss these in terms of the instrument performance., Comment: 9 pages, 8 figures. Copyright 2016 Society of Photo Optical Instrumentation Engineers. One print or electronic copy may be made for personal use only. Systematic reproduction and distribution, duplication of any material in this paper for a fee or for commercial purposes, or modification of the content of the paper are prohibited

Published
2016
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16. Terahertz multi-heterodyne spectroscopy using laser frequency combs

Author

Yang, Yang, Burghoff, David, Hayton, Darren J., Gao, Jian-Rong, Reno, John L., and Hu, Qing

Subjects
Physics - Optics
Abstract

Frequency combs based on terahertz quantum cascade lasers feature broadband coverage and high output powers in a compact package, making them an attractive option for broadband spectroscopy. Here, we demonstrate the first multi-heterodyne spectroscopy using two terahertz quantum cascade laser combs. With just 100 $\mu$s of integration time, we achieve peak signal-to-noise ratios exceeding 60 dB and a spectral coverage greater than 250 GHz centered at 2.8 THz. Even with room-temperature detectors we are able to achieve peak signal-to-noise ratios of 50 dB, and as a proof-of-principle we use these combs to measure the broadband transmission spectrum of etalon samples. Finally, we show that with proper signal processing, it is possible to extend the multi-heterodyne spectroscopy to quantum cascade laser combs operating in pulsed mode, greatly expanding the range of quantum cascade lasers that could be suitable for these techniques.

Published
2016

17. Optical performance of an ultra-sensitive horn-coupled transition-edge-sensor bolometer with hemispherical backshort in the far infrared

Author

Audley, Michael D., de Lange, Gert, Gao, Jian-Rong, Khosropanah, Pourya, Hijmering, Richard, Ridder, Marcel, Mauskopf, Philip D., Morozov, Dmitry, Trappe, Neil A., and Doherty, Stephen

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract

The next generation of far infrared space observatories will require extremely sensitive detectors that can be realized only by combining extremely low intrinsic noise with high optical efficiency. We have measured the broad-band optical response of ultra-sensitive TES bolometers (NEP$\approx2\rm\ aW/\sqrt Hz$) in the 30--60-$\mu\rm m$ band where radiation is coupled to the detectors with a few-moded conical feedhorn and a hemispherical backshort. We show that these detectors have an optical efficiency of 60% (the ratio of the power detected by the TES bolometer to the total power propagating through the feedhorn). We find that the measured optical efficiency can be understood in terms of the modes propagating through the feedhorn with the aid of a spatial mode-filtering technique., Comment: 22 pages, 11 figures. The following article has been accepted by Review of Scientific Instruments. After it is published, it will be found at http://scitation.aip.org/content/aip/journal/rsi

Published
2016
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18. Sequential Cu(II)-promoted oxidation/[3 + 2] cycloaddition/aromatization tandem reaction for the synthesis of 2-substituted benzo[f]isoindole-4,9-dione

Author

Lin, Zhang-qi, Li, Chao-dong, Su, Jun-yi, Niu, Wen-jie, Gao, Jian-rong, and Li, Yu-jin

Subjects
Ring formation (Chemistry) -- Observations, Copper -- Chemical properties -- Usage, Indole -- Chemical properties -- Production processes, Oxidation-reduction reaction -- Observations, Chemistry
Abstract

An efficient method for the synthesis of 2-substituted benzo[f]isoindole-4,9-dione derivatives from N-substituted iminodiacetates and quinones via a Cu(II)-promoted oxidation/[3 + 2] cycloaddition/aromatization tandem reaction was reported. This tandem reaction uses a wide range of N-substituted iminodiacetate derivatives that contain the chain-alkyl, cycloalkyl, and aryl group on the N-atom. Based on optimized reaction conditions, the desired product of 2-substituted benzo[f]isoindole-4,9-diones was obtained in moderate to excellent yields. Taken together, the promising results of this research would provide an especially efficient strategy to synthesize polysubstituted pyrroles from easy available starting materials and promoted by cheaper [Cu(OAc).sub.2]. Key words: tandem reaction, Cu(II)-promoted, 2-substituted benzo[f]isoindole-4,9-dione, oxidation/[3 + 2] cycloaddition/aromatization. Nous présentons une méthode efficace pour la synthèse des dérivés de benzo[f]isoindole-4,9-dione susbstitués en position 2 à partir d'iminodiacétates N-substitués et de quinones. La méthode proposée fait appel à une réaction en tandem qui consiste en une oxydation catalysée par le Cu(II) suivie d'une cycloaddition [3 + 2] et d'une aromatisation. Cette réaction en tandem admet une grande variété de dérivés d'iminodiacétate N-substitués comportant une chaîne alkyle ou un groupe cycloalkyle ou aryle sur l'atome d'azote. En conditions réactionnelles optimisées, nous avons obtenu le produit désiré, soit les benzo[f]isoindole-4,9-diones substituées en position 2, en rendements modérés à excellents. Pris dans leur ensemble, les résultats prometteurs de ces travaux pourraient constituer une stratégie particulièrement efficace pour synthétiser des pyrroles polysubstitués à partir de produits de départ facilement accessibles et de [Cu(OAc).sub.2], un catalyseur peu coûteux. [Traduit par la Rédaction] Mots-clés : réaction en tandem, catalyse par le Cu(II), benzo[f]isoindole-4,9-dione substitué en position 2, oxidation--cycloaddition [3 + 2]--aromatization., Introduction First-row transition metals have been widely used in the construction of organic molecules and have greatly enriched synthetic chemistry in recent years. (1-5) In particular, due to their lower [...]

Published
2020
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19. Hot electron bolometer heterodyne receiver with a 4.7-THz quantum cascade laser as a local oscillator

Author

Kloosterman, Jenna L., Hayton, Darren J., Ren, Yuan, Kao, Tsung-Yu, Hovenier, Neils, Gao, Jian-Rong, Klapwijk, Teun M., Hu, Qing, Walker, Christopher K., and Reno, John L.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We report on a heterodyne receiver designed to observe the astrophysically important neutral atomic oxygen [OI] line at 4.7448 THz. The local oscillator is a third-order distributed feedback Quantum Cascade Laser operating in continuous wave mode at 4.741 THz. A quasi-optical, superconducting NbN hot electron bolometer is used as the mixer. We recorded a double sideband receiver noise temperature (T^DSB_rec) of 815 K, which is ~7 times the quantum noise limit (h{\nu}/2k_B) and an Allan variance time of 15 s at an effective noise fluctuation bandwidth of 18 MHz. Heterodyne performance was confirmed by measuring a methanol line spectrum., Comment: 12 pages, 5 figures; accepted for publication in the Applied Physics Letters

Published
2012
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22. The 2023 terahertz science and technology roadmap

Author

Leitenstorfer, Alfred, Moskalenko, Andrey S., Kampfrath, Tobias, Kono, Junichiro, Castro-Camus, Enrique, Peng, Kun, Qureshi, Naser, Turchinovich, Dmitry, Tanaka, Koichiro, Markelz, Andrea G., Havenith, Martina, Hough, Cameron, Joyce, Hannah J., Padilla, Willie J., Zhou, Binbin, Kim, Ki Yong, Zhang, Xi Cheng, Jepsen, Peter Uhd, Dhillon, Sukhdeep, Vitiello, Miriam, Linfield, Edmund, Davies, A. Giles, Hoffmann, Matthias C., Lewis, Roger, Tonouchi, Masayoshi, Klarskov, Pernille, Seifert, Tom S., Gerasimenko, Yaroslav A., Mihailovic, Dragan, Huber, Rupert, Boland, Jessica L., Mitrofanov, Oleg, Dean, Paul, Ellison, Brian N., Huggard, Peter G., Rea, Simon P., Walker, Christopher, Leisawitz, David T., Gao, Jian Rong, Li, Chong, Chen, Qin, Valušis, Gintaras, Wallace, Vincent P., Pickwell-MacPherson, Emma, Shang, Xiaobang, Hesler, Jeffrey, Ridler, Nick, Renaud, Cyril C., Kallfass, Ingmar, Nagatsuma, Tadao, Zeitler, J. Axel, Arnone, Don, Johnston, Michael B., Cunningham, John, Leitenstorfer, Alfred, Moskalenko, Andrey S., Kampfrath, Tobias, Kono, Junichiro, Castro-Camus, Enrique, Peng, Kun, Qureshi, Naser, Turchinovich, Dmitry, Tanaka, Koichiro, Markelz, Andrea G., Havenith, Martina, Hough, Cameron, Joyce, Hannah J., Padilla, Willie J., Zhou, Binbin, Kim, Ki Yong, Zhang, Xi Cheng, Jepsen, Peter Uhd, Dhillon, Sukhdeep, Vitiello, Miriam, Linfield, Edmund, Davies, A. Giles, Hoffmann, Matthias C., Lewis, Roger, Tonouchi, Masayoshi, Klarskov, Pernille, Seifert, Tom S., Gerasimenko, Yaroslav A., Mihailovic, Dragan, Huber, Rupert, Boland, Jessica L., Mitrofanov, Oleg, Dean, Paul, Ellison, Brian N., Huggard, Peter G., Rea, Simon P., Walker, Christopher, Leisawitz, David T., Gao, Jian Rong, Li, Chong, Chen, Qin, Valušis, Gintaras, Wallace, Vincent P., Pickwell-MacPherson, Emma, Shang, Xiaobang, Hesler, Jeffrey, Ridler, Nick, Renaud, Cyril C., Kallfass, Ingmar, Nagatsuma, Tadao, Zeitler, J. Axel, Arnone, Don, Johnston, Michael B., and Cunningham, John

Abstract

Terahertz (THz) radiation encompasses a wide spectral range within the electromagnetic spectrum that extends from microwaves to the far infrared (100 GHz-∼30 THz). Within its frequency boundaries exist a broad variety of scientific disciplines that have presented, and continue to present, technical challenges to researchers. During the past 50 years, for instance, the demands of the scientific community have substantially evolved and with a need for advanced instrumentation to support radio astronomy, Earth observation, weather forecasting, security imaging, telecommunications, non-destructive device testing and much more. Furthermore, applications have required an emergence of technology from the laboratory environment to production-scale supply and in-the-field deployments ranging from harsh ground-based locations to deep space. In addressing these requirements, the research and development community has advanced related technology and bridged the transition between electronics and photonics that high frequency operation demands. The multidisciplinary nature of THz work was our stimulus for creating the 2017 THz Science and Technology Roadmap (Dhillon et al 2017 J. Phys. D: Appl. Phys. 50 043001). As one might envisage, though, there remains much to explore both scientifically and technically and the field has continued to develop and expand rapidly. It is timely, therefore, to revise our previous roadmap and in this 2023 version we both provide an update on key developments in established technical areas that have important scientific and public benefit, and highlight new and emerging areas that show particular promise. The developments that we describe thus span from fundamental scientific research, such as THz astronomy and the emergent area of THz quantum optics, to highly applied and commercially and societally impactful subjects that include 6G THz communications, medical imaging, and climate monitoring and prediction. Our Roadmap vision draws upon the ex

Published
2023

23. The Athena X-ray Integral Field Unit: a consolidated design for the system requirement review of the preliminary definition phase

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Barret, Didier, Albouys, Vincent, den Herder, Jan-Willem, Piro, Luigi, Cappi, Massimo, Huovelin, Juhani, Kelley, Richard, Mas-Hesse, J. Miguel, Paltani, Stéphane, Rauw, Gregor, Rozanska, Agata, Bernard, Vivian, Berrocal, Alicia, Audard, Marc, Blin, Sylvie, Bonino, Donata, Frericks, Martin, Bonnet, François, Bonny, Patrick, Boorman, Peter, Ptak, Andy, Chaoul, Laurence, Boreux, Charles, Bounab, Ayoub, Boutelier, Martin, Boyce, Kevin, Brienza, Daniele, Bandler, Simon, Bruijn, Marcel, Gabici, Stefano, Bulgarelli, Andrea, Calarco, Simona, Raulin, Desi, Gloaguen, Emilie, Callanan, Paul, Prada Campello, Alberto, Camus, Thierry, Canourgues, Florent, Capobianco, Vito, Cardiel, Nicolas, Castellani, Florent, Barbera, Marco, Gant, Florent, Simionescu, Aurora, Cheatom, Oscar, Doumayrou, Eric, Chervenak, James, Chiarello, Fabio, Clerc, Laurent, Clerc, Nicolas, Cobo, Beatriz, Coeur-Joly, Odile, Coleiro, Alexis, Colonges, Stéphane, Torrejon, Jose M., Corcione, Leonardo, Gao, Jian-Rong, Puccetti, Simonetta, Barcons, Xavier, Coriat, Mickael, Coynel, Alexandre, Cuttaia, Francesco, D’Ai, Antonino, D’anca, Fabio, Dadina, Mauro, Acero, Fabio, Daniel, Christophe, Dauner, Lea, DeNigris, Natalie, Puccio, Elena, Gastaldello, Fabio, Dercksen, Johannes, Bozzo, Enrico, DiPirro, Michael, Genolet, Ludovic, Durkin, Malcom, van Leeuwen, Bert-Joost, Charles, Ivan, Ghizzardi, Simona, Alcacera Gil, M. Angeles, Giovannini, Elisa, Ramon, Pascale, Godet, Olivier, Gomez-Elvira, Javier, Gonzalez, Raoul, Gonzalez, Manuel, Gottardi, Luciano, Branduardi-Raymont, Graziella, Granat, Dolorès, Fioretti, Valentina, Gros, Michel, Costantini, Elisa, Guignard, Nicolas, Reina, Manuel, Hieltjes, Paul, Hurtado, Adolfo Jesús, Irwin, Kent, Jacquey, Christian, Ettori, Stefano, Janiuk, Agnieszka, Jaubert, Jean, Jiménez, Maria, Geoffray, Hervé, Jolly, Antoine, Jourdan, Thierry, Rioland, Guillaume, Dauser, Thomas, Julien, Sabine, Kedziora, Bartosz, Finoguenov, Alexis, Korb, Andrew, Kreykenbohm, Ingo, König, Ole, Langer, Mathieu, Laudet, Philippe, Jacques, Lionel, Laurent, Philippe, Rodriguez, Louis, Laurenza, Monica, Lesrel, Jean, Etcheverry, Christophe, Decourchelle, Anne, Ligori, Sebastiano, Lorenz, Maximilian, Luminari, Alfredo, Maffei, Bruno, Maisonnave, Océane, Marelli, Lorenzo, Kirsch, Christian, Roig, Anton, Massonet, Didier, Petit, Pascal, Maussang, Irwin, Melchor, Alejandro Gonzalo, Le Mer, Isabelle, Duband, Lionel, San Millan, Francisco Javier, Millerioux, Jean-Pierre, Mineo, Teresa, Minervini, Gabriele, Molin, Alexeï, Gatti, Flavio, Grosso, Nicolas, Smith, Stephen, Monestes, David, Montinaro, Nicola, Mot, Baptiste, Murat, David, Nagayoshi, Kenichiro, Duval, Jean-Marc, Nazé, Yaël, Noguès, Loïc, Pailot, Damien, Kaastra, Jelle, Rollet, Bertrand, Panessa, Francesca, Adams, Joseph, Parodi, Luigi, Roncarelli, Mauro, Dubbeldam, Luc, Hoogeveen, Ruud, Roudil, Gilles, Rudnicki, Tomasz, Sanisidro, Julien, Mazzotta, Pasquale, Sciortino, Luisa, Silva, Vitor, Sordet, Michael, Soto-Aguilar, Javier, Spizzi, Pierre, Goldwurm, Andrea, Dupieux, Michel, Surace, Christian, Svoboda, Jiri, Fernández Sánchez, Miguel, Miller, Jon, Taralli, Emanuele, Terrasa, Guilhem, Terrier, Régis, Todaro, Michela, Ubertini, Pietro, Uslenghi, Michela, Vaate, Jan Geralt Bijd de, Dupourqué, Simon, Vaccaro, Davide, den Hartog, Roland, Miniutti, Giovanni, van der Hulst, Paul, Varisco, Salvatore, Varnière, Peggy, Vibert, Laurent, Vidriales, María, Villa, Fabrizio, Vodopivec, Boris Martin, Volpe, Angela, Durand, Jean Louis, Vries, Cor de, Nicastro, Fabrizio, Wakeham, Nicholas, Walmsley, Gavin, Kiviranta, Mikko, Jackson, Brian, Wise, Michael, Wit, Martin de, Woźniak, Grzegorz, Jonker, Peter, Kilbourne, Caroline, Eckert, Dominique, Sciortino, Salvatore, Korpela, Seppo, Macculi, Claudio, Mendez, Mariano, Mitsuda, Kazuhisa, van der Kuur, Jan, Molendi, Silvano, Pajot, François, Pointecouteau, Etienne, Porter, Frederick, Pratt, Gabriel W., van Loon, Dennis, Eiriz, Valvanera, Prêle, Damien, Ravera, Laurent, Sato, Kosuke, Schaye, Joop, Shinozaki, Keisuke, Ledot, Aurélien, Skup, Konrad, Soucek, Jan, Thibert, Tanguy, Yamaguchi, Hiroya, Vink, Jacco, Ercolani, Eric, Webb, Natalie, Beaumont, Sophie, Piconcelli, Enrico, Ceballos, Maria Teresa, Cucchetti, Edoardo, D’Andrea, Matteo, Eckart, Megan, Ferrando, Philippe, Kammoun, Elias, Lotti, Simone, Mesnager, Jean-Michel, Natalucci, Lorenzo, Lyautey, Bertrand, Pinto, Ciro, Peille, Philippe, Doriese, William, de Plaa, Jelle, Ardellier, Florence, Argan, Andrea, Bellouard, Elise, Carron, Jérôme, Cavazzuti, Elisabetta, Fiorini, Mauro, Khosropanah, Pourya, Encinas Plaza, Jose Miguel, Martin, Sylvain, Parot, Yann, Finkbeiner, Fred, Perry, James, Pinsard, Frederic, Pradines, Alice, Rigano, Manuela, Roelfsema, Peter, Schwander, Denis, Torrioli, Guido, Plaza, Borja, Ullom, Joel, Vera, Isabel, Medinaceli Villegas, Eduardo, Fiocchi, Mariateresa, Sakai, Kazuhiro, Zuchniak, Monika, Brachet, Frank, Lo Cicero, Ugo, van Weers, Henk, Wilms, Joern, Fiore, Fabrizio, Abdoelkariem, Shariefa, Adam, Thomas, Adami, Christophe, Aicardi, Corinne, Fossecave, Hervé, Akamatsu, Hiroki, Merino Alonso, Pablo Eleazar, Amato, Roberta, André, Jérôme, Angelinelli, Matteo, Poyatos, David, Anon-Cancela, Manuel, Yamasaki, Noriko, Anvar, Shebli, Atienza, Ricardo, Attard, Anthony, Franssen, Philippe, Auricchio, Natalia, Balado, Ana, Bancel, Florian, Barusso, Lorenzo Ferrari, Prouvé, Thomas, Bascuñan, Arturo, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Barret, Didier, Albouys, Vincent, den Herder, Jan-Willem, Piro, Luigi, Cappi, Massimo, Huovelin, Juhani, Kelley, Richard, Mas-Hesse, J. Miguel, Paltani, Stéphane, Rauw, Gregor, Rozanska, Agata, Bernard, Vivian, Berrocal, Alicia, Audard, Marc, Blin, Sylvie, Bonino, Donata, Frericks, Martin, Bonnet, François, Bonny, Patrick, Boorman, Peter, Ptak, Andy, Chaoul, Laurence, Boreux, Charles, Bounab, Ayoub, Boutelier, Martin, Boyce, Kevin, Brienza, Daniele, Bandler, Simon, Bruijn, Marcel, Gabici, Stefano, Bulgarelli, Andrea, Calarco, Simona, Raulin, Desi, Gloaguen, Emilie, Callanan, Paul, Prada Campello, Alberto, Camus, Thierry, Canourgues, Florent, Capobianco, Vito, Cardiel, Nicolas, Castellani, Florent, Barbera, Marco, Gant, Florent, Simionescu, Aurora, Cheatom, Oscar, Doumayrou, Eric, Chervenak, James, Chiarello, Fabio, Clerc, Laurent, Clerc, Nicolas, Cobo, Beatriz, Coeur-Joly, Odile, Coleiro, Alexis, Colonges, Stéphane, Torrejon, Jose M., Corcione, Leonardo, Gao, Jian-Rong, Puccetti, Simonetta, Barcons, Xavier, Coriat, Mickael, Coynel, Alexandre, Cuttaia, Francesco, D’Ai, Antonino, D’anca, Fabio, Dadina, Mauro, Acero, Fabio, Daniel, Christophe, Dauner, Lea, DeNigris, Natalie, Puccio, Elena, Gastaldello, Fabio, Dercksen, Johannes, Bozzo, Enrico, DiPirro, Michael, Genolet, Ludovic, Durkin, Malcom, van Leeuwen, Bert-Joost, Charles, Ivan, Ghizzardi, Simona, Alcacera Gil, M. Angeles, Giovannini, Elisa, Ramon, Pascale, Godet, Olivier, Gomez-Elvira, Javier, Gonzalez, Raoul, Gonzalez, Manuel, Gottardi, Luciano, Branduardi-Raymont, Graziella, Granat, Dolorès, Fioretti, Valentina, Gros, Michel, Costantini, Elisa, Guignard, Nicolas, Reina, Manuel, Hieltjes, Paul, Hurtado, Adolfo Jesús, Irwin, Kent, Jacquey, Christian, Ettori, Stefano, Janiuk, Agnieszka, Jaubert, Jean, Jiménez, Maria, Geoffray, Hervé, Jolly, Antoine, Jourdan, Thierry, Rioland, Guillaume, Dauser, Thomas, Julien, Sabine, Kedziora, Bartosz, Finoguenov, Alexis, Korb, Andrew, Kreykenbohm, Ingo, König, Ole, Langer, Mathieu, Laudet, Philippe, Jacques, Lionel, Laurent, Philippe, Rodriguez, Louis, Laurenza, Monica, Lesrel, Jean, Etcheverry, Christophe, Decourchelle, Anne, Ligori, Sebastiano, Lorenz, Maximilian, Luminari, Alfredo, Maffei, Bruno, Maisonnave, Océane, Marelli, Lorenzo, Kirsch, Christian, Roig, Anton, Massonet, Didier, Petit, Pascal, Maussang, Irwin, Melchor, Alejandro Gonzalo, Le Mer, Isabelle, Duband, Lionel, San Millan, Francisco Javier, Millerioux, Jean-Pierre, Mineo, Teresa, Minervini, Gabriele, Molin, Alexeï, Gatti, Flavio, Grosso, Nicolas, Smith, Stephen, Monestes, David, Montinaro, Nicola, Mot, Baptiste, Murat, David, Nagayoshi, Kenichiro, Duval, Jean-Marc, Nazé, Yaël, Noguès, Loïc, Pailot, Damien, Kaastra, Jelle, Rollet, Bertrand, Panessa, Francesca, Adams, Joseph, Parodi, Luigi, Roncarelli, Mauro, Dubbeldam, Luc, Hoogeveen, Ruud, Roudil, Gilles, Rudnicki, Tomasz, Sanisidro, Julien, Mazzotta, Pasquale, Sciortino, Luisa, Silva, Vitor, Sordet, Michael, Soto-Aguilar, Javier, Spizzi, Pierre, Goldwurm, Andrea, Dupieux, Michel, Surace, Christian, Svoboda, Jiri, Fernández Sánchez, Miguel, Miller, Jon, Taralli, Emanuele, Terrasa, Guilhem, Terrier, Régis, Todaro, Michela, Ubertini, Pietro, Uslenghi, Michela, Vaate, Jan Geralt Bijd de, Dupourqué, Simon, Vaccaro, Davide, den Hartog, Roland, Miniutti, Giovanni, van der Hulst, Paul, Varisco, Salvatore, Varnière, Peggy, Vibert, Laurent, Vidriales, María, Villa, Fabrizio, Vodopivec, Boris Martin, Volpe, Angela, Durand, Jean Louis, Vries, Cor de, Nicastro, Fabrizio, Wakeham, Nicholas, Walmsley, Gavin, Kiviranta, Mikko, Jackson, Brian, Wise, Michael, Wit, Martin de, Woźniak, Grzegorz, Jonker, Peter, Kilbourne, Caroline, Eckert, Dominique, Sciortino, Salvatore, Korpela, Seppo, Macculi, Claudio, Mendez, Mariano, Mitsuda, Kazuhisa, van der Kuur, Jan, Molendi, Silvano, Pajot, François, Pointecouteau, Etienne, Porter, Frederick, Pratt, Gabriel W., van Loon, Dennis, Eiriz, Valvanera, Prêle, Damien, Ravera, Laurent, Sato, Kosuke, Schaye, Joop, Shinozaki, Keisuke, Ledot, Aurélien, Skup, Konrad, Soucek, Jan, Thibert, Tanguy, Yamaguchi, Hiroya, Vink, Jacco, Ercolani, Eric, Webb, Natalie, Beaumont, Sophie, Piconcelli, Enrico, Ceballos, Maria Teresa, Cucchetti, Edoardo, D’Andrea, Matteo, Eckart, Megan, Ferrando, Philippe, Kammoun, Elias, Lotti, Simone, Mesnager, Jean-Michel, Natalucci, Lorenzo, Lyautey, Bertrand, Pinto, Ciro, Peille, Philippe, Doriese, William, de Plaa, Jelle, Ardellier, Florence, Argan, Andrea, Bellouard, Elise, Carron, Jérôme, Cavazzuti, Elisabetta, Fiorini, Mauro, Khosropanah, Pourya, Encinas Plaza, Jose Miguel, Martin, Sylvain, Parot, Yann, Finkbeiner, Fred, Perry, James, Pinsard, Frederic, Pradines, Alice, Rigano, Manuela, Roelfsema, Peter, Schwander, Denis, Torrioli, Guido, Plaza, Borja, Ullom, Joel, Vera, Isabel, Medinaceli Villegas, Eduardo, Fiocchi, Mariateresa, Sakai, Kazuhiro, Zuchniak, Monika, Brachet, Frank, Lo Cicero, Ugo, van Weers, Henk, Wilms, Joern, Fiore, Fabrizio, Abdoelkariem, Shariefa, Adam, Thomas, Adami, Christophe, Aicardi, Corinne, Fossecave, Hervé, Akamatsu, Hiroki, Merino Alonso, Pablo Eleazar, Amato, Roberta, André, Jérôme, Angelinelli, Matteo, Poyatos, David, Anon-Cancela, Manuel, Yamasaki, Noriko, Anvar, Shebli, Atienza, Ricardo, Attard, Anthony, Franssen, Philippe, Auricchio, Natalia, Balado, Ana, Bancel, Florian, Barusso, Lorenzo Ferrari, Prouvé, Thomas, and Bascuñan, Arturo

Abstract

The Athena X-ray Integral Unit (X-IFU) is the high resolution X-ray spectrometer studied since 2015 for flying in the mid-30s on the Athena space X-ray Observatory. Athena is a versatile observatory designed to address the Hot and Energetic Universe science theme, as selected in November 2013 by the Survey Science Committee. Based on a large format array of Transition Edge Sensors (TES), X-IFU aims to provide spatially resolved X-ray spectroscopy, with a spectral resolution of 2.5 eV (up to 7 keV) over a hexagonal field of view of 5 arc minutes (equivalent diameter). The X-IFU entered its System Requirement Review (SRR) in June 2022, at about the same time when ESA called for an overall X-IFU redesign (including the X-IFU cryostat and the cooling chain), due to an unanticipated cost overrun of Athena. In this paper, after illustrating the breakthrough capabilities of the X-IFU, we describe the instrument as presented at its SRR (i.e. in the course of its preliminary definition phase, so-called B1), browsing through all the subsystems and associated requirements. We then show the instrument budgets, with a particular emphasis on the anticipated budgets of some of its key performance parameters, such as the instrument efficiency, spectral resolution, energy scale knowledge, count rate capability, non X-ray background and target of opportunity efficiency. Finally, we briefly discuss the ongoing key technology demonstration activities, the calibration and the activities foreseen in the X-IFU Instrument Science Center, touch on communication and outreach activities, the consortium organisation and the life cycle assessment of X-IFU aiming at minimising the environmental footprint, associated with the development of the instrument. Thanks to the studies conducted so far on X-IFU, it is expected that along the design-to-cost exercise requested by ESA, the X-IFU will maintain flagship capabilities in spatially resolved high resolution X-ray spectroscopy, enabling most of th

Published
2023

24. Electromagnetic performance comparisons of 0.85 THz integrated bias-tee SIS mixers with twin-junction and end-loaded tuning schemes

Author

Tan, Boon Kok, Rudakov, Kirill, Koshelets, Valery P., Khudchenko, Andrey, Baryshev, Andrey M., Yassin, Ghassan, Zmuidzinas, Jonas, Gao, Jian-Rong, and Astronomy

Subjects
Electromagnetism, Millimetre/Sub-Millimetre Astronomy, Heterodyne Technique, Terahertz Technology, Superconductor-Insulator-Superconductor (SIS) mixer
Abstract

We compare the design of two 0.85 THz SIS mixers fed with a radial probe antenna aligned to the E-Plane of the input full-height rectangular waveguide connected to a drilled smooth-walled horn. Both designs employ the same 0.5 μm2hybrid Nb/AlN/NbN tunnel junction technology, sandwiched between a NbTiN ground and aluminium wiring layer fabricated on top of a 40 μm quartz substrate. The two designs is differed by how we tune out the unwanted junction capacitance for broadband performance. The first design uses the commonly-used twin-junction tuning scheme; whilst the second design utilises an end-loaded scheme. We successfully achieve close to 2× the double sideband quantum noise performance for both schemes, but the twin-junction design is less sensitive to fabrication accuracy of planar circuit components utilised. However, the end-loaded design offers a much better IF bandwidth performance, almost twice wider than the twin-junction design. The need for an ultra-wide IF bandwidth mixer is becoming more pressing and important for the future and up-coming upgrades of various millimetre (mm) and sub-mm astronomical instruments, hence we conclude that the end-loaded design is a better solution for the THz heterodyne mixing applications.

Published
2022

25. 39 THz spatial filter based on a back-to-back Si-lens system

Author

Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Gan, Yuner, Mirzaei, Behnam, van der Poel, Sebastiaan, Silva, Jose RG, Finkel, Matvey, Eggens, Martin, Ridder, Marcel, Khalatpour, Ali, Hu, Qing, van der Tak, Floris, Gao, Jian-Rong, Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Gan, Yuner, Mirzaei, Behnam, van der Poel, Sebastiaan, Silva, Jose RG, Finkel, Matvey, Eggens, Martin, Ridder, Marcel, Khalatpour, Ali, Hu, Qing, van der Tak, Floris, and Gao, Jian-Rong

Abstract

© 2020 Optical Society of America under the terms of the OSA Open Access Publishing Agreement. We present a terahertz spatial filter consisting of two back-to-back (B2B) mounted elliptical silicon lenses and an opening aperture defined on a thin gold layer between the lenses. The beam filtering efficiency of the B2B lens system is investigated by simulation and experiment. Using a unidirectional antenna coupled 3rd-order distributed feedback (DFB) quantum cascade laser (QCL) at 3.86 THz as the source, the B2B lens system shows 72% transmissivity experimentally with a fundamental Gaussian mode as the input, in reasonably good agreement with the simulated value of 80%. With a proper aperture size, the B2B lens system is capable of filtering the non-Gaussian beam from the QCL to a nearly fundamental Gaussian beam, where Gaussicity increases from 74% to 99%, and achieves a transmissivity larger than 30%. Thus, this approach is proven to be an effective beam shaping technique for QCLs, making them to be suitable local oscillators in the terahertz range with a Gaussian beam. Besides, the B2B lens system is applicable to a wide frequency range if the wavelength dependent part is properly scaled.

Published
2022

26. 47 THz asymmetric beam multiplexer for GUSTO

Author

Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Mirzaei, Behnam, Gan, Yuner, Finkel, Matvey, Groppi, Christopher, Young, Abram, Walker, Christopher, Hu, Qing, Gao, Jian-Rong, Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Mirzaei, Behnam, Gan, Yuner, Finkel, Matvey, Groppi, Christopher, Young, Abram, Walker, Christopher, Hu, Qing, and Gao, Jian-Rong

Abstract

A full demonstration of the Fourier phase grating used as 4.7 THz local oscillator (LO) multiplexer for Galactic/Extragalactic ULDB Spectroscopic Terahertz Observatory (GUSTO) is presented in this paper, including its design, modeling, tolerance analysis, and experimental characterizations of the angular and intensity distributions among 2 × 4 output beams and the power efficiency. A quantum cascade laser (QCL) is used to generate the input beam for evaluation of the grating performance in its all relevant aspects with an accuracy level never reported before, where good agreements with modeling results are found. This is the first asymmetric-profile grating fully modelled and characterized at a THz frequency, that further confirms the versatility of this technology for providing an intermediate optical element for feeding multiple array detectors with a single radiation source at such a scientifically interesting frequency regime.

Published
2022

27. An engineered bacterial therapeutic lowers urinary oxalate in preclinical models and in silico simulations of enteric hyperoxaluria

Author

Lubkowicz, David, primary, Horvath, Nicholas G, additional, James, Michael J, additional, Cantarella, Pasquale, additional, Renaud, Lauren, additional, Bergeron, Christopher G, additional, Shmueli, Ron B, additional, Anderson, Cami, additional, Gao, Jian‐Rong, additional, Kurtz, Caroline B, additional, Perreault, Mylene, additional, Charbonneau, Mark R, additional, Isabella, Vincent M, additional, and Hava, David L, additional

Published
2022
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28. 5.3 THz MgB2 hot electron bolometer mixer operated at 20 K

Author

Gao, J.R., Gan, Y., Mirzaei, B., Silva, J. R.G., Cherednichenko, S., Zmuidzinas, Jonas, and Gao, Jian-Rong

Subjects
Hot electron bolometer, IF bandwidth, superconductor, space instrumentation, MgB2, high Tc, THz, mixer
Abstract

Heterodyne receivers combining a NbN HEB mixer with a local oscillator (LO) are the work horse for high resolution (≥106) spectroscopic observations at supra-terahertz frequencies. We report an MgB2 HEB mixer working at 5.3 THz with20 K operation temperature based on a previously published paper [Y. Gan et al, Appl. Phys. Lett., 119, 202601 (2021)]. The HEB consists of a 7 nm thick MgB2 submicron-bridge contacted with a spiral antenna. It has a Tc of 38.4 K. By using hot/cold blackbody loads and a Mylar beam splitter all in vacuum, and applying a 5.25 THz FIR gas laser as the LO, we measured a minimal DSB receiver noise temperature of 3960 K. The latter gives a DSB mixer noise temperature of 1470 K. This sensitivity is 28 times better than a room temperature Schottky mixer at 4.7 THz, but about 2.5 times less sensitive than an NbN HEB mixer. The latter must be operated around 4 K. The IF noise bandwidth is about 10 GHz, which is 2.5-3 times larger than an NbN HEB. With further optimization, such MgB2 HEBs are expected to reach a better sensitivity. That the low noise, wide IF bandwidth MgB2 HEB mixers can be operated in a compact, low dissipation 20 K Stirling cooler can significantly reduce the cost and complexity of heterodyne instruments and therefore facilitate new space missions.

Published
2022

29. Thermal Crosstalk of X-Ray Transition-Edge Sensor Micro-Calorimeters Under Frequency Domain Multiplexing Readout

Author

Vaccaro, Davide, primary, Akamatsu, Hiroki, additional, Bruijn, Marcel, additional, Gottardi, Luciano, additional, den Hartog, Roland, additional, van der Kuur, Jan, additional, van der Linden, Ton, additional, Nagayoshi, Kenishiro, additional, Ravensberg, Kevin, additional, Ridder, Marcel, additional, Taralli, Emanuele, additional, de Wit, Martin, additional, Gao, Jian-Rong, additional, Hoogeveen, Ruud, additional, and den Herder, Jan-Willem, additional

Published
2022
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30. Ti/Au TES 32 × 32 Pixel Array: Uniformity, Thermal Crosstalk and Performance at Different X-Ray Energies

Author

Taralli, Emanuele, primary, D'Andrea, Matteo, additional, Gottardi, Luciano, additional, Nagayoshi, Kenishiro, additional, Ridder, Marcel, additional, de Wit, Martin, additional, Visser, Sven, additional, Vaccaro, Davide, additional, Akamatsu, Hiroki, additional, Ravensberg, Kevin, additional, Hoogeveen, Ruud, additional, Bruijn, Marcel, additional, and Gao, Jian-Rong, additional

Published
2021
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31. Single Pixel Performance of a 32 × 32 Ti/Au TES Array With Broadband X-Ray Spectra

Author

D'Andrea, Matteo, primary, Taralli, Emanuele, additional, Akamatsu, Hiroki, additional, Gottardi, Luciano, additional, Nagayoshi, Kenichiro, additional, Ravensberg, Kevin, additional, Ridder, Marcel L., additional, Vaccaro, Davide, additional, de Vries, Cor P., additional, de Wit, Martin, additional, Bruijn, Marcel P., additional, Hoogeveen, Ruud W. M., additional, and Gao, Jian-Rong, additional

Published
2021
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32. 4.7 THz asymmetric beam multiplexer for GUSTO

Author

Mirzaei, Behnam, primary, Gan, Yuner, additional, Finkel, Matvey, additional, Groppi, Christopher, additional, Young, Abram, additional, Walker, Christopher, additional, Hu, Qing, additional, and Gao, Jian-Rong, additional

Published
2021
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33. 4×2 HEB receiver at 4.7 THz for GUSTO

Author

Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Silva, Jose R., Mirzaei, Behnam, Laauwen, Wouter, Hu, Qing, Groppi, Christopher E., Walker, Christopher, Gao, Jian-Rong, More, Nikhil, Young, Abram, Khalatpour, Ali, Kulesa, Craig, Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Silva, Jose R., Mirzaei, Behnam, Laauwen, Wouter, Hu, Qing, Groppi, Christopher E., Walker, Christopher, Gao, Jian-Rong, More, Nikhil, Young, Abram, Khalatpour, Ali, and Kulesa, Craig

Abstract

© 2018 SPIE. GUSTO will be a NASA balloon borne terahertz observatory to be launched from Antarctica in late 2021 for a flight duration of 100-170 days. It aims at reviewing the life cycle of interstellar medium of our galaxy by simultaneously mapping the three brightest interstellar cooling lines: [OI] at 4.7 THz, [CII] at 1.9 THz, and [NII] at 1.4 THz; along the 124 degrees of the galactic plane and through a part of the Large Magellanic Cloud. It will use three arrays of 4x2 mixers based on NbN hot electron bolometers (HEBs), which are currently the most sensitive mixers for high resolution spectroscopic astronomy at these frequencies. Here we report on the design of a novel 4.7 THz receiver for GUSTO. The receiver consists mainly of two subsystems: a 4×2 HEB quasi-optical mixer array and a 4.7 THz multi-beam LO. We describe the mixer array, which is designed as a compact monolithic unit. We show, for example, 10 potential HEB detectors with the state of the art sensitivity of 720 K measured at 2.5 THz. They have a small variation in sensitivity, being less than 3%, while also meet the LO uniformity requirements. For the multi-beam LO we demonstrate the combination of a phase grating and a single QCL at 4.7 THz, which generates 8 sub-LO beams, where the phase grating shows an efficiency of 75%. A preliminary concept for the integrated LO unit, including QCL, phase grating and beam matching optics is presented.

Published
2021

34. Characterization of low-loss hydrogenated amorphous silicon films for superconducting resonators

Author

Buijtendorp, B.T., Bueno, J., Thoen, David, Sberna, V. Murugesan P.M., Baselmans, J.J.A., Vollebregt, S., Endo, A., Zmuidzinas, Jonas, and Gao, Jian-Rong

Subjects
Amorphous silicon, Materials science, business.industry, Millimeter-wave, Astrophysics::Cosmology and Extragalactic Astrophysics, Kinetic Inductance Detectors, Chemical vapor deposition, Dielectric, Substrate (electronics), Spectrometer, Amorphous Silicon, Condensed Matter::Materials Science, Resonator, chemistry.chemical_compound, chemistry, Submillimeter-wave, Two-level Systems, Optoelectronics, Dissipation factor, Dielectric loss, Dielectric Loss, business, Filter Bank, Microwave
Abstract

Superconducting resonators used in millimeter-submillimeter astronomy would greatly benefit from deposited dielectrics with a small dielectric loss. We deposited hydrogenated amorphous silicon films using plasma-enhanced chemical vapor deposition, at substrate temperatures of 100°C, 250°C and 350° C. The measured void volume fraction, hydrogen content, microstructure parameter, and bond-angle disorder are negatively correlated with the substrate temperature. All three films have a loss tangent below $10^{-5}$ for a resonator energy of $10^5$ photons, at 120 mK and 4-7 GHz. This makes these films promising for microwave kinetic inductance detectors and on-chip millimeter-submilimeter filters.

Published
2020

35. Simulating the Radiation Loss of Superconducting Submillimeter Wave Filters and Transmission Lines Using Sonnet EM

Author

Endo, A., Pascual Laguna, A., Hähnle, S.A., Karatsu, K., Thoen, David, Murugesan, V., Baselmans, J.J.A., Zmuidzinas, Jonas, and Gao, Jian-Rong

Subjects
FOS: Physical sciences, Millimeter-wave, Integrated circuit, Kinetic Inductance Detectors, Radiation, law.invention, Superconductivity (cond-mat.supr-con), Resonator, Optics, law, Radiative transfer, Instrumentation and Methods for Astrophysics (astro-ph.IM), Instrumentation, Coplanar Waveguide, Electronic circuit, Physics, business.industry, Mechanical Engineering, Coplanar waveguide, Condensed Matter - Superconductivity, Astronomy and Astrophysics, Electronic, Optical and Magnetic Materials, astronomy, Astronomical Instrumentation, Integrated Superconducting Spectrometer, Electric power transmission, Space and Planetary Science, Control and Systems Engineering, Submillimeter-wave, DESHIMA, Extremely high frequency, business, Astrophysics - Instrumentation and Methods for Astrophysics, Simulation
Abstract

Superconducting resonators and transmission lines are fundamental building blocks of integrated circuits for millimeter-submillimeter astronomy. Accurate simulation of radiation loss from the circuit is crucial for the design of these circuits because radiation loss increases with frequency, and can thereby deteriorate the system performance. Here we show a stratification for a 2.5-dimensional method-of-moment simulator Sonnet EM that enables accurate simulations of the radiative resonant behavior of submillimeter-wave coplanar resonators and straight coplanar waveguides (CPWs). The Sonnet simulation agrees well with the measurement of the transmission through a coplanar resonant filter at 374.6 GHz. Our Sonnet stratification utilizes artificial lossy layers below the lossless substrate to absorb the radiation, and we use co-calibrated internal ports for de-embedding. With this type of stratification, Sonnet can be used to model superconducting millimeter-submillimeter wave circuits even when radiation loss is a potential concern., Presented at the SPIE Astronomical Telescopes + Instrumentation 2020. Full published paper, poster and video available at https://doi.org/10.1117/12.2560458

Published
2020

36. Observing low elevation sky and the CMB Cold Spot with BICEP3 at the South Pole

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Kang, Jae Hwan, Ade, P. A. R., Ahmed, Zeeshan, Amiri, Mandana, Barkats, Denis, Basu Thakur, R., Bischoff, Colin A., Bock, J. J., Boenish, Hans, Bullock, Eric, Buza, Victor, Cheshire, James R., Connors, Jake, Cornelison, James, Crumrine, Michael, Cukierman, Ari Jozef, Denison, Edward, Dierickx, Marion, Duband, Lionel, Eiben, Miranda, Fatigoni, Sofia, Filippini, Jeff P., Fliescher, Stefan, Goeckner-Wald, Neil, Goldfinger, David, Grayson, James A., Grimes, Paul, Hall, Grantland, Halpern, Mark, Harrison, Sam A., Henderson, Shawn, Hildebrandt, S. R., Hilton, Gene C., Hubmayr, Johannes, Hui, H., Irwin, Kent D., Karkare, Kirit S., Karpel, Ethan, Kefeli, S., Kernasovskiy, Sarah A., Kovac, John M., Kuo, Chao-Lin, Lau, King, Leitch, Erik M., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Yuka, Namikawa, Toshiya, Nguyen, H. T., O'Brient, R., Ogburn, IV, R. Walt, Palladino, Steven, Precup, Nathan, Prouve, Thomas, Pryke, Clement, Racine, Benjamin, Reintsema, Carl D., Richter, Steffen, Schillaci, A., Schmitt, Benjamin, Schwarz, Robert, Sheehy, Chris D., Soliman, A., St Germaine, Tyler, Steinbach, B., Sudiwala, Rashmi, Teply, Grant, Thompson, Keith L., Tolan, James E., Tucker, Carole, Turner, A. D., Umiltà, Caterina, Vieregg, Abigail G., Wandui, A., Weber, A. C., Wiebe, Don, Willmert, Justin, Wong, Chin Lin, Wu, Wai Ling K., Yang, Hung-I, Yoon, Ki Won, Young, Edward, Yu, Cyndia, Zeng, Lingzhen, Zhang, C., Zhang, S., Zmuidzinas, Jonas, Gao, Jian-Rong, Kang, Jae Hwan, Ade, P. A. R., Ahmed, Zeeshan, Amiri, Mandana, Barkats, Denis, Basu Thakur, R., Bischoff, Colin A., Bock, J. J., Boenish, Hans, Bullock, Eric, Buza, Victor, Cheshire, James R., Connors, Jake, Cornelison, James, Crumrine, Michael, Cukierman, Ari Jozef, Denison, Edward, Dierickx, Marion, Duband, Lionel, Eiben, Miranda, Fatigoni, Sofia, Filippini, Jeff P., Fliescher, Stefan, Goeckner-Wald, Neil, Goldfinger, David, Grayson, James A., Grimes, Paul, Hall, Grantland, Halpern, Mark, Harrison, Sam A., Henderson, Shawn, Hildebrandt, S. R., Hilton, Gene C., Hubmayr, Johannes, Hui, H., Irwin, Kent D., Karkare, Kirit S., Karpel, Ethan, Kefeli, S., Kernasovskiy, Sarah A., Kovac, John M., Kuo, Chao-Lin, Lau, King, Leitch, Erik M., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Yuka, Namikawa, Toshiya, Nguyen, H. T., O'Brient, R., Ogburn, IV, R. Walt, Palladino, Steven, Precup, Nathan, Prouve, Thomas, Pryke, Clement, Racine, Benjamin, Reintsema, Carl D., Richter, Steffen, Schillaci, A., Schmitt, Benjamin, Schwarz, Robert, Sheehy, Chris D., Soliman, A., St Germaine, Tyler, Steinbach, B., Sudiwala, Rashmi, Teply, Grant, Thompson, Keith L., Tolan, James E., Tucker, Carole, Turner, A. D., Umiltà, Caterina, Vieregg, Abigail G., Wandui, A., Weber, A. C., Wiebe, Don, Willmert, Justin, Wong, Chin Lin, Wu, Wai Ling K., Yang, Hung-I, Yoon, Ki Won, Young, Edward, Yu, Cyndia, Zeng, Lingzhen, Zhang, C., and Zhang, S.

Abstract

BICEP3 is a 520 mm aperture on-axis refracting telescope at the South Pole, which observes the polarization of the cosmic microwave background (CMB) at 95 GHz to search for the B-mode signal from inflationary gravitational waves. In addition to this main target, we have developed a low-elevation observation strategy to extend coverage of the Southern sky at the South Pole, where BICEP3 can quickly achieve degree-scale E-mode measurements over a large area. An interesting E-mode measurement is probing a potential polarization anomaly around the CMB Cold Spot. During the austral summer seasons of 2018-19 and 2019-20, BICEP3 observed the sky with a flat mirror to redirect the beams to various low elevation ranges. The preliminary data analysis shows degree-scale E-modes measured with high signal-to-noise ratio.

Published
2020

37. Polarization calibration of the BICEP3 CMB polarimeter at the South Pole

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Cornelison, J., Ade, P. A. R., Ahmed, Zeeshan, Amiri, Mandana, Barkats, Denis, Basu Thakur, R., Bischoff, Colin, Bock, J. J., Boenish, Hans, Bullock, Eric, Buza, Victor, Cheshire, James R., Connors, Jake, Crumrine, Michael, Cukierman, Ari J., Denison, Edward, Dierickx, Marion, Duband, Lionel, Eiben, Miranda, Fatigoni, Sofia, Filippini, Jeff, Fliescher, Stefan, Goeckner-Wald, Neil, Goldfinger, David C., Grayson, James A., Grimes, Paul, Hall, Grantland, Halal, George, Halpern, Mark, Harrison, Samuel, Henderson, Shawn, Hildebrandt, S. R., Hilton, Gene C., Hubmayr, Johannes, Hui, H., Irwin, Kent D., Kang, Jae Hwan, Karkare, Kirit, Karpel, Ethan, Kefeli, S., Kernasovkiy, Sarah A., Kovac, John M., Kuo, Chao-Lin, Lau, King, Leitch, Eric, Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Yuka, Namikawa, Toshiya, Nguyen, H. T., O'Brient, R., Ogburn, R W., Palladino, Steven, Precup, Nathan, Prouve, Thomas, Pryke, Clement, Racine, Benjamin, Reintsema, Carl D., Richter, Steffen, Schillaci, A., Schmitt, Benjamin, Schwarz, Robert, Sheehy, Christopher D., Soliman, A., St. Germaine, T., Steinbach, B., Sudiwala, Rashmi, Teply, G. P., Thompson, Keith, Tolan, James E., Tucker, Carole, Turner, A. D., Umilita, Caterina, Vieregg, Abigail G., Wandui, A., Weber, A. C., Wiebe, Don, Willmert, Justin, Wong, Chin Lin, Wu, Kimmy, Yang, Eric, Yoon, Ki Won, Young, Edward, Yu, Cyndia, Zeng, Lingzhen, Zhang, C., Zhang, S., Zmuidzinas, Jonas, Gao, Jian-Rong, Cornelison, J., Ade, P. A. R., Ahmed, Zeeshan, Amiri, Mandana, Barkats, Denis, Basu Thakur, R., Bischoff, Colin, Bock, J. J., Boenish, Hans, Bullock, Eric, Buza, Victor, Cheshire, James R., Connors, Jake, Crumrine, Michael, Cukierman, Ari J., Denison, Edward, Dierickx, Marion, Duband, Lionel, Eiben, Miranda, Fatigoni, Sofia, Filippini, Jeff, Fliescher, Stefan, Goeckner-Wald, Neil, Goldfinger, David C., Grayson, James A., Grimes, Paul, Hall, Grantland, Halal, George, Halpern, Mark, Harrison, Samuel, Henderson, Shawn, Hildebrandt, S. R., Hilton, Gene C., Hubmayr, Johannes, Hui, H., Irwin, Kent D., Kang, Jae Hwan, Karkare, Kirit, Karpel, Ethan, Kefeli, S., Kernasovkiy, Sarah A., Kovac, John M., Kuo, Chao-Lin, Lau, King, Leitch, Eric, Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Yuka, Namikawa, Toshiya, Nguyen, H. T., O'Brient, R., Ogburn, R W., Palladino, Steven, Precup, Nathan, Prouve, Thomas, Pryke, Clement, Racine, Benjamin, Reintsema, Carl D., Richter, Steffen, Schillaci, A., Schmitt, Benjamin, Schwarz, Robert, Sheehy, Christopher D., Soliman, A., St. Germaine, T., Steinbach, B., Sudiwala, Rashmi, Teply, G. P., Thompson, Keith, Tolan, James E., Tucker, Carole, Turner, A. D., Umilita, Caterina, Vieregg, Abigail G., Wandui, A., Weber, A. C., Wiebe, Don, Willmert, Justin, Wong, Chin Lin, Wu, Kimmy, Yang, Eric, Yoon, Ki Won, Young, Edward, Yu, Cyndia, Zeng, Lingzhen, Zhang, C., and Zhang, S.

Abstract

The BICEP3 CMB Polarimeter is a small-aperture refracting telescope located at the South Pole and is specifically designed to search for the possible signature of inflationary gravitational waves in the Cosmic Microwave Background (CMB). The experiment measures polarization on the sky by differencing the signal of co-located, orthogonally polarized antennas coupled to Transition Edge Sensor (TES) detectors. We present precise measurements of the absolute polarization response angles and polarization efficiencies for nearly all of BICEP3's ~800 functioning polarization-sensitive detector pairs from calibration data taken in January 2018. Using a Rotating Polarized Source (RPS), we mapped polarization response for each detector over a full 360 degrees of source rotation and at multiple telescope boresight rotations from which per-pair polarization properties were estimated. In future work, these results will be used to constrain signals predicted by exotic physical models such as Cosmic Birefringence.

Published
2020

38. A four kilopixel 150 GHz KID imager paired with a 1.5 m crossed Dragone telescope

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Sayers, Jack, Day, Peter K., Cunnane, Daniel P., Eom, Byeong Ho, LeDuc, Henry G., O'Brient, Roger C., Runyan, Marcus C., Bryan, Sean A., Gordon, Samuel B., Mauskopf, Philip D., Johnson, Bradley R., McCarrick, Heather, Bhandarkar, Tanay A., Zmuidzinas, Jonas, Gao, Jian-Rong, Sayers, Jack, Day, Peter K., Cunnane, Daniel P., Eom, Byeong Ho, LeDuc, Henry G., O'Brient, Roger C., Runyan, Marcus C., Bryan, Sean A., Gordon, Samuel B., Mauskopf, Philip D., Johnson, Bradley R., McCarrick, Heather, and Bhandarkar, Tanay A.

Abstract

I will describe our development of a four kilopixel photometric imaging camera paired with a 1.5 meter crossed Dragone telescope. The focal plane is composed of aluminum kinetic inductance detectors (KIDs) fabricated on crystalline silicon tiles. The tiles contain 960 KIDs and are approximately 100 mm x 100 mm in size. KID pairs, each sensitive to an orthogonal linear polarization, are coupled to a waveguide/feedhorn machined from aluminum. A single block, with 480 waveguides/feedhorns arranged in a hexagonal close-pack configuration, is paired with each detector tile. Initial tests with prototype KID tiles show the expected noise and optical performance. Full-scale tiles have now been fabricated with >90% yield, and are currently being characterized. The imager is intended for terrestrial applications, and an initial demonstration with the telescope is planned for early 2020. With relatively minor changes to the KID design, it could also be optimized for astronomical applications.

Published
2020

39. A status update on TIME: a mm-wavelength spectrometer designed to probe the Epoch of Reionization

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Crites, Abigail T., Bock, Jamie, Bradford, Matt, Butler, Victoria, Chang, Tzu-Ching, Cheng, Yun-Ting, Emerson, Nick, Frez, Clifford, Hunacek, Jon, Keenan, Ryan, Li, Chao-Te, Madonia, Paolo, Marrone, Daniel, Moncelsi, Lorenzo, Prouve, Thomas, Sun, Guochao, Trumper, Isaac, Turner, Anthony, Weber, Alexis, Wei, Ta-Shun, Zemcov, Mike, Case-Cortes, Tess, Zmuidzinas, Jonas, Gao, Jian-Rong, Crites, Abigail T., Bock, Jamie, Bradford, Matt, Butler, Victoria, Chang, Tzu-Ching, Cheng, Yun-Ting, Emerson, Nick, Frez, Clifford, Hunacek, Jon, Keenan, Ryan, Li, Chao-Te, Madonia, Paolo, Marrone, Daniel, Moncelsi, Lorenzo, Prouve, Thomas, Sun, Guochao, Trumper, Isaac, Turner, Anthony, Weber, Alexis, Wei, Ta-Shun, Zemcov, Mike, and Case-Cortes, Tess

Abstract

TIME is an instrument being developed to study emission from faint objects in our universe using line intensity mapping (LIM) to understand the universe over cosmic time. The TIME instrument is a mm-wavelength grating spectrometer with Transition Edge Sensor (TES) bolometers measuring in the frequency range of 200-300 GHz with 60 spectral pixels and 16 spatial pixels. TIME will measure [CII] emission from redshift 5 to 9 to probe the evolution of our universe during the epoch of reionization. TIME will also measure low-redshift CO fluctuations and map molecular gas in the epoch of peak cosmic star formation from redshift 0.5 to 2. This instrument and the emerging technique of LIM will provide complementary measurements to typical galaxy surveys and illuminate the history of our universe. TIME was recently installed on the 12m ALMA prototype antenna operated by the Arizona Radio Observatory on Kitt Peak for an engineering test and will return for science observations in 2020.

Published
2020

40. Design and pre-flight performance of SPIDER 280 GHz receivers

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Shaw, E. C., Ade, P.A.R., Akers, S., Amiri, M., Austermann, Jason E., Beall, James A., Becker, D.T., Benton, S.J., Bergman, A. S., Bock, J. J., Bond, J.R., Bryan, S.A., Chiang, H.C., Contaldi, C.R., Domagalski, R.S., Doré, O., Duff, S. M., Duivenvoorden, A.J., Eriksen, H.K., Farhang, M., Filippini, J. P., Fissel, L.M., Fraisse, A.A., Freese, K., Galloway, M., Gambrel, A. E., Gandilo, N.N., Ganga, K., Grigorian, A., Gualtieri, R, Gudmundsson, J.E., Halpern, M., Hartley, J., Hasselfield, M., Hilton, G., Holmes, W., Hristov, V. V., Huang, Z., Hubmayr, Johannes, Irwin, K.D., Jones, W.C., Kahn, A., Kuo, C.L., Kermish, Z.D., Lennox, A., Leung, J. S.-Y., Megerian, K., Reintsema, C., Li, S., Mason, P. V., Runyan, M. C., Moncelsi, L., Morford, T. A., Nagy, J.M., Nie, R., Mocanu, L. M., Padilla, I.L., Netterfield, C. B., Osherson, B., Rahlin, A.S., Redmond, S., Turner, A. D., Romualdez, L.J., Nolta, M., Ruhl, J.E., Shariff, J.A., Shiu, C., Soler, J.D., Song, X., Trangsrud, A., Thommesen, H., Tucker, C, Tucker, R. S., Ullom, Joel, van der List, J.F., Van Lanen, Jeff, Vissers, M. R., Weber, A. C., Wen, S., Wehus, I.K., Wiebe, D.V., Young, E.Y., Zmuidzinas, Jonas, Gao, Jian-Rong, Shaw, E. C., Ade, P.A.R., Akers, S., Amiri, M., Austermann, Jason E., Beall, James A., Becker, D.T., Benton, S.J., Bergman, A. S., Bock, J. J., Bond, J.R., Bryan, S.A., Chiang, H.C., Contaldi, C.R., Domagalski, R.S., Doré, O., Duff, S. M., Duivenvoorden, A.J., Eriksen, H.K., Farhang, M., Filippini, J. P., Fissel, L.M., Fraisse, A.A., Freese, K., Galloway, M., Gambrel, A. E., Gandilo, N.N., Ganga, K., Grigorian, A., Gualtieri, R, Gudmundsson, J.E., Halpern, M., Hartley, J., Hasselfield, M., Hilton, G., Holmes, W., Hristov, V. V., Huang, Z., Hubmayr, Johannes, Irwin, K.D., Jones, W.C., Kahn, A., Kuo, C.L., Kermish, Z.D., Lennox, A., Leung, J. S.-Y., Megerian, K., Reintsema, C., Li, S., Mason, P. V., Runyan, M. C., Moncelsi, L., Morford, T. A., Nagy, J.M., Nie, R., Mocanu, L. M., Padilla, I.L., Netterfield, C. B., Osherson, B., Rahlin, A.S., Redmond, S., Turner, A. D., Romualdez, L.J., Nolta, M., Ruhl, J.E., Shariff, J.A., Shiu, C., Soler, J.D., Song, X., Trangsrud, A., Thommesen, H., Tucker, C, Tucker, R. S., Ullom, Joel, van der List, J.F., Van Lanen, Jeff, Vissers, M. R., Weber, A. C., Wen, S., Wehus, I.K., Wiebe, D.V., and Young, E.Y.

Abstract

In this work we describe upgrades to the Spider balloon-borne telescope in preparation for its second flight, currently planned for December 2021. The Spider instrument is optimized to search for a primordial B-mode polarization signature in the cosmic microwave background at degree angular scales. During its first flight in 2015, Spider mapped ~10% of the sky at 95 and 150 GHz. The payload for the second Antarctic flight will incorporate three new 280 GHz receivers alongside three refurbished 95- and 150 GHz receivers from Spider's first flight. In this work we discuss the design and characterization of these new receivers, which employ over 1500 feedhorn-coupled transition-edge sensors. We describe pre-flight laboratory measurements of detector properties, and the optical performance of completed receivers. These receivers will map a wide area of the sky at 280 GHz, providing new information on polarized Galactic dust emission that will help to separate it from the cosmological signal.

Published
2020

41. SuperSpec: On-chip spectrometer design, characterization, and performance

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Redford, Joseph G., Barry, Peter S., Bradford, Charles M., Chapman, Scott, Glenn, Jason, Hailey-Dunsheath, Steven, Janssen, Reinier M. J., Karkare, Kirit S., LeDuc, Henry G., Mauskopf, Philip, McGeehan, Ryan, Shirokoff, Erik, Wheeler, Jordan, Zmuidzinas, J., Zmuidzinas, Jonas, Gao, Jian-Rong, Redford, Joseph G., Barry, Peter S., Bradford, Charles M., Chapman, Scott, Glenn, Jason, Hailey-Dunsheath, Steven, Janssen, Reinier M. J., Karkare, Kirit S., LeDuc, Henry G., Mauskopf, Philip, McGeehan, Ryan, Shirokoff, Erik, Wheeler, Jordan, and Zmuidzinas, J.

Abstract

SuperSpec is an integrated, on-chip spectrometer for millimeter and sub-millimeter astronomy. SuperSpec is demonstrating a proof-of-principle multi-beam spectrometer on the sky at the Large Millimeter Telescope (LMT) in Mexico covering the 200 - 300 GHz frequency range with moderate resolution (R ~ 270 - 290). The dual-polarization, three-pixel instrument will consist of 6 SuperSpec spectrometer chips. We present the design and characterization of the devices being used in the first SuperSpec demonstration along with lab testing of the instrument performance.

Published
2020

42. Upgrading the field-imaging far-infrared line spectrometer for the Stratospheric Observatory for Infrared Astronomy (SOFIA) with KIDs: enabling large sample (extragalactic) surveys

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Colditz, Sebastian, Looney, Leslie W., Bigiel, Frank, Fischer, Christian, Fischer, Jacqueline, Hailey-Dunsheath, Steven, Herrera-Camus, Rodrigo, Krabbe, Alfred, LeDuc, Henry G., Wong, Tony, Zmuidzinas, Jonas, Gao, Jian-Rong, Colditz, Sebastian, Looney, Leslie W., Bigiel, Frank, Fischer, Christian, Fischer, Jacqueline, Hailey-Dunsheath, Steven, Herrera-Camus, Rodrigo, Krabbe, Alfred, LeDuc, Henry G., and Wong, Tony

Abstract

We present the initial design, performance improvements and science opportunities for an upgrade to the Field-Imaging Far-Infrared Line Spectrometer (FIFI-LS). FIFI-LS efficiently measures fine structure cooling lines, delivering critical constraints of the interstellar medium and starforming environments. SOFIA provides the only FIR observational capability in the world, making FIFI-LS a workhorse for FIR lines, combining optimal spectral resolution and a wide velocity range. Its continuous coverage from 51-203 microns makes FIFI-LS a versatile tool to investigate a multitude of diagnostic lines within our galaxy and in extragalactic environments. The sensitivity and field-of-view (FOV) of FIFI-LS are limited by its 90s-era photoconductor arrays. These limits can be overcome by upgrading the instrument using the latest developments in Kinetic Inductance Detectors (KIDs). KIDs provide sensitivity gains in excess of 1.4 and allow larger arrays, enabling an increase in pixel count by an order of magnitude. This increase allows a wider FOV and instantaneous velocity coverage. The upgrade provides gains in point source observation speed by a factor <2 and in mapping speed by a factor <3.5, enabled by the improved sensitivity and pixel count. This upgrade has been proposed to NASA in response to the 2018 SOFIA Next Generation Instrumentation call.

Published
2020

43. Terahertz intensity mapper focal plane and array design

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Janssen, Reinier M. J., Liu, Lunjun, Nie, Rong, Fu, Jianyang, Trumper, Isaac, Hailey-Dunsheath, Steve, Bradford, Charles M., Filippini, Jeffrey P., Zmuidzinas, Jonas, Gao, Jian-Rong, Janssen, Reinier M. J., Liu, Lunjun, Nie, Rong, Fu, Jianyang, Trumper, Isaac, Hailey-Dunsheath, Steve, Bradford, Charles M., and Filippini, Jeffrey P.

Abstract

TIM, the Terahertz Intensity Mapper, is a NASA balloon mission designed to perform [CII] intensity mapping of the peak of cosmic star formation. To achieve this, TIM has two longslit (1 degree slit length) grating spectrometers covering the 240-317 um and 317-420 um wavelength bands at R~250, respectively. We will present the design of the ~4000 pixel, horn-coupled kinetic inductance detector arrays servicing each of the spectrometer arms. Each pixel is a lumped-element superconducting resonator made from a 20 nm thick aluminum film, designed to achieve photon noise limited performance at 100 fW of loading. The inductor is a meandered narrow wire, designed to mimic a metal mesh grid at THz frequencies; it is optimized for absorption of both polarizations delivered by the circular waveguide. Each array will consist of four quadrants containing ~1000 pixels on a single microstrip readout line and will be mounted such that critical parameters of the absorber design are maintained.

Published
2020

44. Antenna-coupled thermal kinetic inductance detectors for ground-based millimeter-wave cosmology

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Wandui, Albert K., Bock, James J., Frez, Clifford, Hunacek, Jon, Minutolo, Lorenzo, Nguyen, Hien, Steinbach, Bryan, Turner, Anthony, O'Brient, Roger, Zmuidzinas, Jonas, Gao, Jian-Rong, Wandui, Albert K., Bock, James J., Frez, Clifford, Hunacek, Jon, Minutolo, Lorenzo, Nguyen, Hien, Steinbach, Bryan, Turner, Anthony, and O'Brient, Roger

Abstract

We present our design for antenna-coupled thermal kinetic inductance detectors (TKIDs) designed for Cosmic Microwave Background (CMB) observations in the 150 GHz band. The next generation of telescopes studying the CMB will require large arrays of detectors on cryogenic focal planes to achieve high sensitivity at the cost of increased integration and readout complexity. TKIDs have demonstrated photon-limited noise performance comparable to traditional bolometers with a radiofrequency (RF) multiplexing architecture that enables the large detector counts needed. We characterize TKIDs fabricated for observing the CMB in a frequency band centered at 150 GHz and discuss the optical performance. These devices are a critical step towards fielding a Keck Array camera with 512 devices on the focal plane at the South Pole.

Published
2020

45. Detection chain and electronic readout of the QUBIC instrument

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Stankowiak, G., Piat, Michel, Battistelli, Elia, D'Alessandro, Giuseppe, de Bernardis, Paolo, De Petris, Marco, González, Manuel, Grandsire, Laurent, Hamilton, Jean-Christophe, Hoang, T. D., Masi, Silvia, Marnieros, Stefanos, Mennella, Aniello, Mousset, L., O'Sullivan, Creidhe, Prêle, Damien, Tartari, Andrea, Thermeau, Jean-Pierre, Torchinsky, Steve, Voisin, Fabrice, Zannoni, Mario, Ade, Peter, Alberro, J. G., Almela, A., Amico, Giorgio, Arnaldi, L. H., Auguste, D., Aumont, Jonathan, Azzoni, Susanna, Banfi, Stefano, Bélier, Benoit, Baù, Alessandro, Bennett, David G., Bergé, Laurent, Bernard, Jean-Philippe, Bersanelli, Marco, Bigot-Sazy, Marie-Anne, Bonaparte, J., Bonis, J., Bunn, Emory, Burke, David, Buzi, Daniele, Cavaliere, Francesco, Chanial, Pierre, Chapron, Claude, Charlassier, Romain, Cobos Cerutti, A. C., Columbro, Fabio, Coppolecchia, Alessandro, de Gasperis, Giancarlo, De Leo, M., Dheilly, Stéphane, Duca, C., Dumoulin, Louis, Etchegoyen, Alberto, Fasciszewski, A., Ferreyro, L. P., Fracchia, D., Franceschet, Cristian, Gamboa Lerena, Martin M., Ganga, Kenneth, García, Beatriz, García Redondo, M. E., Gaspard, M., Gayer, Donnacha, Gervasi, Massimo, Giard, Martin, Gilles, V., Giraud-Héraud, Y., Gómez Berisso, M., Gradziel, Marcin L., Hampel, M. R., Harari, Diego, Henrot-Versillé, Sophie, Incardona, Federico, Jules, E., Kaplan, Jean, Kristukat, Christian, Lamagna, Luca, Loucatos, Sotiris, Louis, Thibaut, Maffei, Bruno, Marty, Wilfried, Mattei, Angelo, May, Andrew, McCulloch, Mark, Mele, Lorenzo, Melo, D., Montier, Ludovic, Mundo, Luis M., Murphy, J. Anthony, Murphy, James D., Nati, Federico, Olivieri, E., Oriol, Christine, Paiella, Alessandro, Pajot, François, Passerini, Andrea, Pastoriza, Hernan, Pelosi, Alessandro, Perbost, Camille, Perciballi, M., Pezzotta, Federico, Piacentini, Francesco, Piccirillo, Lucio, Pisano, Giampaolo, Platino, M., Polenta, Gianluca, Puddu, Roberto, Rambaud, Damien, Ringegni, Pablo Lorenzo, Romero, Gustavo Esteban, Rasztocky, E., Salum, J. M., Schillaci, Alessandro, Scóccola, Claudia, Scully, Stephen, Spinelli, Sebastiano, Stolpovskiy, Mikhail, Supanitsky, A. D., Timbie, Peter, Tomasi, Maurizio, Tucker, Gregory, Tucker, Carole, Viganò, Daniele, Vittorio, Nicola, Wicek, Francois, Wright, M., Zullo, Antonio, Zmuidzinas, Jonas, Gao, Jian-Rong, Stankowiak, G., Piat, Michel, Battistelli, Elia, D'Alessandro, Giuseppe, de Bernardis, Paolo, De Petris, Marco, González, Manuel, Grandsire, Laurent, Hamilton, Jean-Christophe, Hoang, T. D., Masi, Silvia, Marnieros, Stefanos, Mennella, Aniello, Mousset, L., O'Sullivan, Creidhe, Prêle, Damien, Tartari, Andrea, Thermeau, Jean-Pierre, Torchinsky, Steve, Voisin, Fabrice, Zannoni, Mario, Ade, Peter, Alberro, J. G., Almela, A., Amico, Giorgio, Arnaldi, L. H., Auguste, D., Aumont, Jonathan, Azzoni, Susanna, Banfi, Stefano, Bélier, Benoit, Baù, Alessandro, Bennett, David G., Bergé, Laurent, Bernard, Jean-Philippe, Bersanelli, Marco, Bigot-Sazy, Marie-Anne, Bonaparte, J., Bonis, J., Bunn, Emory, Burke, David, Buzi, Daniele, Cavaliere, Francesco, Chanial, Pierre, Chapron, Claude, Charlassier, Romain, Cobos Cerutti, A. C., Columbro, Fabio, Coppolecchia, Alessandro, de Gasperis, Giancarlo, De Leo, M., Dheilly, Stéphane, Duca, C., Dumoulin, Louis, Etchegoyen, Alberto, Fasciszewski, A., Ferreyro, L. P., Fracchia, D., Franceschet, Cristian, Gamboa Lerena, Martin M., Ganga, Kenneth, García, Beatriz, García Redondo, M. E., Gaspard, M., Gayer, Donnacha, Gervasi, Massimo, Giard, Martin, Gilles, V., Giraud-Héraud, Y., Gómez Berisso, M., Gradziel, Marcin L., Hampel, M. R., Harari, Diego, Henrot-Versillé, Sophie, Incardona, Federico, Jules, E., Kaplan, Jean, Kristukat, Christian, Lamagna, Luca, Loucatos, Sotiris, Louis, Thibaut, Maffei, Bruno, Marty, Wilfried, Mattei, Angelo, May, Andrew, McCulloch, Mark, Mele, Lorenzo, Melo, D., Montier, Ludovic, Mundo, Luis M., Murphy, J. Anthony, Murphy, James D., Nati, Federico, Olivieri, E., Oriol, Christine, Paiella, Alessandro, Pajot, François, Passerini, Andrea, Pastoriza, Hernan, Pelosi, Alessandro, Perbost, Camille, Perciballi, M., Pezzotta, Federico, Piacentini, Francesco, Piccirillo, Lucio, Pisano, Giampaolo, Platino, M., Polenta, Gianluca, Puddu, Roberto, Rambaud, Damien, Ringegni, Pablo Lorenzo, Romero, Gustavo Esteban, Rasztocky, E., Salum, J. M., Schillaci, Alessandro, Scóccola, Claudia, Scully, Stephen, Spinelli, Sebastiano, Stolpovskiy, Mikhail, Supanitsky, A. D., Timbie, Peter, Tomasi, Maurizio, Tucker, Gregory, Tucker, Carole, Viganò, Daniele, Vittorio, Nicola, Wicek, Francois, Wright, M., and Zullo, Antonio

Abstract

The Q and U Bolometric Interferometer for Cosmology (QUBIC) Technical Demonstrator (TD) aiming to shows the feasibility of the combination of interferometry and bolometric detection. The electronic readout system is based on an array of 128 NbSi Transition Edge Sensors cooled at 350mK readout with 128 SQUIDs at 1K controlled and amplified by an Application Specific Integrated Circuit at 40K. This readout design allows a 128:1 Time Domain Multiplexing. We report the design and the performance of the detection chain in this paper. The technological demonstrator unwent a campaign of test in the lab. Evaluation of the QUBIC bolometers and readout electronics includes the measurement of I-V curves, time constant and the Noise Equivalent Power. Currently the mean Noise Equivalent Power is ~ 2 x 10⁻¹⁶ W/√Hz.

Published
2020

47. Submillimeter superconducting integrated receivers: Fabrication and Yield

Author

Filippenko, Lyudmila V., Shitov, Sergey V., Dmitriev, Pavel, N., Ermakov, Andrey B., Koshelets, Valery P., and Gao, Jian-Rong

Subjects
Superconductors -- Research, Business, Electronics, Electronics and electrical industries
Abstract

Superconducting integrating receivers were fabricated and a yield analysis undertaken.

Published
2001

48. Nb superconducting hot electron bolometer mixers coupled with microstrip lines

Author

Ganzevles, Walter F.M., Yagoubov, Pavel, Gao, Jian Rong, Klapwijk, Teun M., and de Korte, Piet A.J.

Subjects
Mixers (Electronics) -- Research, Strip transmission lines -- Analysis, Business, Electronics, Electronics and electrical industries
Abstract

A study of a superconducting Nb hot-electron bolometer mixer with quasi-optical coupling is presented with emphasis on its response at 2.5 terahertz. A new coupling circuit with microstrip lines is incorporated in this mixer.

Published
2001

49. 3.9 THz spatial filter based on a back-to-back Si-lens system

Author

Gan, Yuner, primary, Mirzaei, Behnam, additional, van der Poel, Sebastiaan, additional, Silva, Jose R. G., additional, Finkel, Matvey, additional, Eggens, Martin, additional, Ridder, Marcel, additional, Khalatpour, Ali, additional, Hu, Qing, additional, van der Tak, Floris, additional, and Gao, Jian-Rong, additional

Published
2020
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