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1. CCAT: LED Mapping and Characterization of the 280 GHz TiN KID Array

Author

Middleton, Alicia, Choi, Steve K., Walker, Samantha, Austermann, Jason, Burgoyne, James R., Butler, Victoria, Chapman, Scott C., Crites, Abigail T., Duell, Cody J., Freundt, Rodrigo G., Huber, Anthony I., Huber, Zachary B., Hubmayr, Johannes, Keller, Ben, Lin, Lawrence T., Niemack, Michael D., Patel, Darshan, Sinclair, Adrian K., Smith, Ema, Vaskuri, Anna, Vavagiakis, Eve M., Vissers, Michael, Wang, Yuhan, and Wheeler, Jordan

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

Prime-Cam, one of the primary instruments for the Fred Young Submillimeter Telescope (FYST) developed by the CCAT Collaboration, will house up to seven instrument modules, with the first operating at 280 GHz. Each module will include three arrays of superconducting microwave kinetic inductance detectors (KIDs). The first KID array fabricated for the 280 GHz module uses titanium-nitride (TiN) as the superconducting material and has 3,456 individual detectors, while the other two arrays use aluminum. This paper presents the design and laboratory characterization of the 280 GHz TiN array, which is cooled below its critical temperature to ~0.1 K and read out over six RF feedlines. LED mapping, a technique for matching the measured resonant frequency of a detector to its physical position, was performed on the array so that the results can be used to lithographically trim the KID capacitors and increase the yield of the array by reducing frequency collisions. We present the methods and results of LED mapping the 280 GHz TiN KID array before deployment on FYST., Comment: 4 pages, 4 figures, submitted to IEEE Transactions on Applied Superconductivity (IEEE TAS)

Published
2024

2. CCAT: A status update on the EoR-Spec instrument module for Prime-Cam

Author

Freundt, Rodrigo, Li, Yaqiong, Henke, Doug, Austermann, Jason, Burgoyne, James R., Chapman, Scott, Choi, Steve K., Duell, Cody J., Huber, Zach, Niemack, Michael, Nikola, Thomas, Lin, Lawrence, Riechers, Dominik A., Stacey, Gordon, Vaskuri, Anna K., Vavagiakis, Eve M., Wheeler, Jordan, and Zou, Bugao

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

The Epoch of Reionization Spectrometer (EoR-Spec) is an upcoming Line Intensity Mapping (LIM) instrument designed to study the evolution of the early universe (z = 3.5 to 8) by probing the redshifted [CII] 158 $\mu$m fine-structure line from aggregates of galaxies. The [CII] emission is an excellent tracer of star formation since it is the dominant cooling line from neutral gas heated by OB star light and thus can be used to probe the reionization of the early Universe due to star formation. EoR-Spec will be deployed on Prime-Cam, a modular direct-detection receiver for the 6-meter Fred Young Submillimeter Telescope (FYST), currently under construction by CPI Vertex Antennentechnik GmbH and to be installed near the summit of Cerro Chajnantor in the Atacama Desert. This instrument features an image plane populated with more than 6500 Microwave Kinetic Inductance Detectors (MKIDs) that are illuminated by a 4-lens optical design with a cryogenic, scanning Fabry-Perot Interferometer (FPI) at the pupil of the optical system. The FPI is designed to provide a spectral resolving power of $R\sim100$ over the full spectral range of 210--420 GHz. EoR-Spec will tomographically survey the E-COSMOS and E-CDFS fields with a depth of about 4000 hours over a 5 year period. Here we give an update on EoR-Spec's final mechanical/optical design and the current status of fabrication, characterization and testing towards first light in 2026., Comment: Presented at SPIE Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XII

Published
2024
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3. CCAT: Nonlinear effects in 280 GHz aluminum kinetic inductance detectors

Author

Duell, Cody J., Austermann, Jason, Burgoyne, James R., Chapman, Scott C., Choi, Steve K., Crites, Abigail T., Freundt, Rodrigo G., Huber, Anthony I., Huber, Zachary B., Hubmayr, Johannes, Keller, Ben, Lin, Lawrence T., Middleton, Alicia M., Murphy, Colin C., Niemack, Michael D., Nikola, Thomas, Patel, Darshan, Sinclair, Adrian K., Smith, Ema, Stacey, Gordon J., Vaskuri, Anna, Vavagiakis, Eve M., Vissers, Michael, Walker, Samantha, and Wheeler, Jordan

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Prime-Cam, a first-generation science instrument for the Atacama-based Fred Young Submillimeter Telescope, is being built by the CCAT Collaboration to observe at millimeter and submillimeter wavelengths using kinetic inductance detectors (KIDs). Prime-Cam's 280 GHz instrument module will deploy with two aluminum-based KID arrays and one titanium nitride-based KID array, totaling approximately 10,000 detectors at the focal plane, all of which have been fabricated and are currently undergoing testing. One complication of fielding large arrays of KIDs under dynamic loading conditions is tuning the detector tone powers to maximize signal-to-noise while avoiding bifurcation due to the nonlinear kinetic inductance. For aluminum-based KIDs, this is further complicated by additional nonlinear effects which couple tone power to resonator quality factors and resonant frequencies. While both nonequilibrium quasiparticle dynamics and two-level system fluctuations have been shown to give rise to qualitatively similar distortions, modeling these effects alongside nonlinear kinetic inductance is inefficient when fitting thousands of resonators on-sky with existing models. For this reason, it is necessary to have a detailed understanding of the nonlinear effects across relevant detector loading conditions, including how they impact on on-sky noise and how to diagnose the detector's relative performance. We present a study of the competing nonlinearities seen in Prime-Cam's 280 GHz aluminum KIDs, with a particular emphasis on the resulting distortions to the resonator line shape and how these impact detector parameter estimation., Comment: 10 pages, 4 figures, Conference proceedings from SPIE Astronomical Telescopes + Instrumentation (AS24)

Published
2024
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4. CCAT: Comparisons of 280 GHz TiN and Al Kinetic Inductance Detector Arrays

Author

Duell, Cody J., Austermann, Jason, Beall, James, Burgoyne, James R., Chapman, Scott C., Choi, Steve K., Freundt, Rodrigo G., Gao, Jiansong, Groppi, Christopher, Huber, Anthony I., Huber, Zachary B., Hubmayr, Johannes, Keller, Ben, Li, Yaqiong, Lin, Lawrence T., Matthewson, Justin, Mauskopf, Philip, Middleton, Alicia, Murphy, Colin C., Niemack, Michael D., Nikola, Thomas, Sinclair, Adrian K., Smith, Ema, van Lanen, Jeff, Vaskuri, Anna, Vavagiakis, Eve M., Vissers, Michael, Walker, Samantha, Wheeler, Jordan, and Zou, Bugao

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The CCAT Collaboration's six-meter Fred Young Submillimeter Telescope is scheduled to begin observing in the Chilean Atacama in 2025, targeting a variety of science goals throughout cosmic history. Prime-Cam is a 1.8-meter diameter cryostat that will host up to seven independent instrument modules designed for simultaneous spectroscopic and broadband, polarimetric surveys at millimeter to submillimeter wavelengths. The first of these instrument modules, the 280 GHz module, will include ${\sim}$10,000 kinetic inductance detectors (KIDs) across three arrays. While the first array was fabricated out of tri-layer TiN/Ti/TiN, the other two arrays were fabricated out of a single layer of Al. This combination of materials within the same instrument provides a unique opportunity to directly compare the performance and noise properties of two different detector materials that are seeing increasing use within the field. We present preliminary comparisons here based on lab testing, along with a discussion of the potential impacts on operation when observing and translating raw data to science-grade maps., Comment: 6 pages, 3 figures, conference proceedings submitted to the Journal of Low Temperature Physics

Published
2024

5. The BLAST Observatory: A Sensitivity Study for Far-IR Balloon-borne Polarimeters

Author

The BLAST Observatory Collaboration, Coppi, Gabriele, Dicker, Simon, Aguirre, James E., Austermann, Jason E., Beall, James A., Clark, Susan E., Cox, Erin G., Devlin, Mark J., Fissel, Laura M., Galitzki, Nicholas, Hensley, Brandon S., Hubmayr, Johannes, Molinari, Sergio, Nati, Federico, Novak, Giles, Schisano, Eugenio, Soler, Juan D., Tucker, Carole E., Ullom, Joel N., Vaskuri, Anna, Vissers, Michael R., Wheeler, Jordan D., and Zannoni, Mario

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Sensitive wide-field observations of polarized thermal emission from interstellar dust grains will allow astronomers to address key outstanding questions about the life cycle of matter and energy driving the formation of stars and the evolution of galaxies. Stratospheric balloon-borne telescopes can map this polarized emission at far-infrared wavelengths near the peak of the dust thermal spectrum - wavelengths that are inaccessible from the ground. In this paper we address the sensitivity achievable by a Super Pressure Balloon (SPB) polarimetry mission, using as an example the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) Observatory. By launching from Wanaka, New Zealand, BLAST Observatory can obtain a 30-day flight with excellent sky coverage - overcoming limitations of past experiments that suffered from short flight duration and/or launch sites with poor coverage of nearby star-forming regions. This proposed polarimetry mission will map large regions of the sky at sub-arcminute resolution, with simultaneous observations at 175, 250, and 350 $\mu m$, using a total of 8274 microwave kinetic inductance detectors. Here, we describe the scientific motivation for the BLAST Observatory, the proposed implementation, and the forecasting methods used to predict its sensitivity. We also compare our forecasted experiment sensitivity with other facilities., Comment: Published in PASP

Published
2024
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8. CCAT: nonlinear effects in 280 GHz aluminum kinetic inductance detectors

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Duell, Cody J., Austermann, Jason, Burgoyne, James R., Chapman, Scott C., Choi, Steve K., Crites, Abigail T., Freundt, Rodrigo G., Huber, Anthony I., Huber, Zachary B., Hubmayr, Johannes, Keller, Ben, Lin, Lawrence T., Middleton, Alicia M., Murphy, Colin C., Niemack, Michael D., Nikola, Thomas, Patel, Darshan, Sinclair, Adrian K., Smith, Ema, Stacey, Gordon J., Vaskuri, Anna, Vavagiakis, Eve M., Vissers, Michael, Walker, Samantha, and Wheeler, Jordan

Published
2024
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9. CCAT: a status update on the EoR-Spec instrument module for Prime-Cam

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Freundt, Rodrigo, Li, Yaqiong, Henke, Doug, Austermann, Jason, Burgoyne, James R., Chapman, Scott, Choi, Steve K., Duell, Cody J., Huber, Zach, Niemack, Michael, Nikola, Thomas, Lin, Lawrence, Riechers, Dominik A., Stacey, Gordon, Vaskuri, Anna K., Vavagiakis, Eve M., Wheeler, Jordan, and Zou, Bugao

Published
2024
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11. MOSFET-based HTS flux pump

Author

Jurčo, Róbert, primary, Vaskuri, Anna, additional, Curé, Benoit, additional, Dudarev, Alexey, additional, and Mentink, Matthias, additional

Published
2023
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15. Characteristics of Aluminium-Stabilized HTS Detector Magnet Cable at 4 K and 5 T

Author

Vaskuri, Anna K., Van den Eijnden, Joep L., Cure, Benoit, Dudarev, Alexey, and Mentink, Matthias

Abstract

A high-temperature superconducting (HTS) cable for future particle detector magnets has been developed using a 99.3% pure aluminium alloy as a stabilizer for the HTS. This HTS conductor features a stack of four ReBCO tapes (4 mm wide, SuperOx) soldered to a tin-coated copper-clad aluminium alloy cable profile using tin–lead solder at 188 °C. Here, we experimentally demonstrate that the cable withstands both thermal cycling between 4 K and room temperature and Lorentz forces induced by external magnetic field of 5 T when the HTS cable is driven by 4.5 kA. The HTS cable has no visual damage and no change in the critical current after being exposed multiple times to these extreme conditions. We show that since the phase transition of ReBCO is gradual, an aluminium alloy with low residual resistivity ratio (RRR) can be used as a stabilizer, which brings many advantages, such as a better availability compared to pure aluminium and a mechanically stronger cable.

Published
2024
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17. Annual Report 2022

Author

Aglieri, Gianluca, Aleksa, Martin, Feito, Diego Alvarez, Carballo, Aitor Amatriain, Andorno, Marco, Angeletti, Massimo, Antoszczuk, Pablo, Zarate, Fernando Aretio, Tortajada, I. Asensi, Auffray, Etiennette, Ballabriga, Rafael, Balutto, Mattia, Bandi, Franco, Higueras, Maria Barba, Barney, David, Baron, Sophie, Baszczyk, Mateusz Karol, Bialas, Wojciech, Biereigel, Stefan, Blomer, Jakob, Bordelius, Aleksandar, Borghello, G., Bouvier, Philippe, Boyer, Francois, Braach, Justus, De Souza Mendes, Eduardo Brandao, Brondolin, Erica, Brunbauer, Florian, Buschmann, Eric, Buytaert, Jan, Byczynski, Wiktor, Cala', Roberto, Campbell, Michael, Caratelli, Alessandro, Carnesecchi, Ricardo, Catinaccio, Andrea, Cecconi, Leonardo, Ceresa, Davide, Lemos, Edgar Cid, Coco, Victor, Collins, Paula, Contiero, Luca, Arena, Maria Cristina, Cure, Benoit, Rivera, Esteban Curras, Dachs, Florian, Dall'Omo, Frederik, D'Ambrosio, Carmelo, Dannheim, Dominik, Dao, Valerio, De Melo, Joao, De Oliveira, Rui, Deng, Wenjing, Detraz, Stephane, Dhaliwal, Jashandeep, Di Castro, Mario, Di Mauro, Antonello, Dias, Matheo, Dobrijevic, Dominik, Martin, Ana Dorda, Dorosz, Piotr, Dort, Katharina, Dudarev, Alexey, Dumps, Raphael, Emiliani, Simone, Faccio, Federico, Francois, Brieuc, Bulling, Anthony Frederick, Frei, Christoph, Gabrielli, Andrea, Gargiulo, Corrado, Gessinger-Befurt, Paul, Gkougkousis, Vagelis, Gluchowska, Weronika, Gose, Melwin, Guida, Roberto, Gustavino, Carlo, Haimberger, Jakob, Halvorsen, Marius, Hasenbichler, Jan, Hawkings, Richard, Hong, Geun Hee, Hegner, Benedikt, Hellenschmidt, Desiree, Heribi, Quassim, Hillemans, Hartmut, Himmerlich, Anja, Ijzermans, Pieter, Jaekel, Martin, Jakobsen, Sune, Jama, Kacper, Janot, Patrick, Janssens, Djunes, Floethner, Karl Jonathan, Joram, Christian, Junique, Antoine, Jurco, Robert, Kaplon, Jan, Keizer, Floris, Kiehn, Moritz, Klekotko, Adam, Kloukinas, Kostas, Kluge, Alex, Krammer, Manfred, Kratochwil, Nicolaus, Kremastiotis, Iraklis, Kucharska, Gabriela, Kugathasan, Thanushan, Kühn, Susanne, Kulis, Szymon, La Rosa, Alessandro, Lalovic, Milana, Laudi, Elisa, Le Blanc, M., Ledey, Gael, Miotto, Giovanna Lehmann, Lemoine, Corentin, Linssen, Lucie, Lisowska, Marta, Gomez, Javier Lopez, Mager, Magnus, Malentacca, Lorenzo, Mandelli, Beatrice, Manolescu, Florentian, Martina, Francesco, Martinazzoli, Loris, Martinengo, Paolo, Vila, Pere Mato, Maulerova, Vendula, Mazzei, Francesco, McAlpine, Lee, Mehl, Bertrand, Mentink, Matthias, Michelis, Stephano, Carceller, Juan Miguel, Leitao, Pedro Miguel Vicente, Mlynarikova, Michaela, Moll, Michael, Moneta, Lorenzo, Muller, Hans, Musa, Luciano, Bandi, Franco Nahuel, Nauman, Axel, Nookala, Anvesh, Olantera, Lauri, Oliveri, Eraldo, Orlandini, Giorgio, Pacifico, Nicola, Padulano, Vincenzo, Pandey, Awanish, Pantaleo, Felice, Pape, Sebastian, Pejasinovic, Risto, Pernegger, Heinz, Petagna, Paolo, Piedigrossi, Didier, Diaz, Francisco Piernas, Piller, Markus, Piro, Francesco, Pizzichemi, Marco, Pizzirusso, Olivier, Poblocki, Marcin, Prousalidi, Thenia, Rebane, Karolina, Reichenbach, Leonhard, Reidt, Felix, Rembser, Christoph, Riedler, Petra, Riegler, Werner, Rigoletti, Gianluca, Moreira, Paulo Rodrigues Simoes, Rodrigues, Alexis, Roloff, Philipp, Ropelewski, Leszek, Rovere, Marco, Sailer, André, Salamani, Dalila, Salomoni, Matteo, Salzburger, Andreas, Sanna, Isabella, Sasikumar, Swathi, Sauli, Fabio, Scarcella, Carmelo, Scharenberg, Lucian, Schindler, Heinrich, Schmidt, Burkhard, Schmidt, Janis, Schneider, Thomas, Schopper, Andreas, Secouet, Pascal, Sharma, Abhishek, Sicking, Eva, Sigaud, Christophe, Singh, Shuvay, Sirskaran, Viros, Snoeys, Walter, Solans, Carlos, Gonzalez, Maria Soledad Molina, Soos, Csaba, Stewart, Graeme A., Suljic, Miljenko, Svhira, Peter, Teixeira, Antonio, Teofili, Lorenzo, Termo, Gennaro, Troska, Jan, Utrobicic, Antonija, Van Beelen, Jacob, Van Rijnbach, Milou, Van Stenis, Miranda, Vasey, Francois, Vaskuri, Anna, Nunez, Marcos Vazquez, Veenhof, Rob, Verzeroli, Mattia, Pinto, Mateus Vicente Barreto, Leitao, Pedro Vicente, Volker, Alexander, Volkl, Valentin, Wanotayaroj, Chaowaroj, Weick, Julian, Wiehe, Moritz, Wilkens, Henric, and Zaborowska, Anna

Abstract

This report summarises the activities and main achievements of the CERN strategic R&D programme on technologies for future experiments during the year 2022

Published
2023

18. Extension of the R&D Programme on Technologies for Future Experiments

Author

Joram, Christian, Aglieri, Gianluca, Aleksa, Martin, Feito, Diego Alvarez, Carballo, Aitor Amatriain, Andorno, Marco, Angeletti, Massimo, Antoszczuk, Pablo, Zarate, Fernando Aretio, Tortajada, I. Asensi, Auffray, Etiennette, Ballabriga, Rafael, Balutto, Mattia, Bandi, Franco, Higueras, Maria Barba, Barney, David, Baron, Sophie, Baszczyk, Mateusz Karol, Bialas, Wojciech, Biereigel, Stefan, Blomer, Jakob, Bordelius, Aleksandar, Borghello, G., Bouvier, Philippe, Boyer, Francois, Braach, Justus, De Souza Mendes, Eduardo Brandao, Brondolin, Erica, Brunbauer, Florian, Buschmann, Eric, Buytaert, Jan, Byczynski, Wiktor, Cala', Roberto, Campbell, Michael, Caratelli, Alessandro, Carnesecchi, Ricardo, Catinaccio, Andrea, Cecconi, Leonardo, Ceresa, Davide, Lemos, Edgar Cid, Coco, Victor, Collins, Paula, Contiero, Luca, Arena, Maria Cristina, Cure, Benoit, Rivera, Esteban Curras, Dachs, Florian, Dall'Omo, Frederik, D'Ambrosio, Carmelo, Dannheim, Dominik, Dao, Valerio, De Melo, Joao, De Oliveira, Rui, Deng, Wenjing, Detraz, Stephane, Dhaliwal, Jashandeep, Di Castro, Mario, Di Mauro, Antonello, Dias, Matheo, Dobrijevic, Dominik, Martin, Ana Dorda, Dorosz, Piotr, Dort, Katharina, Dudarev, Alexey, Dumps, Raphael, Emiliani, Simone, Faccio, Federico, Francois, Brieuc, Bulling, Anthony Frederick, Frei, Christoph, Gabrielli, Andrea, Gargiulo, Corrado, Gessinger-Befurt, Paul, Gkougkousis, Vagelis, Gluchowska, Weronika, Gose, Melwin, Guida, Roberto, Gustavino, Carlo, Haimberger, Jakob, Halvorsen, Marius, Hasenbichler, Jan, Hawkings, Richard, Hong, Geun Hee, Hegner, Benedikt, Hellenschmidt, Desiree, Heribi, Quassim, Hillemans, Hartmut, Himmerlich, Anja, Ijzermans, Pieter, Jaekel, Martin, Jakobsen, Sune, Jama, Kacper, Janot, Patrick, Janssens, Djunes, Floethner, Karl Jonathan, Junique, Antoine, Jurco, Robert, Kaplon, Jan, Keizer, Floris, Kiehn, Moritz, Klekotko, Adam, Kloukinas, Kostas, Kluge, Alex, Krammer, Manfred, Kratochwil, Nicolaus, Kremastiotis, Iraklis, Kucharska, Gabriela, Kugathasan, Thanushan, Kühn, Susanne, Kulis, Szymon, La Rosa, Alessandro, Lalovic, Milana, Laudi, Elisa, Le Blanc, M., Ledey, Gael, Miotto, Giovanna Lehmann, Lemoine, Corentin, Linssen, Lucie, Lisowska, Marta, Gomez, Javier Lopez, Mager, Magnus, Malentacca, Lorenzo, Mandelli, Beatrice, Manolescu, Florentian, Martina, Francesco, Martinazzoli, Loris, Martinengo, Paolo, Vila, Pere Mato, Maulerova, Vendula, Mazzei, Francesco, McAlpine, Lee, Mehl, Bertrand, Mentink, Matthias, Michelis, Stephano, Carceller, Juan Miguel, Leitao, Pedro Miguel Vicente, Mlynarikova, Michaela, Moll, Michael, Moneta, Lorenzo, Muller, Hans, Musa, Luciano, Bandi, Franco Nahuel, Nauman, Axel, Nookala, Anvesh, Olantera, Lauri, Oliveri, Eraldo, Orlandini, Giorgio, Pacifico, Nicola, Padulano, Vincenzo, Pandey, Awanish, Pantaleo, Felice, Pape, Sebastian, Pejasinovic, Risto, Pernegger, Heinz, Petagna, Paolo, Piedigrossi, Didier, Diaz, Francisco Piernas, Piller, Markus, Piro, Francesco, Pizzichemi, Marco, Pizzirusso, Olivier, Poblocki, Marcin, Prousalidi, Thenia, Rebane, Karolina, Reichenbach, Leonhard, Reidt, Felix, Rembser, Christoph, Riedler, Petra, Riegler, Werner, Rigoletti, Gianluca, Moreira, Paulo Rodrigues Simoes, Rodrigues, Alexis, Roloff, Philipp, Ropelewski, Leszek, Rovere, Marco, Sailer, André, Salamani, Dalila, Salomoni, Matteo, Salzburger, Andreas, Sanna, Isabella, Sasikumar, Swathi, Sauli, Fabio, Scarcella, Carmelo, Scharenberg, Lucian, Schindler, Heinrich, Schmidt, Burkhard, Schmidt, Janis, Schneider, Thomas, Schopper, Andreas, Secouet, Pascal, Sharma, Abhishek, Sicking, Eva, Sigaud, Christophe, Singh, Shuvay, Sirskaran, Viros, Snoeys, Walter, Solans, Carlos, Gonzalez, Maria Soledad Molina, Soos, Csaba, Stewart, Graeme A., Suljic, Miljenko, Svhira, Peter, Teixeira, Antonio, Teofili, Lorenzo, Termo, Gennaro, Troska, Jan, Utrobicic, Antonija, Van Beelen, Jacob, Van Rijnbach, Milou, Van Stenis, Miranda, Vasey, Francois, Vaskuri, Anna, Nunez, Marcos Vazquez, Veenhof, Rob, Verzeroli, Mattia, Pinto, Mateus Vicente Barreto, Leitao, Pedro Vicente, Volker, Alexander, Volkl, Valentin, Wanotayaroj, Chaowaroj, Weick, Julian, Wiehe, Moritz, Wilkens, Henric, and Zaborowska, Anna

Abstract

we have conceived an extension of the R&D programme covering the period 2024 to 2028, i.e. again a 5-year period, however with 2024 as overlap year. This step was encouraged by the success of the current programme but also by the Europe-wide efforts to launch new Detector R&D collaborations in the framework of the ECFA Detector R&D Roadmap. We propose to continue our R&D programme with the main activities in essentially the same areas. All activities are fully aligned with the ECFA Roadmap and in most cases will be carried out under the umbrella of one of the new DRD collaborations. The program is a mix of natural continuations of the current activities and a couple of very innovative new developments, such as a radiation hard embedded FPGA implemented in an ASIC based on System-on-Chip technology. A special and urgent topic is the fabrication of Al-reinforced super-conducting cables. Such cables are a core ingredient of any new superconducting magnet such as BabyIAXO, PANDA, EIC, ALICE-3 etc. Production volumes are small and demands come in irregular intervals. Industry (world-wide) is no longer able and willing to fabricate such cables. The most effective approach (technically and financially) may be to re-invent the process at CERN, together with interested partners, and offer this service to the community.

Published
2023

20. Strategic R&D Programme on Technologies for Future Experiments - Annual Report 2021

Author

Aglieri Rinella, Gianluca, Aleksa,Martin, Alvarez Feito,Diego, Andorno,Marco, Angeletti,Massimo, Antoszczuk,Pablo, Asensi Tortajada,I., Auffray Hillemanns, Etiennette, Ballabriga,Raphael, Balutto,Mattia, Bandi,Franco, Barba Higueras,Maria, Barney,David, Baron,Sophie, Barreto Pinto,Mateus, Bastian Van Beelen,Jacob, Baszczyk,Mateusz Karol, Beguin,Marina, Bialas,W., Biereigel,Stefan, Blomer,Jakob, Borghello,G., Braach,Justus, Brandao De Souza Mendes,Eduardo, Brondolin,Erica, Brunbauer,Florian, Buschmann,Eric, Buytaert,Jan, Byczynski,Wiktor, Cala',Roberto, Cambie,Federico, Campbell,Michael, Caratelli,Alessandro, Carnesecchi,F., Catinaccio,Andrea, Cecconi,Leonardo, Ceresa,Davide, Cid Lemos,Edgar, Coco,Victor, Collins,Paula, Contiero,Luca, Corbetta,Mara, Cure,Benoit, Curras Rivera,Esteban, Dachs,Florian, Dall'Omo,Frederik, D'Ambrosio,Carmelo, Dannheim,Dominik, Dao,V., De Melo,Joao, De Oliveira,Rui, Deng,W., Deng,Wenjing, Detraz,Stephane, Di Mauro,Antonello, Dias,Matheo, Dobrijevic,D., Dobrijevic,Dominik, Dorda Martin,A., Dorda Martin,Ana, Dorosz,P., Dort,Katharina, Dudarev,Alexey, Dumps,Raphael, Faccio,Federico, Fernandez Declara,Placido, Fiorenza,Gabriele, Francois,Brieuc, Frederick Bulling ,Anthony, Frei,Christoph, Gabrielli,A., Gargiulo,Corrado, Gessinger-Befurt,Paul, Gkougkousis,Vagelis, Gluchowska,Weronika, Gose,Melwin, Guida,Roberto, Gustavino,C., Haimberger,Jakob, Halvorsen,Marius, Hasenbichler,J., Hawkings,Richard, Hee Hong,Geun, Hellenschmidt,Desiree, Heribi,Quassim, Hillemans,H., Himmerlich,Anja, Ijzermans,Pieter, Janot,Patrick, Janssens,Djunes, Jonathan Floethner ,Karl, Joram,Christian, Kaplon,Jan, Keizer,Floris, Kiehn,Moritz, Klekotko,Adam, Kloukinas,Kostas, Kluge,Alex, Krammer,Manfred, Kratochwil,Nicolaus, Kremastiotis, Iraklis, Kroeger,Jens, Kugathasan,T., La Rosa,Alessandro, Lafuente,Antonio, Lalovic,Milana, Laudi,Elisa, Le Blanc,M., Ledey,Gael, Leitao,M., Linssen,Lucie, Lisowska,Marta, Lopez Gomez,Javier, Maciej Malinowski,Filip, Magatti,Demetrio, Mager,Magnus, Mandelli,Beatrice, Martinazzoli,Loris, Martinengo,Paolo, Mato Vila,Pere, Maulerova,Vendula, Mehl,Bertrand, Mentink,Matthias, Moll,Michael, Muller,Hans, Musa,Luciano, Neroni,Michela, Olantera ,Lauri, Oliveri,Eraldo, Orlandini,Giorgio, Padulano,Vincenzo, Pantaleo,Felice, Pape,Sebastian, Pejasinovic,Risto, Pernegger,Heinz, Petagna,Paolo, Piedigrossi,Didier, Piernas Diaz,Francisco, Piller,Markus, Piro,Francesco, Pizzichemi, Marco, Pizzirusso,Olivier, Prousalidi ,Thenia, Rebane,K., Reidt,F., Rembser,Christoph, Riedler,Petra, Riegler,Werner, Rigoletti,Gianluca, Rodrigues Simoes Moreira,Paulo, Roloff, Philipp Gerhard, Ropelewski,Leszek, Rovere,Marco, Sailer,André, Salamani,Dalila, Salomoni,Matteo, Salzburger,Andreas, Sanna,I., Scarcella ,Carmelo, Scharenberg,Lucian, Schindler,Heinrich, Schmidt,Burkhard, Schmidt,Janis, Schneider,Thomas, Schopper,Andreas, Secouet,Pascal, Sharma,A., Singh,Shuvay, Sirskaran,Viros, Snoeys,Walter, Solans,Carlos, Soledad Molina Gonzalez,Maria, Soos,Csaba, Stewart,Graeme A, Suljic,M., Svhira,Peter, Teixeira,Antonio, Teofili,Lorenzo, Termo,Gennaro, Troska,Jan, Utrobicic,Antonija, Van Rijnbach,Milou, Van Stenis,Miranda, Vasey,Francois, Vaskuri,Anna, Veenhof,Rob, Verzeroli,Mattia, Vicente Leitao,Pedro, Vicente,M., Volkl,Valentin, Wanotayaroj,Chaowaroj, Weick,Julian, Wiehe,Moritz, and Zaborowska,Anna

Abstract

This report summarises the activities and main achievements of the CERN strategic R&D programme on technologies for future experiments during the year 2021.

Published
2022

21. Towards Ultra-Thin Detector Magnet Designs by Insulating Coil Windings With V<inline-formula><tex-math notation="LaTeX">$_{2}$</tex-math></inline-formula>O<inline-formula><tex-math notation="LaTeX">$_{3}$</tex-math></inline-formula>-Epoxy Composite

Author

Vaskuri, Anna, Cure, Benoit, Dudarev, Alexey, Mentink, Matthias, Pfeiffer, Stephan, and Teissandier, Benoit

Abstract

We have measured temperature dependent resistivity of two types of vanadium oxide (V$_{2}$O$_{3}$) epoxy composites from 77 K to room temperature. Such a composite could be used as an insulating layer between the windings of a superconducting magnet. During a magnet quench, the composite is expected to change from insulating to metallic at approximately 150 K, re-distributing the current through the heated windings. Our measurement results show significantly different phase transition characteristics of the samples. A sample mixed using 99.7% pure V$_{2}$O$_{3}$ powder with sharp edges in particles and an average equivalent circle diameter (ECD) of 4.5 $\mu$m has a factor of 23 resistivity change and a sample mixed using 95% pure V$_{2}$O$_{3}$ powder with round edges in particles and an average ECD of 70 $\mu$m has a change of three orders of magnitude, respectively. Using V$_{2}$O$_{3}$-epoxy composite as an insulating layer between the coil windings might allow thinner detector magnet designs since the current and heat would spread more uniformly across the magnet during a quench.

Published
2023
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25. Development of 300 mW Background-Compensated Planar Absolute Radiometer Operating at Room Temperature

Author

Vaskuri, Anna, Stephens, M S., Tomlin, N. A., Yung, C. S., Walowitz, A. J., Straatsma, C., Harber, D., and Lehman, J.

Abstract

NIST’s C-series isoperibol calorimeters [1] operating at room temperature have been used as reference instruments in the laser power calibrations at NIST for over 50 years. These calorimeters operate from 100 μW to 300 mW with an expanded uncertainty of 0.86% (k = 2). Recently developed vertically aligned carbon-nanotube (VACNT) absorbers, with spectrally flat and hemispherical absorptance better than 99.95%, have enabled development of planar absolute bolometers with smaller size and significantly faster measurements compared to traditional laser calorimeters. In this work, we present the latest progress of the Planar Absolute Radiometer for Room Temperature (PARRoT) [2] currently under construction that will replace the old reference C-series calorimeters. PARRoT is based on the electrical power substitution method and it can measure laser powers up to 300 mW with a predicted expanded uncertainty better than 0.1% (k = 2). The radiometer is operated at room temperature and placed in a 15 cm cube vacuum chamber to minimize convection while still providing a compact and sturdy standard. The laser beam is transmitted to the absorber by an uncoated fused silica window with a 0.5° wedge assuring polarization independent laser power detection. PARRoT is background compensated by differential operation where the reference detector chip is driven by a constant DC power and the measuring detector chip is feedback controlled to follow the temperature of the reference detector chip. The closed loop operation makes the radiometer’s response linear across the operational power range. We have optimized the detector chip design by thermal modeling [2]. The modeled electro-optical inequivalence for a centered laser beam is 0.007% and the spatial non-uniformity is ±0.02% within 4 mm radius from the absorber’s center, meaning that PARRoT is not sensitive to small alignment offsets. PARRoT’s differential background compensation makes it insensitive to variations in background radiation. That combined with a compact design would allow it to be used as a radiance detector standard for field calibrations and atmospheric measurements outdoors or as a transfer standard between laboratories. Similar bolometers will be launched in a CubeSat satellite next year to measure total solar irradiance [3]. By changing a few resistance values in the electronics, by changing the detector chip’s heater resistance, and modifying the thermal conductance of the heat link design, the power range of PARRoT can be modified for different applications without compromising the accuracy. For example, reducing the heater resistance and increasing the heat link’s thermal conductance can extend the power range to 2 W. This enables, for instance, direct calibration of the 1 W laser beam power in LIGO (Laser Interferometer Gravitational-wave Observatory) with an expanded uncertainty of 0.1% (k = 2) which would be an order of magnitude improvement to its current calibration against NIST’s reference calorimeter via an integrating sphere transfer standard. Acknowledgements: Jenny and Antti Wihuri Foundation, Finland is acknowledged for the financial support of this research. 1. E. D. West et al., “A Reference Calorimeter for Laser Energy Measurements,” J. Res. Natl. Bur. Stand. (U. S.) 76A, 13–26 (1972). 2. A. Vaskuri et al., “Microfabricated bolometer based on a vertically aligned carbon nanotube absorber,” Proc. SPIE 11269, 1–12, Synthesis and Photonics of Nanoscale Materials XVII, 112690L (March 2020). 3. D. Harber et al., “Compact total irradiance monitor flight demonstration,” Proc. SPIE 11131, 1–8, CubeSats and SmallSats for Remote Sensing III, 111310D (August 2019).

Published
2020

26. Cryostat setup for measuring spectral and electrical properties of light-emitting diodes at junction temperatures from 81 K to 297 K

Author

Martikainen, Elvira, Vaskuri, Anna, Dönsberg, Timo, Ikonen, Erkki, Metrology Research Institute, Dept Signal Process and Acoust, Aalto-yliopisto, and Aalto University

Abstract

We introduce a cryostat setup for measuring fundamental optical and electrical properties of light-emitting diodes (LEDs). With the setup, the cryostat pressure and the LED properties of the forward voltage, junction temperature, and electroluminescence spectrum are monitored with temperature steps less than 1.5 K, over the junction temperature range of 81-297 K. We applied the setup to commercial yellow AlGaInP and blue InGaN LEDs. At cryogenic temperatures, the fine structure of the electroluminescence spectra became resolved. For the yellow LED, we observed the phonon replica at 2.094 eV that was located 87 meV below the peak energy at the junction temperature of 81 K. For the blue LED, we observed the cascade phonon replicas at 2.599 eV, 2.510 eV, and 2.422 eV with the energy interval of 89 meV. For both LED types, the forward voltage increased sharply toward the lower temperatures due to the increased resistivity of materials in the LED components. We found significant differences between the temperaturedependent behaviors of the forward voltages, spectral peak energies, and bandgap energies of LEDs obtained from the Varshni formula. We also noted a sharp pressure peak at 180-185 K arising from the solid-vapor phase transition of water when the base level of the cryostat pressure was approximately 0.4 mPa.

Published
2020
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32. Modeling the spectral shape of InGaAlP-based red light-emitting diodes.

Author

Vaskuri, Anna, Baumgartner, Hans, Kärhä, Petri, Andor, György, and Ikonen, Erkki

Subjects
*LIGHT emitting diodes, *LIGHT sources, *QUANTUM wells spectra, *ELECTRONIC spectra, *ELECTRIC properties of semiconductors
Abstract

We have developed a spectral model for describing the shape of the emission spectrum of InGaAlP-based red light-emitting diodes (LEDs) with quantum-well structure. The model is based on Maxwell-Boltzmann distribution with junction temperature Tj and an experimental twodimensional joint density of states (DOS). We model the DOS with a sum of two exponentially broadened step functions describing the two lowest sub-bands in semiconductor quantum well. The relative locations ΔE1 =0meV and βE2 =112.7 meV above the band gap energy Eg=1.983 eV and the ratio 2.13 of the step heights were fixed using an experimental DOS extracted from a LED spectrum measured at known Tj and driving current I. The model can then be fitted to other spectra of other LED samples at varied Tj and I by varying the fitting parameters Eg; Tj, and the broadening of the sub-band edges. The model was tested for three LED samples over I=200-370mA and Tj=303-398 K. Junction temperatures obtained by modeling were compared with calibrated Tj obtained by the forward voltage method. The mean absolute difference was about 2.9K (0.8%) over the whole region studied and the maximum difference was 8.5 K. The thermal coefficient measured for Eg was -0.509 meVK-1. For the first and second sub-band edges, the thermal broadening coefficients were 18 leVK-1 and 37 leVK-1, respectively. [ABSTRACT FROM AUTHOR]

Published
2015
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34. Portable Monochromatic Infrared Light Source Based on a Supercontinuum Laser

Author

Vaskuri, Anna, Manoocheri, Farshid, Sähkötekniikan korkeakoulu, Ikonen, Erkki, Maham, Kinza, Vaskuri, Anna, Manoocheri, Farshid, Sähkötekniikan korkeakoulu, Ikonen, Erkki, and Maham, Kinza

Abstract

A portable wavelength tunable light source to calibrate the spectral responsivities of detectors in the infrared region was developed and characterized. It comprises of a supercontinuum laser, laser line tunable filter (LLTF), and output coupling optics, such as a focusing lens and a cut-on filter. This light source improves spectral responsivity calibrations of the detectors as the developed setup is automated. To automate this setup a motorized XY translation stage and a filter wheel was used. In order to characterize the monochromatic light source and its coupling optics, a spectroradiometer was used. The wavelength scale of this spectroradiometer was calibrated using HgAr pen lamps and KrAr+ laser lines to ensure the spectral peaks of LLTF are measured correctly. Three photovoltaic detectors, of which two were based on indium gallium arsenide and one based on germanium, were calibrated using the automated wavelength tunable light source setup against a pyroelectric radiometer. The pyroelectric radiometer was used as a reference detector due to its spectrally flat responsivity. The aperture diameters of indium gallium arsenide and germanium detectors are 5 mm and 10 mm, respectively. Due to the small active areas of the detectors, the collimated laser beam output from the multimode fiber was focused on the detector plane. The spectral responsivity calibrations were performed over the spectral range from 800 nm to 2000 nm. As the optimal working spectral range of LLTF is 1000 nm - 2000 nm and depending on the band gap edge of the photovoltaic detectors, the standard deviations of the readings measured at wavelengths below 820 nm and above 1600 nm are slightly higher. The spectral responsivities of the photovoltaic detectors studied were compared to the older calibrations performed using a reference spectroradiometer at the Metrology Research Institute. Through careful analysis of the experiments and comparisons, it is found that this setup decreases the expanded u

Published
2018

44. The BLAST Observatory: A Sensitivity Study for Far-IR Balloon-borne Polarimeters

Author

Coppi, Gabriele, Dicker, Simon, Aguirre, James E., Austermann, Jason E., Beall, James A., Clark, Susan E., Cox, Erin G., Devlin, Mark J., Fissel, Laura M., Galitzki, Nicholas, Hensley, Brandon S., Hubmayr, Johannes, Molinari, Sergio, Nati, Federico, Novak, Giles, Schisano, Eugenio, Soler, Juan D., Tucker, Carole E., Ullom, Joel N., Vaskuri, Anna, Vissers, Michael R., Wheeler, Jordan D., and Zannoni, Mario

Abstract

Sensitive wide-field observations of polarized thermal emission from interstellar dust grains will allow astronomers to address key outstanding questions about the life cycle of matter and energy driving the formation of stars and the evolution of galaxies. Stratospheric balloon-borne telescopes can map this polarized emission at far-infrared wavelengths near the peak of the dust thermal spectrum—wavelengths that are inaccessible from the ground. In this paper we address the sensitivity achievable by a Super Pressure Balloon polarimetry mission, using as an example the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) Observatory. By launching from Wanaka, New Zealand, the BLAST Observatory can obtain a 30 days flight with excellent sky coverage—overcoming limitations of past experiments that suffered from short flight duration and/or launch sites with poor coverage of nearby star-forming regions. This proposed polarimetry mission will map large regions of the sky at sub-arcminute resolution, with simultaneous observations at 175, 250, and 350 μm, using a total of 8274 microwave kinetic inductance detectors. Here, we describe the scientific motivation for the BLAST Observatory, the proposed implementation, and the forecasting methods used to predict its sensitivity. We also compare our forecasted experiment sensitivity with other facilities.

Published
2024
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46. Monte Carlo method for determining uncertainty of total ozone derived from direct solar irradiance spectra: Application to Izaña results.

Author

Vaskuri, Anna, Kärhä, Petri, Egli, Luca, Gröbner, Julian, and Ikonen, Erkki

Subjects
*MONTE Carlo method, *SPECTRAL irradiance
Abstract

We demonstrate a Monte Carlo model to calculate the uncertainties of total ozone column, TOC, derived from ground-based directional solar spectral irradiance measurements. The model takes into account effects that correlations in the spectral irradiance data may have on the results. The model is tested with spectral data measured with three different spectroradiometers at an intercomparison campaign of the research project Traceability for atmospheric total column ozone at Izaña, Tenerife on 17 September 2016. The TOC values derived at noon have expanded uncertainties of 1.3% for a high-end scanning spectroradiometer, 1.3% for a high-end array spectroradiometer, and 3.3% for a roughly adopted instrument based on commercially available components and an array spectroradiometer. The level of TOC measured with reference Brewer spectrophotometer #183 is of the order of 282 DU during the analysed day and in agreement with the results of the two former instruments. [ABSTRACT FROM AUTHOR]

Published
2018
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48. Lasereihin perustuva laitteisto optisten ilmaisimien ja materiaalien karakterisointiin

Author

Kärhä, Petri, Dönsberg, Timo, Sähkötekniikan korkeakoulu, Ikonen, Erkki, Vaskuri, Anna, Kärhä, Petri, Dönsberg, Timo, Sähkötekniikan korkeakoulu, Ikonen, Erkki, and Vaskuri, Anna

Abstract

Optisia ilmaisimia käytetään monissa sovelluksissa kuvantamislaitteista, turvajärjestelmistä sekä konenäkösovelluksista merkinanto- ja tiedonsiirtojärjestelmiin. Spektrinen tehoherkkyys ja spatiaalivaste ovat ratkaisevan tärkeitä parametreja optisten ilmaisimien karakterisoinnissa. Tässä työssä on suunniteltu ja toteutettu lasereihin perustuva laitteisto kyseisiä mittauksia varten. Mittauslaitteisto ohjaa stabiilin, kollimoidun ja halkaisijaltaan kapean lasersäteen näytepidikkeelle, joka on asennettu korkearesoluutioiselle XY-siirtimelle. Ilmaisimia voidaan vaihtaa keskenään absoluuttisen tehoherkkyyden kalibroimiseksi, tai niiden spatiaalivasteet voidaan skannata. Mittauslaitteistolla voidaan myös karakterisoida materiaalien optisia ominaisuuksia, kuten kellastumista, mittaamalla niiden transmittanssit. Laitteiston suorituskyky karakterisoitiin mittaamalla lasersäteen laatua. Mittausten perusteella laitteiston lasersäteen 8 h stabiilisuuden suhteellinen keskihajonta oli 0.01 % käytettäessä tehosäädintä. Stabiloidun lasersäteen tarkkailu erillisellä ilmaisimella laski suhteellisen keskihajonnan alle 0.007 %:iin. Lisäksi laitteistossa käytetyn spatiaalisuodattimen todettiin tasoittavan lasersäteen profiilia, etenkin diodilaseria käytettäessä. Kehitetty laitteisto parantaa MIKES-Aalto Mittaustekniikassa suoritettavien peräkkäisten vuotuisten ilmaisinkalibrointien tarkkuutta ja toistettavuutta. Laitteisto mahdollistaa spatiaalivasteen rutiiniskannauksen kalibroinnin yhteydessä; sillä voidaan tarkistaa esimerkiksi ilmaisimen kunto. Materiaalitieteen alalla ultravioletti (UV) spektrografin ja kehitetyn mittauslaitteiston yhdistelmä mahdollistaa uuden menetelmän tutkia UV-säteilyn aiheuttamaa materiaalien hajoamista alle 2 nm resoluutiolla, mikä on merkittävä parannus aiempiin menetelmiin verrattuna., Optical detectors are used in various applications ranging from imaging devices, security systems, and robotic vision, to signaling and transmission systems. Spectral power responsivity and spatial uniformity are crucial parameters for characterizing detectors. In this thesis, a multi-wavelength setup based on lasers has been designed and constructed for these measurements. The setup directs a stable, collimated laser beam with a narrow beam diameter to a sample holder unit mounted on a high-resolution XY translation stage. Detectors can be interchanged to calibrate absolute power responsivities, or they can be scanned to obtain spatial uniformities. The measurement setup can also be used to characterize optical properties of materials, such as photoyellowing, by measuring their transmittances. The performance of the setup was characterized by measuring the quality of the laser beam. Based on the measurements, the 8 h stability of the laser when using the laser power controller had a relative standard deviation of 0.01 %. By monitoring the stabilized beam with a monitor detector, the relative standard deviation decreased below 0.007 %. The spatial filter used in the setup was verified to smooth the beam profile, especially with diode lasers. The setup developed improves the accuracy and repeatability of consecutive annual detector calibrations in the Metrology Research Institute. The setup enables routine scanning of the spatial uniformity in pursuance of the calibration; it can be used, e.g., to check the condition of the detector. In the material science, a combination of the ultraviolet (UV) spectrograph and the measurement setup developed enables a novel method for studying the UV radiation-induced degradation of materials with a resolution smaller than 2 nm, which is a significant improvement for earlier methods.

Published
2014

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