Aaron Chou, Kent Irwin, Reina H. Maruyama, Oliver K. Baker, Chelsea Bartram, Karl K. Berggren, Gustavo Cancelo, Daniel Carney, Clarence L. Chang, Hsiao-Mei Cho, Maurice Garcia-Sciveres, Peter W. Graham, Salman Habib, Roni Harnik, J. G. E. Harris, Scott A. Hertel, David B. Hume, Rakshya Khatiwada, Timothy L. Kovachy, Noah Kurinsky, Steve K. Lamoreaux, Konrad W. Lehnert, David R. Leibrandt, Dale Li, Ben Loer, Julián Martínez-Rincón, Lee McCuller, David C. Moore, Holger Mueller, Cristian Pena, Raphael C. Pooser, Matt Pyle, Surjeet Rajendran, Marianna S. Safronova, David I. Schuster, Matthew D. Shaw, Maria Spiropulu, Paul Stankus, Alexander O. Sushkov, Lindley Winslow, Si Xie, Kathryn M. Zurek
Strong motivation for investing in quantum sensing arises from the need to investigate phenomena that are very weakly coupled to the matter and fields well described by the Standard Model. These can be related to the problems of dark matter, dark sectors not necessarily related to dark matter (for example sterile neutrinos), dark energy and gravity, fundamental constants, and problems with the Standard Model itself including the Strong CP problem in QCD. Resulting experimental needs typically involve the measurement of very low energy impulses or low power periodic signals that are normally buried under large backgrounds. This report documents the findings of the 2023 Quantum Sensors for High Energy Physics workshop which identified enabling quantum information science technologies that could be utilized in future particle physics experiments, targeting high energy physics science goals.
Aaron S. Chou
Experimental searches for axions or axion-like particles rely on semiclassical phenomena resulting from the postulated coupling of the axion to two photons. Sensitive probes of the extremely small coupling constant can be made by exploiting familiar, coherent electromagnetic laboratory techniques, including resonant enhancement of transitions using microwave and optical cavities, Bragg scattering, and coherent photon-axion oscillations. The axion beam may either be astrophysical in origin as in the case of dark matter axion searches and solar axion searches, or created in the laboratory from laser interactions with magnetic fields. This note is meant to be a sampling of recent experimental results.
Aaron S. Chou, Richard Gustafson, Craig Hogan, Brittany Kamai, Ohkyung Kwon, Robert Lanza, Lee McCuller, Stephan S. Meyer, Jonathan Richardson, Chris Stoughton, Raymond Tomlin, Samuel Waldman, Rainer Weiss
Measurements are reported of the cross-correlation of spectra of differential position signals from the Fermilab Holometer, a pair of co-located 39 m long, high power Michelson interferometers with flat, broadband frequency response in the MHz range. The instrument obtains sensitivity to high frequency correlated signals far exceeding any previous measurement in a broad frequency band extending beyond the 3.8 MHz inverse light crossing time of the apparatus. The dominant but uncorrelated shot noise is averaged down over $2\times 10^8$ independent spectral measurements with 381 Hz frequency resolution to obtain $2.1\times 10^{-20} \ \mathrm{m}/\sqrt{\mathrm{Hz}}$ sensitivity to stationary signals. For signal bandwidths $Δf > 11$ kHz, the sensitivity to strain $h$ or shear power spectral density of classical or exotic origin surpasses a milestone $PSD_{δh} < t_p$ where $t_p= 5.39\times 10^{-44}/\mathrm{Hz}$ is the Planck time.
Aaron S. Chou
Jun 30, 2006·astro-ph·PDF We consider the possibility that the ultra-high-energy cosmic ray flux has a small component of exotic particles which create showers much deeper in the atmosphere than ordinary hadronic primaries. It is shown that applying the conventional AGASA/HiRes/Auger data analysis procedures to such exotic events results in large systematic biases in the energy spectrum measurement. SubGZK exotic showers may be mis-reconstructed with much higher energies and mimick superGZK events. Alternatively, superGZK exotic showers may elude detection by conventional fluorescence analysis techniques.
Aaron S. Chou
We present recent measurements by SLD of the branching fractions of B hadrons to states with 0 and 2 open charm hadrons, BR_{0D} and BR_{2D}, from which both the average charm yield per B decay, N_c and the inclusive branching ratio into rare modes not containing any charmed hadrons, BR_{rare} can be derived. We also present a new measurement of the B_d mixing frequency Delta m_d and limits on the B_s mixing frequency Delta m_s. These analyses take advantage of the excellent vertexing resolution of the VXD3, a pixel-based CCD vertex detector, which enables the topological separation of the B and cascade D decay vertices.
Toshinori Abe, Aaron S. Chou
Several different vertex detector designs for the Linear Collider Detector(LCD) are evaluated in the context of measurements of the branching ratio of the standard model Higgs particle decaying into charm/anti-charm final states. Fast Monte Carlo simulations are used to model the detector and neural network-optimized flavor tagging is used to perform the measurements. These tools are used to study the effects of pixel resolution, material thickness, and inner layer radius on the flavor tagging efficiency-purity curve and ultimately on the branching ratio measurement error.
Stefan Knirck, Gabe Hoshino, Mohamed H. Awida, Gustavo I. Cancelo, Martin Di Federico, Benjamin Knepper, Alex Lapuente, Mira Littmann, David W. Miller, Donald V. Mitchell, Derrick Rodriguez, Mark K. Ruschman, Matthew A. Sawtell, Leandro Stefanazzi, Andrew Sonnenschein, Gary W. Teafoe, Daniel Bowring, G. Carosi, Aaron Chou, Clarence L. Chang, Kristin Dona, Rakshya Khatiwada, Noah A. Kurinsky, Jesse Liu, Cristián Pena, Chiara P. Salemi, Christina W. Wang, Jialin Yu
We present first results from a dark photon dark matter search in the mass range from 44 to 52 $μ{\rm eV}$ ($10.7 - 12.5\,{\rm GHz}$) using a room-temperature dish antenna setup called GigaBREAD. Dark photon dark matter converts to ordinary photons on a cylindrical metallic emission surface with area $0.5\,{\rm m}^2$ and is focused by a novel parabolic reflector onto a horn antenna. Signals are read out with a low-noise receiver system. A first data taking run with 24 days of data does not show evidence for dark photon dark matter in this mass range, excluding dark photon - photon mixing parameters $χ\gtrsim 10^{-12}$ in this range at 90% confidence level. This surpasses existing constraints by about two orders of magnitude and is the most stringent bound on dark photons in this range below 49 $μ$eV.
Marco Battaglieri, Alberto Belloni, Aaron Chou, Priscilla Cushman, Bertrand Echenard, Rouven Essig, Juan Estrada, Jonathan L. Feng, Brenna Flaugher, Patrick J. Fox, Peter Graham, Carter Hall, Roni Harnik, JoAnne Hewett, Joseph Incandela, Eder Izaguirre, Daniel McKinsey, Matthew Pyle, Natalie Roe, Gray Rybka, Pierre Sikivie, Tim M. P. Tait, Natalia Toro, Richard Van De Water, Neal Weiner, Kathryn Zurek, Eric Adelberger, Andrei Afanasev, Derbin Alexander, James Alexander, Vasile Cristian Antochi, David Mark Asner, Howard Baer, Dipanwita Banerjee, Elisabetta Baracchini, Phillip Barbeau, Joshua Barrow, Noemie Bastidon, James Battat, Stephen Benson, Asher Berlin, Mark Bird, Nikita Blinov, Kimberly K. Boddy, Mariangela Bondi, Walter M. Bonivento, Mark Boulay, James Boyce, Maxime Brodeur, Leah Broussard, Ranny Budnik, Philip Bunting, Marc Caffee, Sabato Stefano Caiazza, Sheldon Campbell, Tongtong Cao, Gianpaolo Carosi, Massimo Carpinelli, Gianluca Cavoto, Andrea Celentano, Jae Hyeok Chang, Swapan Chattopadhyay, Alvaro Chavarria, Chien-Yi Chen, Kenneth Clark, John Clarke, Owen Colegrove, Jonathon Coleman, David Cooke, Robert Cooper, Michael Crisler, Paolo Crivelli, Francesco D'Eramo, Domenico D'Urso, Eric Dahl, William Dawson, Marzio De Napoli, Raffaella De Vita, Patrick DeNiverville, Stephen Derenzo, Antonia Di Crescenzo, Emanuele Di Marco, Keith R. Dienes, Milind Diwan, Dongwi Handiipondola Dongwi, Alex Drlica-Wagner, Sebastian Ellis, Anthony Chigbo Ezeribe, Glennys Farrar, Francesc Ferrer, Enectali Figueroa-Feliciano, Alessandra Filippi, Giuliana Fiorillo, Bartosz Fornal, Arne Freyberger, Claudia Frugiuele, Cristian Galbiati, Iftah Galon, Susan Gardner, Andrew Geraci, Gilles Gerbier, Mathew Graham, Edda Gschwendtner, Christopher Hearty, Jaret Heise, Reyco Henning, Richard J. Hill, David Hitlin, Yonit Hochberg, Jason Hogan, Maurik Holtrop, Ziqing Hong, Todd Hossbach, T. B. Humensky, Philip Ilten, Kent Irwin, John Jaros, Robert Johnson, Matthew Jones, Yonatan Kahn, Narbe Kalantarians, Manoj Kaplinghat, Rakshya Khatiwada, Simon Knapen, Michael Kohl, Chris Kouvaris, Jonathan Kozaczuk, Gordan Krnjaic, Valery Kubarovsky, Eric Kuflik, Alexander Kusenko, Rafael Lang, Kyle Leach, Tongyan Lin, Mariangela Lisanti, Jing Liu, Kun Liu, Ming Liu, Dinesh Loomba, Joseph Lykken, Katherine Mack, Jeremiah Mans, Humphrey Maris, Thomas Markiewicz, Luca Marsicano, C. J. Martoff, Giovanni Mazzitelli, Christopher McCabe, Samuel D. McDermott, Art McDonald, Bryan McKinnon, Dongming Mei, Tom Melia, Gerald A. Miller, Kentaro Miuchi, Sahara Mohammed Prem Nazeer, Omar Moreno, Vasiliy Morozov, Frederic Mouton, Holger Mueller, Alexander Murphy, Russell Neilson, Tim Nelson, Christopher Neu, Yuri Nosochkov, Ciaran O'Hare, Noah Oblath, John Orrell, Jonathan Ouellet, Saori Pastore, Sebouh Paul, Maxim Perelstein, Annika Peter, Nguyen Phan, Nan Phinney, Michael Pivovaroff, Andrea Pocar, Maxim Pospelov, Josef Pradler, Paolo Privitera, Stefano Profumo, Mauro Raggi, Surjeet Rajendran, Nunzio Randazzo, Tor Raubenheimer, Christian Regenfus, Andrew Renshaw, Adam Ritz, Thomas Rizzo, Leslie Rosenberg, Andre Rubbia, Ben Rybolt, Tarek Saab, Benjamin R. Safdi, Elena Santopinto, Andrew Scarff, Michael Schneider, Philip Schuster, George Seidel, Hiroyuki Sekiya, Ilsoo Seong, Gabriele Simi, Valeria Sipala, Tracy Slatyer, Oren Slone, Peter F Smith, Jordan Smolinsky, Daniel Snowden-Ifft, Matthew Solt, Andrew Sonnenschein, Peter Sorensen, Neil Spooner, Brijesh Srivastava, Ion Stancu, Louis Strigari, Jan Strube, Alexander O. Sushkov, Matthew Szydagis, Philip Tanedo, David Tanner, Rex Tayloe, William Terrano, Jesse Thaler, Brooks Thomas, Brianna Thorpe, Thomas Thorpe, Javier Tiffenberg, Nhan Tran, Marco Trovato, Christopher Tully, Tony Tyson, Tanmay Vachaspati, Sven Vahsen, Karl van Bibber, Justin Vandenbroucke, Anthony Villano, Tomer Volansky, Guojian Wang, Thomas Ward, William Wester, Andrew Whitbeck, David A. Williams, Matthew Wing, Lindley Winslow, Bogdan Wojtsekhowski, Hai-Bo Yu, Shin-Shan Yu, Tien-Tien Yu, Xilin Zhang, Yue Zhao, Yi-Ming Zhong
Aaron Chou, Henry Glass, H. Richard Gustafson, Craig J. Hogan, Brittany L. Kamai, Ohkyung Kwon, Robert Lanza, Lee McCuller, Stephan S. Meyer, Jonathan W. Richardson, Chris Stoughton, Ray Tomlin, Rainer Weiss
Final measurements and analysis are reported from the first-generation Holometer, the first instrument capable of measuring correlated variations in space-time position at strain noise power spectral densities smaller than a Planck time. The apparatus consists of two co-located, but independent and isolated, 40 m power-recycled Michelson interferometers, whose outputs are cross-correlated to 25 MHz. The data are sensitive to correlations of differential position across the apparatus over a broad band of frequencies up to and exceeding the inverse light crossing time, 7.6 MHz. By measuring with Planck precision the correlation of position variations at spacelike separations, the Holometer searches for faint, irreducible correlated position noise backgrounds predicted by some models of quantum space-time geometry. The first-generation optical layout is sensitive to quantum geometrical noise correlations with shear symmetry---those that can be interpreted as a fundamental noncommutativity of space-time position in orthogonal directions. General experimental constraints are placed on parameters of a set of models of spatial shear noise correlations, with a sensitivity that exceeds the Planck-scale holographic information bound on position states by a large factor. This result significantly extends the upper limits placed on models of directional noncommutativity by currently operating gravitational wave observatories.
Zeeshan Ahmed, Yuri Alexeev, Giorgio Apollinari, Asimina Arvanitaki, David Awschalom, Karl K. Berggren, Karl Van Bibber, Przemyslaw Bienias, Geoffrey Bodwin, Malcolm Boshier, Daniel Bowring, Davide Braga, Karen Byrum, Gustavo Cancelo, Gianpaolo Carosi, Tom Cecil, Clarence Chang, Mattia Checchin, Sergei Chekanov, Aaron Chou, Aashish Clerk, Ian Cloet, Michael Crisler, Marcel Demarteau, Ranjan Dharmapalan, Matthew Dietrich, Junjia Ding, Zelimir Djurcic, John Doyle, James Fast, Michael Fazio, Peter Fierlinger, Hal Finkel, Patrick Fox, Gerald Gabrielse, Andrei Gaponenko, Maurice Garcia-Sciveres, Andrew Geraci, Jeffrey Guest, Supratik Guha, Salman Habib, Ron Harnik, Amr Helmy, Yuekun Heng, Jason Henning, Joseph Heremans, Phay Ho, Jason Hogan, Johannes Hubmayr, David Hume, Kent Irwin, Cynthia Jenks, Nick Karonis, Raj Kettimuthu, Derek Kimball, Jonathan King, Eve Kovacs, Richard Kriske, Donna Kubik, Akito Kusaka, Benjamin Lawrie, Konrad Lehnert, Paul Lett, Jonathan Lewis, Pavel Lougovski, Larry Lurio, Xuedan Ma, Edward May, Petra Merkel, Jessica Metcalfe, Antonino Miceli, Misun Min, Sandeep Miryala, John Mitchell, Vesna Mitrovic, Holger Mueller, Sae Woo Nam, Hogan Nguyen, Howard Nicholson, Andrei Nomerotski, Michael Norman, Kevin O'Brien, Roger O'Brient, Umeshkumar Patel, Bjoern Penning, Sergey Perverzev, Nicholas Peters, Raphael Pooser, Chrystian Posada, James Proudfoot, Tenzin Rabga, Tijana Rajh, Sergio Rescia, Alexander Romanenko, Roger Rusack, Monika Schleier-Smith, Keith Schwab, Julie Segal, Ian Shipsey, Erik Shirokoff, Andrew Sonnenschein, Valerie Taylor, Robert Tschirhart, Chris Tully, David Underwood, Vladan Vuletic, Robert Wagner, Gensheng Wang, Harry Weerts, Nathan Woollett, Junqi Xie, Volodymyr Yefremenko, John Zasadzinski, Jinlong Zhang, Xufeng Zhang, Vishnu Zutshi
Report of the first workshop to identify approaches and techniques in the domain of quantum sensing that can be utilized by future High Energy Physics applications to further the scientific goals of High Energy Physics.
Ankur Agrawal, Akash V. Dixit, Tanay Roy, Srivatsan Chakram, Kevin He, Ravi K. Naik, David I. Schuster, Aaron Chou
The manipulation of quantum states of light has resulted in significant advancements in both dark matter searches and gravitational wave detectors [1-4]. Current dark matter searches operating in the microwave frequency range use nearly quantum-limited amplifiers [3, 5, 6]. Future high frequency searches will use photon counting techniques [1] to evade the standard quantum limit. We present a signal enhancement technique that utilizes a superconducting qubit to prepare a superconducting microwave cavity in a non-classical Fock state and stimulate the emission of a photon from a dark matter wave. By initializing the cavity in an $|n=4\rangle$ Fock state, we demonstrate a quantum enhancement technique that increases the signal photon rate and hence also the dark matter scan rate each by a factor of 2.78. Using this technique, we conduct a dark photon search in a band around $\mathrm{5.965\, GHz \, (24.67\, μeV)}$, where the kinetic mixing angle $ε\geq 4.35 \times 10^{-13}$ is excluded at the $90\%$ confidence level.
Pete Barry, Karl Berggren, A. Baha Balantekin, John Bollinger, Ray Bunker, Ilya Charaev, Jeff Chiles, Aaron Chou, Marcel Demarteau, Joe Formaggio, Peter Graham, Salman Habib, David Hume, Kent Irwin, Mikhail Lukin, Joseph Lykken, Reina Maruyama, Holger Mueller, SaeWoo Nam, Andrei Nomerotski, John Orrell, Robert Plunkett, Raphael Pooser, John Preskill, Surjeet Rajendran, Alex Sushkov, Ronald Walsworth
A subset of QuantISED Sensor PIs met virtually on May 26, 2020 to discuss a response to a charge by the DOE Office of High Energy Physics. In this document, we summarize the QuantISED sensor community discussion, including a consideration of HEP science enabled by quantum sensors, describing the distinction between Quantum 1.0 and Quantum 2.0, and discussing synergies/complementarity with the new DOE NQI centers and with research supported by other SC offices. Quantum 2.0 advances in sensor technology offer many opportunities and new approaches for HEP experiments. The DOE HEP QuantISED program could support a portfolio of small experiments based on these advances. QuantISED experiments could use sensor technologies that exemplify Quantum 2.0 breakthroughs. They would strive to achieve new HEP science results, while possibly spinning off other domain science applications or serving as pathfinders for future HEP science targets. QuantISED experiments should be led by a DOE laboratory, to take advantage of laboratory technical resources, infrastructure, and expertise in the safe and efficient construction, operation, and review of experiments. The QuantISED PIs emphasized that the quest for HEP science results under the QuantISED program is distinct from the ongoing DOE HEP programs on the energy, intensity, and cosmic frontiers. There is robust evidence for the existence of particles and phenomena beyond the Standard Model, including dark matter, dark energy, quantum gravity, and new physics responsible for neutrino masses, cosmic inflation, and the cosmic preference for matter over antimatter. Where is this physics and how do we find it? The QuantISED program can exploit new capabilities provided by quantum technology to probe these kinds of science questions in new ways and over a broader range of science parameters than can be achieved with conventional techniques.
Akash V. Dixit, Srivatsan Chakram, Kevin He, Ankur Agrawal, Ravi K. Naik, David I. Schuster, Aaron Chou
Detection mechanisms for low mass bosonic dark matter candidates, such the axion or hidden photon, leverage potential interactions with electromagnetic fields, whereby the dark matter (of unknown mass) on rare occasion converts into a single photon. Current dark matter searches operating at microwave frequencies use a resonant cavity to coherently accumulate the field sourced by the dark matter and a near standard quantum limited (SQL) linear amplifier to read out the cavity signal. To further increase sensitivity to the dark matter signal, sub-SQL detection techniques are required. Here we report the development of a novel microwave photon counting technique and a new exclusion limit on hidden photon dark matter. We operate a superconducting qubit to make repeated quantum non-demolition measurements of cavity photons and apply a hidden Markov model analysis to reduce the noise to 15.7 dB below the quantum limit, with overall detector performance limited by a residual background of real photons. With the present device, we perform a hidden photon search and constrain the kinetic mixing angle to $ε\leq 1.68 \times 10^{-15}$ in a band around 6.011 GHz (24.86 $μ$eV) with an integration time of 8.33 s. This demonstrated noise reduction technique enables future dark matter searches to be sped up by a factor of 1300. By coupling a qubit to an arbitrary quantum sensor, more general sub-SQL metrology is possible with the techniques presented in this work.
Aaron Chou, Henry Glass, H. Richard Gustafson, Craig Hogan, Brittany L. Kamai, Ohkyung Kwon, Robert Lanza, Lee McCuller, Stephan S. Meyer, Jonathan Richardson, Chris Stoughton, Ray Tomlin, Rainer Weiss
This paper describes the Fermilab Holometer, an instrument for measuring correlations of position variations over a four-dimensional volume of space-time. The apparatus consists of two co-located, but independent and isolated, 40m power-recycled Michelson interferometers, whose outputs are cross-correlated to 25 MHz. The data are sensitive to correlations of differential position across the apparatus over a broad band of frequencies up to and exceeding the inverse light crossing time, 7.6 MHz. A noise model constrained by diagnostic and environmental data distinguishes among physical origins of measured correlations, and is used to verify shot-noise-limited performance. These features allow searches for exotic quantum correlations that depart from classical trajectories at spacelike separations, with a strain noise power spectral density sensitivity smaller than the Planck time. The Holometer in current and future configurations is projected to provide precision tests of a wide class of models of quantum geometry at the Planck scale, beyond those already constrained by currently operating gravitational wave observatories.
Fabian Schmidt, Maximo Ave, Lorenzo Cazon, Aaron Chou
Dec 21, 2007·astro-ph·PDF Surface detector arrays are designed to measure the spectrum and composition of high-energy cosmic rays by detecting the secondary particle flux of the Extensive Air Showers (EAS) induced by the primary cosmic rays. Electromagnetic particles and muons constitute the dominant contribution to the ground detector signals. In this paper, we show that the ground signal deposit of an EAS can be described in terms of only very few parameters: the primary energy E, the zenith angle theta, the distance of the shower maximum X_max to the ground, and a muon flux normalization N_mu. This set of physical parameters is sufficient to predict the average particle fluxes at ground level to around 10% accuracy. We show that this is valid for hadronic air showers, using the two standard hadronic interaction models used in cosmic ray physics, QGSJetII and Sibyll, and for primaries from protons to iron. Based on this model, a new approach to calibrating the energy scale of ground array experiments is developed, which factors out the model dependence inherent in such calibrations up to now. Additionally, the method yields a measurement of the average number of muons in EAS. The measured distribution of N_mu of cosmic ray air showers can then be analysed, in conjunction with measurements of X_max from fluorescence detectors, to put constraints on the cosmic ray composition and hadronic interaction models.
Fabian Schmidt, Maximo Ave, Lorenzo Cazon, Aaron Chou
Jun 13, 2007·astro-ph·PDF Air shower universality states that the electromagnetic part of hadron-induced extensive air showers (EAS) can be completely described in terms of the primary energy and shower age. In addition, simulations show that the muon part is well characterized by an overall normalization which depends on the primary particle and hadronic interaction model. We investigate the consequences of EAS universality for ground arrays, which sample EAS at large core distances, and show how universality can be used to experimentally determine the muon content as well as the primary energy of cosmic ray air showers in a model-independent way.
Jorge de Blas, Monica Dunford, Emanuele Bagnaschi, Ayres Freitas, Pier Paolo Giardino, Christian Grefe, Michele Selvaggi, Angela Taliercio, Falk Bartels, Andrea Dainese, Cristinel Diaconu, Chiara Signorile-Signorile, Néstor Armesto, Roberta Arnaldi, Andy Buckley, David d'Enterria, Antoine Gérardin, Valentina Mantovani Sarti, Sven-Olaf Moch, Marco Pappagallo, Raimond Snellings, Urs Achim Wiedemann, Gino Isidori, Marie-Hélène Schune, Maria Laura Piscopo, Marta Calvi, Yuval Grossman, Thibaud Humair, Andreas Jüttner, Jernej F. Kamenik, Matthew Kenzie, Patrick Koppenburg, Radoslav Marchevski, Angela Papa, Guillaume Pignol, Justine Serrano, Pilar Hernandez, Sara Bolognesi, Ivan Esteban, Stephen Dolan, Valerie Domcke, Joseph Formaggio, M. C. Gonzalez-Garcia, Aart Heijboer, Aldo Ianni, Joachim Kopp, Elisa Resconi, Mark Scott, Viola Sordini, Fabio Maltoni, Rebeca Gonzalez Suarez, Benedikt Maier, Timothy Cohen, Annapaola de Cosa, Nathaniel Craig, Roberto Franceschini, Loukas Gouskos, Aurelio Juste, Sophie Renner, Lesya Shchutska, Jocelyn Monroe, Matthew McCullough, Yohei Ema, Paolo Agnes, Francesca Calore, Emanuele Castorina, Aaron Chou, Monica D'Onofrio, Maksym Ovchynnikov, Tina Pollman, Josef Pradler, Yotam Soreq, Julia Katharina Vogel, Gianluigi Arduini, Philip Burrows, Jacqueline Keintzel, Deepa Angal-Kalinin, Bernhard Auchmann, Massimo Ferrario, Angeles Faus Golfe, Roberto Losito, Anke-Susanne Mueller, Tor Raubenheimer, Marlene Turner, Pierre Vedrine, Hans Weise, Walter Wuensch, Chenghui Yu, Thomas Bergauer, Ulrich Husemann, Dorothea vom Bruch, Thea Aarrestad, Daniela Bortoletto, Shikma Bressler, Marcel Demarteau, Michael Doser, Gabriella Gaudio, Inés Gil-Botella, Andrea Giuliani, Fabrizio Palla, Rok Pestotnik, Felix Sefkow, Frank Simon, Maksym Titov, Tommaso Boccali, Borut Kersevan, Daniel Murnane, Gonzalo Merino Arevalo, John Derek Chapman, Frank-Dieter Gaede, Stefano Giagu, Maria Girone, Heather M. Gray, Giovanni Iadarola, Stephane Jezequel, Gregor Kasieczka, David Lange, Sinéad M. Ryan, Nicole Skidmore, Sofia Vallecorsa, Eric Laenen, Anadi Canepa, Xinchou Lou, Rogerio Rosenfeld, Yuji Yamazaki, Roger Forty, Karl Jakobs, Hugh Montgomery, Mike Seidel, Paris Sphicas
Ivone F. M. Albuquerque, Aaron Chou
The highest energy cosmic ray event reported by the Auger Observatory has an energy of 148 EeV. It does not correlate with any nearby (z$<$0.024) object capable of originating such a high energy event. Intrigued by the fact that the highest energy event ever recorded (by the Fly's Eye collaboration) points to a faraway quasar with very high radio luminosity and large Faraday rotation measurement, we have searched for a similar source for the Auger event. We find that the Auger highest energy event points to a quasar with similar characteristics to the one correlated to the Fly's Eye event. We also find the same kind of correlation for one of the highest energy AGASA events. We conclude that so far these types of quasars are the best source candidates for both Auger and Fly's Eye highest energy events. We discuss a few exotic candidates that could reach us from gigaparsec distances.
Fang Zhao, Ziqian Li, Akash V. Dixit, Tanay Roy, Andrei Vrajitoarea, Riju Banerjee, Alexander Anferov, Kan-Heng Lee, David I. Schuster, Aaron Chou
Jan 12, 2025·quant-ph·PDF Developing a dark matter detector with wide mass tunability is an immensely desirable property, yet it is challenging due to maintaining strong sensitivity. Resonant cavities for dark matter detection have traditionally employed mechanical tuning, moving parts around to change electromagnetic boundary conditions. However, these cavities have proven challenging to operate in sub-Kelvin cryogenic environments due to differential thermal contraction, low heat capacities, and low thermal conductivities. Instead, we develop an electronically tunable cavity architecture by coupling a superconducting 3D microwave cavity with a DC flux tunable SQUID. With a flux delivery system engineered to maintain high coherence in the cavity, we perform a hidden-photon dark matter search below the quantum-limited threshold. A microwave photon counting technique is employed through repeated quantum non-demolition measurements using a transmon qubit. With this device, we perform a hidden-photon search and constrain the kinetic mixing angle to ${\varepsilon}< 8.2\times 10^{-15}$ in a tunable band from 5.672 GHz to 5.694 GHz. By coupling multimode tunable cavities to the transmon, wider hidden-photon searching ranges are possible.
Jesse Liu, Kristin Dona, Gabe Hoshino, Stefan Knirck, Noah Kurinsky, Matthew Malaker, David W. Miller, Andrew Sonnenschein, Mohamed H. Awida, Peter S. Barry, Karl K. Berggren, Daniel Bowring, Gianpaolo Carosi, Clarence Chang, Aaron Chou, Rakshya Khatiwada, Samantha Lewis, Juliang Li, Sae Woo Nam, Omid Noroozian, Tony X. Zhou
We introduce the Broadband Reflector Experiment for Axion Detection (BREAD) conceptual design and science program. This haloscope plans to search for bosonic dark matter across the [10$^{-3}$, 1] eV ([0.24, 240] THz) mass range. BREAD proposes a cylindrical metal barrel to convert dark matter into photons, which a novel parabolic reflector design focuses onto a photosensor. This unique geometry enables enclosure in standard cryostats and high-field solenoids, overcoming limitations of current dish antennas. A pilot 0.7 m$^{2}$ barrel experiment planned at Fermilab is projected to surpass existing dark photon coupling constraints by over a decade with one-day runtime. Axion sensitivity requires $<10^{-20}$ W/$\sqrt{\textrm{Hz}}$ sensor noise equivalent power with a 10 T solenoid and 10 m$^{2}$ barrel. We project BREAD sensitivity for various sensor technologies and discuss future prospects.