Pub Date : 2026-02-10DOI: 10.1088/1475-7516/2026/02/026
Jason Arakawa, Muhammad H. Zaheer, Volodymyr Takhistov, Marianna S. Safronova, Joshua Eby and Charles Cheung
Ultralight bosonic (ULB) fields with mass mϕ ≪ 1 eV often arise in theories beyond the Standard Model (SM). If such fields exist, violent astrophysical events that result in emission of gravitational wave, photon, or neutrino signals could also produce bursts of high-density relativistic ULB fields. Detection of such ULB fields in terrestrial or space-based laboratories correlated with other signals from transient astrophysical events opens a novel avenue for multimessenger astronomy. We show that quantum sensors are particularly well-suited to observe emitted scalar and pseudoscalar axion-like ULB fields coupled to SM. We demonstrate that multimessenger astronomy with ULB fields is possible even when accounting for matter screening effects.
{"title":"Multimessenger astronomy beyond the Standard Model: New window from quantum sensors","authors":"Jason Arakawa, Muhammad H. Zaheer, Volodymyr Takhistov, Marianna S. Safronova, Joshua Eby and Charles Cheung","doi":"10.1088/1475-7516/2026/02/026","DOIUrl":"https://doi.org/10.1088/1475-7516/2026/02/026","url":null,"abstract":"Ultralight bosonic (ULB) fields with mass mϕ ≪ 1 eV often arise in theories beyond the Standard Model (SM). If such fields exist, violent astrophysical events that result in emission of gravitational wave, photon, or neutrino signals could also produce bursts of high-density relativistic ULB fields. Detection of such ULB fields in terrestrial or space-based laboratories correlated with other signals from transient astrophysical events opens a novel avenue for multimessenger astronomy. We show that quantum sensors are particularly well-suited to observe emitted scalar and pseudoscalar axion-like ULB fields coupled to SM. We demonstrate that multimessenger astronomy with ULB fields is possible even when accounting for matter screening effects.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"45 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146145913","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-10DOI: 10.1088/1361-6382/ae0aad
K E Saavik Ford and Barry McKernan
Active galactic nuclei (AGN) are powered by accretion disks onto supermassive black holes (SMBHs) in the centers of galaxies. AGN are believed to play important roles in the evolution of both SMBHs and their host galaxies over cosmic time. AGN and the nuclear star clusters (NSCs) that interact with them remain unresolved with present and planned telescopes. As a result, the properties of AGN and NSCs are highly uncertain. Here we review how binary black hole (BBH) mergers can occur in AGN disks and how both the gravitational wave and electromagnetic wave properties of such mergers allow us to reverse-engineer the properties of AGN disks and NSCs over cosmic time. We point out that the feature in the BBH mass spectrum around is an excellent probe of hierarchical merger models. Likewise constraints on the spins of upper-mass gap BH ( ) test the AGN channel. The effective spin ( ) distribution, including asymmetry, islands of structure and magnitudes are excellent tests of AGN model predictions. We also argue, that the rate of AGN-driven BBH mergers as a function of redshift should scale slightly shallower than the AGN number density, at least out to redshifts of , and should turnover at the same redshift as the AGN number density. Finally, we emphasize a determination of an AGN fraction of observed BBH mergers ( ), regardless of the actual value, allows us to infer the average properties of AGN disks and NSCs out to high redshift.
{"title":"Using gravitational waves & multi-messenger astronomy to reverse-engineer the properties of galactic nuclei","authors":"K E Saavik Ford and Barry McKernan","doi":"10.1088/1361-6382/ae0aad","DOIUrl":"https://doi.org/10.1088/1361-6382/ae0aad","url":null,"abstract":"Active galactic nuclei (AGN) are powered by accretion disks onto supermassive black holes (SMBHs) in the centers of galaxies. AGN are believed to play important roles in the evolution of both SMBHs and their host galaxies over cosmic time. AGN and the nuclear star clusters (NSCs) that interact with them remain unresolved with present and planned telescopes. As a result, the properties of AGN and NSCs are highly uncertain. Here we review how binary black hole (BBH) mergers can occur in AGN disks and how both the gravitational wave and electromagnetic wave properties of such mergers allow us to reverse-engineer the properties of AGN disks and NSCs over cosmic time. We point out that the feature in the BBH mass spectrum around is an excellent probe of hierarchical merger models. Likewise constraints on the spins of upper-mass gap BH ( ) test the AGN channel. The effective spin ( ) distribution, including asymmetry, islands of structure and magnitudes are excellent tests of AGN model predictions. We also argue, that the rate of AGN-driven BBH mergers as a function of redshift should scale slightly shallower than the AGN number density, at least out to redshifts of , and should turnover at the same redshift as the AGN number density. Finally, we emphasize a determination of an AGN fraction of observed BBH mergers ( ), regardless of the actual value, allows us to infer the average properties of AGN disks and NSCs out to high redshift.","PeriodicalId":10282,"journal":{"name":"Classical and Quantum Gravity","volume":"15 1","pages":""},"PeriodicalIF":3.5,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146146188","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
High-dimensional encoding of quantum information holds the potential to greatly increase the computational power of existing devices by enlarging the accessible state space for a fixed register size and by reducing the number of required entangling gates. However, qudit-based quantum computation remains far less developed than conventional qubit-based approaches, particularly for photons, which represent natural multilevel information carriers that play a crucial role in the development of quantum networks. A major obstacle for realizing quantum gates between two individual photons is the restriction of direct interaction between photons in linear media. In particular, essential logic components for quantum operations such as native qudit–qudit entangling gates are still missing for optical quantum information processing. Here we address this challenge by presenting a protocol for realizing an entangling gate—the controlled phase-flip gate—for two photonic qudits in an arbitrary dimension. We experimentally demonstrate this protocol by realizing a four-dimensional qudit–qudit controlled phase-flip gate, whose decomposition would require at least 13 two-qubit entangling gates. Our photonic qudits are encoded in orbital angular momentum, and we have developed a new active high-precision phase-locking technology to construct a high-dimensional orbital angular momentum beamsplitter that increases the stability of the controlled phase-flip gate, resulting in a process fidelity within a range of [0.71 ± 0.01, 0.85 ± 0.01]. Our experiment represents an important advance for high-dimensional optical quantum information processing and has the potential for wider applications beyond optical system.
{"title":"Heralded high-dimensional photon–photon quantum gate","authors":"Zhi-Feng Liu, Zhi-Cheng Ren, Pei Wan, Wen-Zheng Zhu, Zi-Mo Cheng, Jing Wang, Yu-Peng Shi, Han-Bing Xi, Marcus Huber, Nicolai Friis, Xiaoqin Gao, Xi-Lin Wang, Hui-Tian Wang","doi":"10.1038/s41566-026-01846-x","DOIUrl":"https://doi.org/10.1038/s41566-026-01846-x","url":null,"abstract":"High-dimensional encoding of quantum information holds the potential to greatly increase the computational power of existing devices by enlarging the accessible state space for a fixed register size and by reducing the number of required entangling gates. However, qudit-based quantum computation remains far less developed than conventional qubit-based approaches, particularly for photons, which represent natural multilevel information carriers that play a crucial role in the development of quantum networks. A major obstacle for realizing quantum gates between two individual photons is the restriction of direct interaction between photons in linear media. In particular, essential logic components for quantum operations such as native qudit–qudit entangling gates are still missing for optical quantum information processing. Here we address this challenge by presenting a protocol for realizing an entangling gate—the controlled phase-flip gate—for two photonic qudits in an arbitrary dimension. We experimentally demonstrate this protocol by realizing a four-dimensional qudit–qudit controlled phase-flip gate, whose decomposition would require at least 13 two-qubit entangling gates. Our photonic qudits are encoded in orbital angular momentum, and we have developed a new active high-precision phase-locking technology to construct a high-dimensional orbital angular momentum beamsplitter that increases the stability of the controlled phase-flip gate, resulting in a process fidelity within a range of [0.71 ± 0.01, 0.85 ± 0.01]. Our experiment represents an important advance for high-dimensional optical quantum information processing and has the potential for wider applications beyond optical system.","PeriodicalId":18926,"journal":{"name":"Nature Photonics","volume":"3 1","pages":""},"PeriodicalIF":35.0,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146152330","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-10DOI: 10.1051/0004-6361/202557914
Jean-François Gonzalez, Stéphane Michoulier
Context. The radial drift and fragmentation of small dust grains in protoplanetary discs impedes their growth past centimetre sizes. Several mechanisms have been proposed to overcome these planet formation barriers, such as dust porosity or the streaming instability (SI), which is today regarded as the most promising mechanism to form planetesimals.Aims. Here, we examine whether the conditions for the SI to lead to strong clumping (the first step in planetesimal formation) are realised in protoplanetary discs containing porous grains.Methods. We used results from previous simulations of the evolution of porous grains subjected to growth, fragmentation, compaction, and bouncing in protoplanetary discs. In the ensuing disc structures, we determined the regions where the dust-to-gas ratio exceeds the critical value for strong clumping found in simulations of the SI including external turbulence.Results. We find that the conditions for strong clumping are met within the first hundred thousand years in large regions of protoplanetary discs containing porous grains, provided that the CO snow line is taken into account. If the CO snow line is neglected, the conditions are only met very close to the inner disc edge early on or over large areas well after 200 000 yr.
{"title":"The CO snow line favours strong clumping by the streaming instability in protoplanetary discs with porous grains","authors":"Jean-François Gonzalez, Stéphane Michoulier","doi":"10.1051/0004-6361/202557914","DOIUrl":"https://doi.org/10.1051/0004-6361/202557914","url":null,"abstract":"<i>Context.<i/> The radial drift and fragmentation of small dust grains in protoplanetary discs impedes their growth past centimetre sizes. Several mechanisms have been proposed to overcome these planet formation barriers, such as dust porosity or the streaming instability (SI), which is today regarded as the most promising mechanism to form planetesimals.<i>Aims.<i/> Here, we examine whether the conditions for the SI to lead to strong clumping (the first step in planetesimal formation) are realised in protoplanetary discs containing porous grains.<i>Methods.<i/> We used results from previous simulations of the evolution of porous grains subjected to growth, fragmentation, compaction, and bouncing in protoplanetary discs. In the ensuing disc structures, we determined the regions where the dust-to-gas ratio exceeds the critical value for strong clumping found in simulations of the SI including external turbulence.<i>Results.<i/> We find that the conditions for strong clumping are met within the first hundred thousand years in large regions of protoplanetary discs containing porous grains, provided that the CO snow line is taken into account. If the CO snow line is neglected, the conditions are only met very close to the inner disc edge early on or over large areas well after 200 000 yr.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"11 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146153540","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-10DOI: 10.1051/0004-6361/202557682
Zhaosheng Li, Lucien Kuiper, Yuanyue Pan, Renxin Xu, Mingyu Ge, Shanshan Weng, Long Peng, Wenhui Yu, Yue Huang, Liang Zhang, Liming Song, Sergey V. Molkov, Alexander A. Lutovinov, Shu Zhang, Shuang-Nan Zhang
We presented a comprehensive multi-epoch timing and multiwavelength analysis of the accreting millisecond X-ray pulsar MAXI J1957+032, covering two major outbursts in 2022 and 2025. By reanalyzing the 2022 outburst data from the Neutron Star Interior Composition Explorer (NICER), we found the spin frequency and orbital parameters from the observations in 0.3–5 keV. For the 2025 outburst, we reported the detection of pulsations with the Einstein Probe (EP). Based on the ∼3-year baseline between these two outbursts, we measured a significant long-term spin-down rate of . Assuming that the quiescent spin-down is driven by magnetic dipole radiation, we inferred a spin-down luminosity of L ≈ 1.1 × 1036 erg s−1 and a surface dipolar magnetic field of B ≈ (7.3 − 10.4)×108 G. Furthermore, we conducted a deep radio pulsation search with the Five-hundred-meter Aperture Spherical radio Telescope (FAST) during the X-ray quiescent state in 2024, resulting in a non-detection with a 7σ flux density upper limit of 12.3 μJy. This corresponds to a radio efficiency upper limit of ξ < 2.8 × 10−10, which is significantly lower than that of typical millisecond pulsars with a similar spin-down power. This profound radio pulsation faintness can be explained by two primary scenarios: either a geometric effect, wherein the pulsar’s radio beam is directed away from our line of sight, or a physical suppression of the emission mechanism, potentially caused by a persistent low-level accretion flow during the X-ray quiescent state.
{"title":"X-ray and radio observations of the AMXP MAXI J1957+032 covering the 2022–2025 outbursts","authors":"Zhaosheng Li, Lucien Kuiper, Yuanyue Pan, Renxin Xu, Mingyu Ge, Shanshan Weng, Long Peng, Wenhui Yu, Yue Huang, Liang Zhang, Liming Song, Sergey V. Molkov, Alexander A. Lutovinov, Shu Zhang, Shuang-Nan Zhang","doi":"10.1051/0004-6361/202557682","DOIUrl":"https://doi.org/10.1051/0004-6361/202557682","url":null,"abstract":"We presented a comprehensive multi-epoch timing and multiwavelength analysis of the accreting millisecond X-ray pulsar MAXI J1957+032, covering two major outbursts in 2022 and 2025. By reanalyzing the 2022 outburst data from the <i>Neutron Star Interior Composition Explorer<i/> (NICER), we found the spin frequency and orbital parameters from the observations in 0.3–5 keV. For the 2025 outburst, we reported the detection of pulsations with the <i>Einstein Probe<i/> (EP). Based on the ∼3-year baseline between these two outbursts, we measured a significant long-term spin-down rate of . Assuming that the quiescent spin-down is driven by magnetic dipole radiation, we inferred a spin-down luminosity of <i>L<i/> ≈ 1.1 × 10<sup>36<sup/> erg s<sup>−1<sup/> and a surface dipolar magnetic field of <i>B<i/> ≈ (7.3 − 10.4)×10<sup>8<sup/> G. Furthermore, we conducted a deep radio pulsation search with the <i>Five-hundred-meter Aperture Spherical radio Telescope<i/> (FAST) during the X-ray quiescent state in 2024, resulting in a non-detection with a 7<i>σ<i/> flux density upper limit of 12.3 μJy. This corresponds to a radio efficiency upper limit of <i>ξ<i/> < 2.8 × 10<sup>−10<sup/>, which is significantly lower than that of typical millisecond pulsars with a similar spin-down power. This profound radio pulsation faintness can be explained by two primary scenarios: either a geometric effect, wherein the pulsar’s radio beam is directed away from our line of sight, or a physical suppression of the emission mechanism, potentially caused by a persistent low-level accretion flow during the X-ray quiescent state.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"97 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146153542","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-10DOI: 10.1088/2058-9565/ae3fc8
Chenyu Shi, Vedran Dunjko and Hao Wang
The variational quantum eigensolver (VQE) is one of the most prominent algorithms using near-term quantum devices, designed to find the ground state of a Hamiltonian. In VQE, a classical optimizer iteratively updates the parameters in the quantum circuit. Among various optimization methods, the quantum natural gradient descent (QNG) stands out as a promising optimization approach for VQE. However, standard QNG only leverages the quantum Fisher information of the entire system and treats each subsystem equally in the optimization process, without accounting for the different weights and contributions of each subsystem corresponding to each local term in the Hamiltonian. To address this limitation, we propose a Weighted Approximate QNG (WA-QNG) method tailored for k-local Hamiltonians. In this paper, we theoretically analyze the potential advantages of WA-QNG compared to QNG from three distinct perspectives and reveal its connection with the Gauss–Newton method. We also show it outperforms the standard QNG descent in the numerical simulations for seeking the ground state of the Hamiltonian.
{"title":"Weighted approximate quantum natural gradient for variational quantum eigensolver","authors":"Chenyu Shi, Vedran Dunjko and Hao Wang","doi":"10.1088/2058-9565/ae3fc8","DOIUrl":"https://doi.org/10.1088/2058-9565/ae3fc8","url":null,"abstract":"The variational quantum eigensolver (VQE) is one of the most prominent algorithms using near-term quantum devices, designed to find the ground state of a Hamiltonian. In VQE, a classical optimizer iteratively updates the parameters in the quantum circuit. Among various optimization methods, the quantum natural gradient descent (QNG) stands out as a promising optimization approach for VQE. However, standard QNG only leverages the quantum Fisher information of the entire system and treats each subsystem equally in the optimization process, without accounting for the different weights and contributions of each subsystem corresponding to each local term in the Hamiltonian. To address this limitation, we propose a Weighted Approximate QNG (WA-QNG) method tailored for k-local Hamiltonians. In this paper, we theoretically analyze the potential advantages of WA-QNG compared to QNG from three distinct perspectives and reveal its connection with the Gauss–Newton method. We also show it outperforms the standard QNG descent in the numerical simulations for seeking the ground state of the Hamiltonian.","PeriodicalId":20821,"journal":{"name":"Quantum Science and Technology","volume":"11 1","pages":""},"PeriodicalIF":6.7,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146146192","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-10DOI: 10.1007/s10714-026-03515-4
Luis Aké Hau, Saul Burgos, Didier A. Solis
{"title":"The causal structure of the c-completion of warped spacetimes","authors":"Luis Aké Hau, Saul Burgos, Didier A. Solis","doi":"10.1007/s10714-026-03515-4","DOIUrl":"https://doi.org/10.1007/s10714-026-03515-4","url":null,"abstract":"","PeriodicalId":578,"journal":{"name":"General Relativity and Gravitation","volume":"9 1","pages":""},"PeriodicalIF":2.8,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146153609","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-10DOI: 10.1051/0004-6361/202558710
R. Weinberger, C. Pfrommer
A significant fraction of galaxy clusters show central cooling times of less than 1 Gyr and associated central cluster entropies below 30 keV cm2. We provide a straightforward explanation for these low central entropies in cool core systems and how this is related to accretion onto supermassive black holes (SMBHs). Assuming a time-averaged equilibrium between active galactic nucleus (AGN) jet heating of the radiatively cooling intracluster medium and Bondi accretion, we derived an equilibrium entropy that scales with the SMBH and cluster mass as . At fixed cluster mass, overly massive SMBHs would raise the central entropy above the cool core threshold, thus implying a novel way of limiting SMBH masses in cool-core clusters. We find a limiting mass of 1.4 × 1010 M⊙ in a cool-core cluster of mass 1015 M⊙. We carried out three-dimensional hydrodynamical simulations of an idealised Perseus-like cluster with AGN jets and find that they reproduce the predictions of our analytic model, once corrections for elevated jet entropies are applied when calculating X-ray emissivity-weighted cluster entropies. Our findings have significant implications for modelling galaxy clusters in cosmological simulations: a combination of overmassive SMBHs and high heating efficiencies precludes the formation of cool-core clusters.
{"title":"How supermassive black holes shape central entropies in galaxy clusters","authors":"R. Weinberger, C. Pfrommer","doi":"10.1051/0004-6361/202558710","DOIUrl":"https://doi.org/10.1051/0004-6361/202558710","url":null,"abstract":"A significant fraction of galaxy clusters show central cooling times of less than 1 Gyr and associated central cluster entropies below 30 keV cm<sup>2<sup/>. We provide a straightforward explanation for these low central entropies in cool core systems and how this is related to accretion onto supermassive black holes (SMBHs). Assuming a time-averaged equilibrium between active galactic nucleus (AGN) jet heating of the radiatively cooling intracluster medium and Bondi accretion, we derived an equilibrium entropy that scales with the SMBH and cluster mass as . At fixed cluster mass, overly massive SMBHs would raise the central entropy above the cool core threshold, thus implying a novel way of limiting SMBH masses in cool-core clusters. We find a limiting mass of 1.4 × 10<sup>10<sup/> M<sub>⊙<sub/> in a cool-core cluster of mass 10<sup>15<sup/> M<sub>⊙<sub/>. We carried out three-dimensional hydrodynamical simulations of an idealised Perseus-like cluster with AGN jets and find that they reproduce the predictions of our analytic model, once corrections for elevated jet entropies are applied when calculating X-ray emissivity-weighted cluster entropies. Our findings have significant implications for modelling galaxy clusters in cosmological simulations: a combination of overmassive SMBHs and high heating efficiencies precludes the formation of cool-core clusters.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"46 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146153658","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-10DOI: 10.1038/s41377-026-02221-9
Martin J Booth
{"title":"Inaugural message from the new Co-Editor-in-Chief.","authors":"Martin J Booth","doi":"10.1038/s41377-026-02221-9","DOIUrl":"https://doi.org/10.1038/s41377-026-02221-9","url":null,"abstract":"","PeriodicalId":18093,"journal":{"name":"Light, science & applications","volume":"15 1","pages":"112"},"PeriodicalIF":23.4,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146149419","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-10DOI: 10.22331/q-2026-02-10-2002
Roozbeh Bassirian, Adam Bouland, Bill Fefferman, Sam Gunn, Avishay Tal
Certified randomness has a long history in quantum information, with many potential applications. Recently Aaronson and Hung proposed a novel public certified randomness protocol based on existing random circuit sampling (RCS) experiments. The security of their protocol, however, relies on non-standard complexity-theoretic conjectures which were not previously studied in the literature.
Inspired by this work, we study certified randomness in the quantum random oracle model (QROM). We show that quantum Fourier Sampling can be used to define a publicly verifiable certified randomness protocol with black-box security without any computational assumptions. In addition to giving a certified randomness protocol in the QROM, our work can also be seen as supporting Aaronson and Hung's conjectures for RCS-based randomness generation, as our protocol is in some sense the "black-box version" of Aaronson and Hung's protocol. In further support of Aaronson and Hung's proposal, we prove a Fourier Sampling version of Aaronson and Hung's conjecture by extending Raz and Tal's separation of BQP vs PH.
Our work complements the subsequent certified randomness protocol of Yamakawa and Zhandry (2022) in the QROM. Whereas the security of that protocol relied on the Aaronson-Ambainis conjecture, ours does not rely on any computational assumption – at the expense of requiring exponential-time classical verification. Our protocol also has a simple heuristic implementation.
{"title":"On Certified Randomness from Fourier Sampling or Random Circuit Sampling","authors":"Roozbeh Bassirian, Adam Bouland, Bill Fefferman, Sam Gunn, Avishay Tal","doi":"10.22331/q-2026-02-10-2002","DOIUrl":"https://doi.org/10.22331/q-2026-02-10-2002","url":null,"abstract":"Certified randomness has a long history in quantum information, with many potential applications. Recently Aaronson and Hung proposed a novel public certified randomness protocol based on existing random circuit sampling (RCS) experiments. The security of their protocol, however, relies on non-standard complexity-theoretic conjectures which were not previously studied in the literature.<br/>\u0000<br/> Inspired by this work, we study certified randomness in the quantum random oracle model (QROM). We show that quantum Fourier Sampling can be used to define a publicly verifiable certified randomness protocol with black-box security without any computational assumptions. In addition to giving a certified randomness protocol in the QROM, our work can also be seen as supporting Aaronson and Hung's conjectures for RCS-based randomness generation, as our protocol is in some sense the \"black-box version\" of Aaronson and Hung's protocol. In further support of Aaronson and Hung's proposal, we prove a Fourier Sampling version of Aaronson and Hung's conjecture by extending Raz and Tal's separation of BQP vs PH.<br/>\u0000<br/> Our work complements the subsequent certified randomness protocol of Yamakawa and Zhandry (2022) in the QROM. Whereas the security of that protocol relied on the Aaronson-Ambainis conjecture, ours does not rely on any computational assumption – at the expense of requiring exponential-time classical verification. Our protocol also has a simple heuristic implementation.","PeriodicalId":20807,"journal":{"name":"Quantum","volume":"45 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146146747","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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