Pub Date : 2025-12-19DOI: 10.1021/acsphotonics.5c01253
Christian Soeller, Alexandre F. E. Bokhobza, Javier Casares-Arias, Alexander H. Clowsley
MINFLUX is a powerful single-molecule approach capable of achieving high spatially isotropic resolution in three dimensions. Current implementations collect localizations strictly serially, but criteria for when to terminate acquisition are often unclear. We therefore systematically investigate the time course of effective labeling efficiency (ELE) and achievable saturation values in MINFLUX 3D DNA-PAINT microscopy of Nup96 proteins in a U-2 OS-Nup96-mEGFP modified cell line using a commercial MINFLUX microscope. ELE was measured using a quantitative procedure based on maximum-likelihood template fitting. We collected data measured over various scan sizes and achieved ELE values of ∼60% after passing a time interval dependent on the region size, typically requiring long-duration acquisitions over several hours. Our data and a simple model suggest that maximizing marker detection is key to achieving the limits set by chemical labeling efficiency. A factor limiting the marker detection probability when using conventional DNA-PAINT markers is docking strand site-loss, observed over the duration required to build up the image data of MINFLUX acquisitions, which also limits the achievable number of labeling site visits to values around 1–3. Using repeat DNA-PAINT, i.e., employing oligonucleotide sequences with repeated docking sites, we observed greatly reduced site-loss and could increase the number of individual visits to site locations by more than 3-fold over the same period. Additionally, this enabled increasing stringency criteria for labeling (i.e., higher threshold values) and maximizing marker detection probabilities so that ELE reaches the limits set by chemical labeling efficiency.
MINFLUX是一种强大的单分子方法，能够在三维空间中实现高空间各向同性分辨率。当前的实现严格按顺序收集定位信息，但何时终止获取的标准往往不明确。因此，我们使用商用MINFLUX显微镜系统地研究了在U-2 OS-Nup96-mEGFP修饰细胞系中，在MINFLUX 3D DNA-PAINT显微镜下Nup96蛋白的有效标记效率（ELE）和可达到的饱和值的时间过程。使用基于最大似然模板拟合的定量程序测量ELE。我们收集了在各种扫描尺寸上测量的数据，并在通过依赖于区域大小的时间间隔后获得了约60%的ELE值，通常需要几个小时的长时间采集。我们的数据和一个简单的模型表明，最大化标记物检测是实现化学标记效率限制的关键。在使用传统DNA-PAINT标记时，限制标记检测概率的一个因素是对接链位点丢失，这是在建立MINFLUX获取的图像数据所需的持续时间内观察到的，这也限制了标记站点访问的可实现次数在1-3左右。使用重复DNA-PAINT，即使用具有重复对接位点的寡核苷酸序列，我们观察到大大减少了位点丢失，并且可以在同一时期将个体访问位点的次数增加3倍以上。此外，这增加了标记的严格标准（即更高的阈值）和最大化标记物检测概率，使ELE达到化学标记效率设定的极限。
{"title":"Optimizing Effective Labeling Efficiency in MINFLUX 3D DNA-PAINT Microscopy by Maximizing Marker Detection Probability","authors":"Christian Soeller, Alexandre F. E. Bokhobza, Javier Casares-Arias, Alexander H. Clowsley","doi":"10.1021/acsphotonics.5c01253","DOIUrl":"https://doi.org/10.1021/acsphotonics.5c01253","url":null,"abstract":"MINFLUX is a powerful single-molecule approach capable of achieving high spatially isotropic resolution in three dimensions. Current implementations collect localizations strictly serially, but criteria for when to terminate acquisition are often unclear. We therefore systematically investigate the time course of effective labeling efficiency (ELE) and achievable saturation values in MINFLUX 3D DNA-PAINT microscopy of Nup96 proteins in a U-2 OS-Nup96-mEGFP modified cell line using a commercial MINFLUX microscope. ELE was measured using a quantitative procedure based on maximum-likelihood template fitting. We collected data measured over various scan sizes and achieved ELE values of ∼60% after passing a time interval dependent on the region size, typically requiring long-duration acquisitions over several hours. Our data and a simple model suggest that maximizing marker detection is key to achieving the limits set by chemical labeling efficiency. A factor limiting the marker detection probability when using conventional DNA-PAINT markers is docking strand site-loss, observed over the duration required to build up the image data of MINFLUX acquisitions, which also limits the achievable number of labeling site visits to values around 1–3. Using repeat DNA-PAINT, i.e., employing oligonucleotide sequences with repeated docking sites, we observed greatly reduced site-loss and could increase the number of individual visits to site locations by more than 3-fold over the same period. Additionally, this enabled increasing stringency criteria for labeling (i.e., higher threshold values) and maximizing marker detection probabilities so that ELE reaches the limits set by chemical labeling efficiency.","PeriodicalId":23,"journal":{"name":"ACS Photonics","volume":"7 1","pages":""},"PeriodicalIF":7.0,"publicationDate":"2025-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145786329","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 : 2025-12-19DOI: 10.1134/S1063773725700422
V. V. Bobylev, A. T. Bajkova, A. A. Smirnov
Based on a sample of masers, we have solved the basic kinematic equations with the inclusion of the Galactic rotation parameters and the peculiar solar velocity as the sought-for unknowns. Based on a spectral analysis, we have obtained the following estimates: (|f|_{R,theta}=(7.0,5.1)pm(1.2,1.4)) km s({}^{-1}), the corresponding wavelengths (lambda_{R,theta}=(1.9,1.7)pm(0.4,0.7)) kpc, and (chi_{odot}={-}140^{circ}pm 15^{circ}). We have confirmed the presence of periodic perturbations in the vertical maser velocities with an amplitude (|f|_{W}=3.1pm 1.4) km s({}^{-1}) and a wavelength (lambda=1.9pm 0.8) kpc. We show that the velocity perturbations (f_{R}) and (f_{theta}) can have both the same and opposite signs. Therefore, we have obtained a large spread of estimates. For example, if (f_{R}) and (f_{theta}) have the same signs, then (Omega_{p}=25.8pm 2.0) km s({}^{-1}) kpc({}^{-1}) and (R_{textrm{cor}}=9.1pm 0.8) kpc, while if (f_{R}) and (f_{theta}) have opposite signs, then (Omega_{p}=35.4pm 2.0) km s({}^{-1}) kpc({}^{-1}) and (R_{textrm{cor}}=6.8pm 0.8) kpc.
在一个脉泽样本的基础上，我们求解了包含银河系旋转参数和特殊太阳速度的基本运动学方程，作为寻找的未知数。根据光谱分析，我们得到了以下估计：(|f|_{R,theta}=(7.0,5.1)pm(1.2,1.4)) km s ({}^{-1})，对应的波长(lambda_{R,theta}=(1.9,1.7)pm(0.4,0.7)) kpc和(chi_{odot}={-}140^{circ}pm 15^{circ})。我们已经证实在垂直脉泽速度中存在周期性扰动，其振幅为(|f|_{W}=3.1pm 1.4) km s ({}^{-1})，波长为(lambda=1.9pm 0.8) kpc。我们证明了速度摄动(f_{R})和(f_{theta})可以同时具有相同和相反的符号。因此，我们得到了一个很大的估计范围。例如，(f_{R})和(f_{theta})有相同的符号，则(Omega_{p}=25.8pm 2.0) km为({}^{-1}) kpc ({}^{-1})和(R_{textrm{cor}}=9.1pm 0.8) kpc，而(f_{R})和(f_{theta})有相反的符号，则(Omega_{p}=35.4pm 2.0) km为({}^{-1}) kpc ({}^{-1})和(R_{textrm{cor}}=6.8pm 0.8) kpc。
{"title":"The Spiral Pattern Speed in the Milky Way Galaxy","authors":"V. V. Bobylev, A. T. Bajkova, A. A. Smirnov","doi":"10.1134/S1063773725700422","DOIUrl":"10.1134/S1063773725700422","url":null,"abstract":"<p>Based on a sample of masers, we have solved the basic kinematic equations with the inclusion of the Galactic rotation parameters and the peculiar solar velocity as the sought-for unknowns. Based on a spectral analysis, we have obtained the following estimates: <span>(|f|_{R,theta}=(7.0,5.1)pm(1.2,1.4))</span> km s<span>({}^{-1})</span>, the corresponding wavelengths <span>(lambda_{R,theta}=(1.9,1.7)pm(0.4,0.7))</span> kpc, and <span>(chi_{odot}={-}140^{circ}pm 15^{circ})</span>. We have confirmed the presence of periodic perturbations in the vertical maser velocities with an amplitude <span>(|f|_{W}=3.1pm 1.4)</span> km s<span>({}^{-1})</span> and a wavelength <span>(lambda=1.9pm 0.8)</span> kpc. We show that the velocity perturbations <span>(f_{R})</span> and <span>(f_{theta})</span> can have both the same and opposite signs. Therefore, we have obtained a large spread of estimates. For example, if <span>(f_{R})</span> and <span>(f_{theta})</span> have the same signs, then <span>(Omega_{p}=25.8pm 2.0)</span> km s<span>({}^{-1})</span> kpc<span>({}^{-1})</span> and <span>(R_{textrm{cor}}=9.1pm 0.8)</span> kpc, while if <span>(f_{R})</span> and <span>(f_{theta})</span> have opposite signs, then <span>(Omega_{p}=35.4pm 2.0)</span> km s<span>({}^{-1})</span> kpc<span>({}^{-1})</span> and <span>(R_{textrm{cor}}=6.8pm 0.8)</span> kpc.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":"51 5","pages":"278 - 286"},"PeriodicalIF":0.8,"publicationDate":"2025-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145779209","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 : 2025-12-19DOI: 10.1134/S1063773725700446
M. V. Buntov, N. P. Semena, V. V. Levin, S. V. Molkov, F. A. Voronin, D. M. Gamkov, A. G. Glushenko, E. B. Gurova, O. V. Demin, V. P. Konoshenko, A. V. Krivchenko, V. M. Kuznetsov, M. V. Kuznetsova, I. Yu. Lapshov, V. A. Lipilin, A. A. Lutovinov, A. V. Markov, A. M. Pristash, A. A. Rotin, D. V. Serbinov, D. V. Sibirtsev, D. M. Surin, V. V. Tambov, A. G. Toporkov, A. E. Shtykovskiy, G. A. Kharchenko
We describe the scientific and technological goals of the ‘‘Monitor Vsego Neba’’ (MVN, All-Sky Monitor) space experiment and present its first results. This experiment began to operate onboard the International Space Station (ISS) on December 19, 2024. An analysis of the first results of its observations and the in-orbit operation of the equipment has shown that the basic MVN characteristics correspond to the declared ones in sensitivity, spatial, energy, and time resolution. We have obtained observational data for the brightest sources that can be used for the further calibration of the instrument. We have also determined the particle background of the Earth’s radiation belts and the constraints that are imposed by the enhanced background in the regions of the South Atlantic Anomaly and high latitudes on the observations of celestial sources. We have revealed a problem of the thermal regime of the detectors due to the off-design additional heat flow from the ISS surface that reduces the effective exposure time of observations. The technological goals of the experiment are successfully accomplished. An analysis of the operation of the equipment has shown the validity of the underlying software and hardware solutions. We present the possibility of extending the scientific part of the research with regard to direct X-ray observations of the Sun.
{"title":"MVN Space Experiment: The First Results of Its In-orbit Operation","authors":"M. V. Buntov, N. P. Semena, V. V. Levin, S. V. Molkov, F. A. Voronin, D. M. Gamkov, A. G. Glushenko, E. B. Gurova, O. V. Demin, V. P. Konoshenko, A. V. Krivchenko, V. M. Kuznetsov, M. V. Kuznetsova, I. Yu. Lapshov, V. A. Lipilin, A. A. Lutovinov, A. V. Markov, A. M. Pristash, A. A. Rotin, D. V. Serbinov, D. V. Sibirtsev, D. M. Surin, V. V. Tambov, A. G. Toporkov, A. E. Shtykovskiy, G. A. Kharchenko","doi":"10.1134/S1063773725700446","DOIUrl":"10.1134/S1063773725700446","url":null,"abstract":"<p>We describe the scientific and technological goals of the ‘‘Monitor Vsego Neba’’ (MVN, All-Sky Monitor) space experiment and present its first results. This experiment began to operate onboard the International Space Station (ISS) on December 19, 2024. An analysis of the first results of its observations and the in-orbit operation of the equipment has shown that the basic MVN characteristics correspond to the declared ones in sensitivity, spatial, energy, and time resolution. We have obtained observational data for the brightest sources that can be used for the further calibration of the instrument. We have also determined the particle background of the Earth’s radiation belts and the constraints that are imposed by the enhanced background in the regions of the South Atlantic Anomaly and high latitudes on the observations of celestial sources. We have revealed a problem of the thermal regime of the detectors due to the off-design additional heat flow from the ISS surface that reduces the effective exposure time of observations. The technological goals of the experiment are successfully accomplished. An analysis of the operation of the equipment has shown the validity of the underlying software and hardware solutions. We present the possibility of extending the scientific part of the research with regard to direct X-ray observations of the Sun.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":"51 5","pages":"287 - 309"},"PeriodicalIF":0.8,"publicationDate":"2025-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145779258","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 : 2025-12-19DOI: 10.1134/S1063773725700409
Yu. A. Nagovitsyn, A. I. Larionova, A. A. Osipova
The recurrence times RT (also known as waiting times) of solar flares in active regions in soft X-rays are studied using GOES satellite data from 1998 to 2025. It is shown that the RT distribution is fairly well approximated by a lognormal distribution. Based on grouped samples, changes in three types of average values of log RT distributions over time are studied. From these studies, it can be concluded that the average logarithms of recurrence times, regardless of the method of calculation, show variations similar to variations in sunspot numbers SSN; mean RT values vary between 110 and 280 min.
{"title":"Cyclic Variations in the Mean Recurrence Times of Solar Flares in Active Regions","authors":"Yu. A. Nagovitsyn, A. I. Larionova, A. A. Osipova","doi":"10.1134/S1063773725700409","DOIUrl":"10.1134/S1063773725700409","url":null,"abstract":"<p>The recurrence times <i>RT</i> (also known as waiting times) of solar flares in active regions in soft X-rays are studied using GOES satellite data from 1998 to 2025. It is shown that the <i>RT</i> distribution is fairly well approximated by a lognormal distribution. Based on grouped samples, changes in three types of average values of log <i>RT</i> distributions over time are studied. From these studies, it can be concluded that the average logarithms of recurrence times, regardless of the method of calculation, show variations similar to variations in sunspot numbers <i>SSN</i>; mean <i>RT</i> values vary between 110 and 280 min.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":"51 5","pages":"322 - 326"},"PeriodicalIF":0.8,"publicationDate":"2025-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145779259","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 : 2025-12-19DOI: 10.1021/acsphotonics.5c02204
Seunghwi Kim, Sander A. Mann, Xiang Ni, Andrea Alù
Delay lines are essential components in photonic systems, facilitating data processing, storage, interconnects, and generally enhancing light-matter interactions. They rely on slow light phenomena, which can be realized in integrated photonic platforms such as coupled-resonator optical waveguides, photonic crystals and optical waveguides. In practice, delay lines require robustness, broadband operation and small footprints. Yet, typically, these features need to be traded against each other at the design stage due to constraints stemming from passivity, linearity and time-invariance. Here, we demonstrate that compactness, robustness and bandwidth can be simultaneously achieved by routing light in the synthetic frequency dimension along topological edge states, achieving delay-bandwidth products far beyond conventional limits combined with inherent robustness.
{"title":"Slow Light by Topological Routing in Synthetic Dimensions","authors":"Seunghwi Kim, Sander A. Mann, Xiang Ni, Andrea Alù","doi":"10.1021/acsphotonics.5c02204","DOIUrl":"https://doi.org/10.1021/acsphotonics.5c02204","url":null,"abstract":"Delay lines are essential components in photonic systems, facilitating data processing, storage, interconnects, and generally enhancing light-matter interactions. They rely on slow light phenomena, which can be realized in integrated photonic platforms such as coupled-resonator optical waveguides, photonic crystals and optical waveguides. In practice, delay lines require robustness, broadband operation and small footprints. Yet, typically, these features need to be traded against each other at the design stage due to constraints stemming from passivity, linearity and time-invariance. Here, we demonstrate that compactness, robustness and bandwidth can be simultaneously achieved by routing light in the synthetic frequency dimension along topological edge states, achieving delay-bandwidth products far beyond conventional limits combined with inherent robustness.","PeriodicalId":23,"journal":{"name":"ACS Photonics","volume":"116 1","pages":""},"PeriodicalIF":7.0,"publicationDate":"2025-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145777601","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 : 2025-12-19DOI: 10.1134/S1063773725700458
N. N. Chugai
The origin of the circumstellar (CS) shell of the unusual SN Ia 2020aeuh is explored using a light curve model and observational constraints. The synthesized ({}^{56})Ni mass (({approx}1)(M_{odot})), the mass of the CS shell (0.04–0.2 (M_{odot})), the radius ((2times 10^{16}) cm), and its expansion velocity (({lesssim}200) km s({}^{-1})) have been estimated. The large ({}^{56})Ni mass and the properties of the CS shell are consistent with the scenario of a massive binary C/O white dwarf merger that was accompanied by the loss of ({sim}0.1)(M_{odot}) of matter. The supernova is shown to have exploded ({gtrsim}30) years after the white dwarf merger.
利用光曲线模型和观测约束探讨了不寻常的SN Ia 2020aeuh的星周壳的起源。计算出了合成的({}^{56}) Ni质量（({approx}1)(M_{odot})）、CS壳层质量（0.04-0.2 (M_{odot})）、半径（(2times 10^{16}) cm）和膨胀速度（({lesssim}200) km s ({}^{-1})）。巨大的({}^{56}) Ni质量和CS壳层的性质与巨大的C/O二元白矮星合并的情景一致，伴随着({sim}0.1)(M_{odot})物质的损失。这颗超新星在白矮星合并后({gtrsim}30)年爆炸。
{"title":"SN Ia CSM 2020aeuh: A Massive Binary C/O White Dwarf Merger?","authors":"N. N. Chugai","doi":"10.1134/S1063773725700458","DOIUrl":"10.1134/S1063773725700458","url":null,"abstract":"<p>The origin of the circumstellar (CS) shell of the unusual SN Ia 2020aeuh is explored using a light curve model and observational constraints. The synthesized <span>({}^{56})</span>Ni mass (<span>({approx}1)</span>\u0000 <span>(M_{odot})</span>), the mass of the CS shell (0.04–0.2 <span>(M_{odot})</span>), the radius (<span>(2times 10^{16})</span> cm), and its expansion velocity (<span>({lesssim}200)</span> km s<span>({}^{-1})</span>) have been estimated. The large <span>({}^{56})</span>Ni mass and the properties of the CS shell are consistent with the scenario of a massive binary C/O white dwarf merger that was accompanied by the loss of <span>({sim}0.1)</span>\u0000 <span>(M_{odot})</span> of matter. The supernova is shown to have exploded <span>({gtrsim}30)</span> years after the white dwarf merger.</p>","PeriodicalId":55443,"journal":{"name":"Astronomy Letters-A Journal of Astronomy and Space Astrophysics","volume":"51 5","pages":"257 - 261"},"PeriodicalIF":0.8,"publicationDate":"2025-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145779198","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 : 2025-12-19DOI: 10.1088/2058-9565/ae2b31
Alon Levi, Ziv Ossi, Eliahu Cohen and Amit Te’eni
A hybrid quantum–classical algorithm is a computational scheme in which quantum circuits are used to extract information that is then processed by a classical routine to guide subsequent quantum operations. These algorithms are especially valuable in the noisy intermediate-scale quantum era, where quantum resources are constrained and classical optimization plays a central role. Here, we improve the performance of a hybrid algorithm through principled, information-theoretic optimization. We focus on Quantum Likelihood Estimation (QLE)–-a hybrid algorithm designed to identify the Hamiltonian governing a quantum system by iteratively updating a weight distribution based on measurement outcomes and Bayesian inference. While QLE already achieves convergence using quantum measurements and Bayesian inference, its efficiency can vary greatly depending on the choice of parameters at each step. We propose an optimization strategy that dynamically selects the initial state, measurement basis, and evolution time in each iteration to maximize the mutual information between the measurement outcome and the true Hamiltonian. This approach builds upon the information-theoretic framework recently developed in Te’eni et al (2024 arXiv:2409.15549), and leverages mutual information as a guiding cost function for parameter selection. Our implementation employs a simulated annealing routine to minimize the conditional von Neumann entropy, thereby maximizing information gain in each iteration. The results demonstrate that our optimized version significantly reduces the number of iterations required for convergence, thus proposing a practical method for accelerating Hamiltonian learning in quantum systems. Finally, we propose a general scheme that extends our approach to solve a broader family of quantum learning problems.
{"title":"Optimal quantum likelihood estimation","authors":"Alon Levi, Ziv Ossi, Eliahu Cohen and Amit Te’eni","doi":"10.1088/2058-9565/ae2b31","DOIUrl":"https://doi.org/10.1088/2058-9565/ae2b31","url":null,"abstract":"A hybrid quantum–classical algorithm is a computational scheme in which quantum circuits are used to extract information that is then processed by a classical routine to guide subsequent quantum operations. These algorithms are especially valuable in the noisy intermediate-scale quantum era, where quantum resources are constrained and classical optimization plays a central role. Here, we improve the performance of a hybrid algorithm through principled, information-theoretic optimization. We focus on Quantum Likelihood Estimation (QLE)–-a hybrid algorithm designed to identify the Hamiltonian governing a quantum system by iteratively updating a weight distribution based on measurement outcomes and Bayesian inference. While QLE already achieves convergence using quantum measurements and Bayesian inference, its efficiency can vary greatly depending on the choice of parameters at each step. We propose an optimization strategy that dynamically selects the initial state, measurement basis, and evolution time in each iteration to maximize the mutual information between the measurement outcome and the true Hamiltonian. This approach builds upon the information-theoretic framework recently developed in Te’eni et al (2024 arXiv:2409.15549), and leverages mutual information as a guiding cost function for parameter selection. Our implementation employs a simulated annealing routine to minimize the conditional von Neumann entropy, thereby maximizing information gain in each iteration. The results demonstrate that our optimized version significantly reduces the number of iterations required for convergence, thus proposing a practical method for accelerating Hamiltonian learning in quantum systems. Finally, we propose a general scheme that extends our approach to solve a broader family of quantum learning problems.","PeriodicalId":20821,"journal":{"name":"Quantum Science and Technology","volume":"56 1","pages":""},"PeriodicalIF":6.7,"publicationDate":"2025-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145777639","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 : 2025-12-19DOI: 10.1016/j.physc.2025.1354824
Yi Gao
We studied the superconducting pairing symmetry based on a newly constructed tight-binding model of LaNiO under pressure, where the band sinks below the Fermi level and does not form the Fermi surface. The superconducting pairing symmetry is -wave and is robust against the variation of the interaction strength. In this model, although the and bands are away from the Fermi level, the superconducting pairing function on them is not tiny. Instead, since the top of the band and bottom of the band are both located at 500 meV away from the Fermi level, and they are almost nested by the peak structure in the spin fluctuation, thus by forming an anti-phase pairing function on them, these two bands act constructively to superconductivity. Finally with detailed derivation and numerical calculation, we demonstrate that the Fermi surface approximated Eliashberg equation may lead to deviation of the pairing symmetry.
{"title":"Robust s±-wave pairing in a bilayer two-orbital model of pressurized La3Ni2O7 without the γ Fermi surface","authors":"Yi Gao","doi":"10.1016/j.physc.2025.1354824","DOIUrl":"10.1016/j.physc.2025.1354824","url":null,"abstract":"<div><div>We studied the superconducting pairing symmetry based on a newly constructed tight-binding model of La<span><math><msub><mrow></mrow><mrow><mn>3</mn></mrow></msub></math></span>Ni<span><math><msub><mrow></mrow><mrow><mn>2</mn></mrow></msub></math></span>O<span><math><msub><mrow></mrow><mrow><mn>7</mn></mrow></msub></math></span> under pressure, where the <span><math><mi>γ</mi></math></span> band sinks below the Fermi level and does not form the Fermi surface. The superconducting pairing symmetry is <span><math><msub><mrow><mi>s</mi></mrow><mrow><mo>±</mo></mrow></msub></math></span>-wave and is robust against the variation of the interaction strength. In this model, although the <span><math><mi>γ</mi></math></span> and <span><math><mi>δ</mi></math></span> bands are away from the Fermi level, the superconducting pairing function on them is not tiny. Instead, since the top of the <span><math><mi>γ</mi></math></span> band and bottom of the <span><math><mi>δ</mi></math></span> band are both located at <span><math><mo>∼</mo></math></span>500 meV away from the Fermi level, and they are almost nested by the peak structure in the spin fluctuation, thus by forming an anti-phase pairing function on them, these two bands act constructively to superconductivity. Finally with detailed derivation and numerical calculation, we demonstrate that the Fermi surface approximated Eliashberg equation may lead to deviation of the pairing symmetry.</div></div>","PeriodicalId":20159,"journal":{"name":"Physica C-superconductivity and Its Applications","volume":"640 ","pages":"Article 1354824"},"PeriodicalIF":1.0,"publicationDate":"2025-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145788353","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}
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