检索结果-内蒙古大学图书馆

arXiv 2024年

作者： Li, Shaohong Zheng, Yi Chen, Ziyang Xu, Haojie Yang, Xiaohu School of Physics and Astronomy Sun Yat-sen University 2 Daxue Road Tangjia Zhuhai519082 China CSST Science Center for the Guangdong–Hong Kong–Macau Greater Bay Area SYSU Zhuhai519082 China Department of Astronomy School of Physics and Astronomy Shanghai JiaoTong University Shanghai200240 China Shanghai Key Laboratory for Particle Physics and Cosmology China Shanghai Astronomical Observatory Chinese Academy of Sciences Nandan Road 80 Shanghai200240 China Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai200240 China

We report a ∼ 5.2σ detection of the kinetic Sunyaev–Zel’dovich (kSZ) effect in Fourier space, by combining the DESI galaxy groups and the Planck data. We use the density-weighted pairwise kSZ power spectrum as the summary statistic, and the detailed procedure of its measurement is presented in this paper. Meanwhile, we analyze the redshift space group density power spectrum to constrain its bias parameters and photo-z uncertainties. These best-fitted parameters are substituted to a nonlinear kSZ model, and we fit the measured kSZ power spectrum with this model to constrain the group optical depth τ¯. Selected by a varying lower mass threshold Mth, the galaxy group catalogs with different median masses (M˜) are constructed from the DR9 data of the DESI Legacy Imaging Surveys. M˜ spans a wide range of ∼ 1013 − 1014M☉/h and the heaviest M˜ ∼ 1014M☉/h is larger than those of most other kSZ detections. When the aperture photometric filter radius θAP is set to be 4.2 arcmin, the M˜ = 1.75×1013M☉/h group sample at the median redshift z˜ = 0.64 has the highest kSZ detection S/N = 5.2. By fitting τ¯s from various samples against their M˜s, we obtain a linear log τ¯ − log M˜ relation: log τ¯ = γ(log M˜ −14)+log β, in which γ = 0.55±0.1. We also vary the aperture photometric filter radius and measure the τ¯ profiles of group samples, whose constraints on the baryon distribution within and around dark matter halos will be discussed in a companion paper. © 2024, CC BY-NC-ND.

关键词： Power spectrum

来源：评论

学校读者我要写书评

暂无评论

KPM: A flexible and data-driven K-process model for nucleosynthesis

arXiv

引用

arXiv 2023年

作者： Griffith, Emily J. Hogg, David W. Dalcanton, Julianne J. Hasselquist, Sten Ratcliffe, Bridget Ness, Melissa Weinberg, David H. Center for Astrophysics and Space Astronomy Department of Astrophysical and Planetary Sciences University of Colorado 389 UCB BoulderCO80309-0389 United States Center for Cosmology and Particle Physics Department of Physics New York University 726 Broadway New YorkNY10003 United States Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue New YorkNY10010 United States Department of Astronomy University of Washington Box 351580 SeattleWA98195 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States An der Sternwarte 16 Potsdam14482 Germany Department of Astronomy Columbia University Pupin Physics Laboratories New YorkNY10027 United States The Department of Astronomy Center of Cosmology and AstroParticle Physics The Ohio State University ColumbusOH43210 United States

The element abundance pattern found in Milky Way disk stars is close to two-dimensional, dominated by production from one prompt process and one delayed process. This simplicity is remarkable, since the elements are produced by a multitude of nucleosynthesis mechanisms operating in stars with a wide range of progenitor masses. We fit the abundances of 14 elements for 48,659 red-giant stars from APOGEE DR17 using a flexible, data-driven K-process model—dubbed KPM. In our fiducial model, with K = 2, each abundance in each star is described as the sum of a prompt and a delayed process contribution. We find that KPMwith K = 2 is able to explain the abundances well, recover the observed abundance bimodality, and detect the bimodality over a greater range in metallicity than previously has been possible. We compare to prior work by Weinberg et al. (2022), finding that KPMproduces similar results, but that KPMbetter predicts stellar abundances, especially for elements C+N and Mn and for stars at super-solar metallicities. The model fixes the relative contribution of the prompt and delayed process to two elements to break degeneracies and improve interpretability;we find that some of the nucleosynthetic implications are dependent upon these detailed choices. We find that moving to four processes adds flexibility and improves the model’s ability to predict the stellar abundances, but doesn’t qualitatively change the story. The results of KPMwill help us to interpret and constrain the formation of the Galaxy disk, the relationship between abundances and ages, and the physics of nucleosynthesis. © 2023, CC BY.

关键词： Supernovae

来源：评论

学校读者我要写书评

暂无评论

Dark Matter Halo Parameters from Overheated Exoplanets via Bayesian Hierarchical Inference

arXiv

引用

arXiv 2024年

作者： Benito, María Karchev, Konstantin Leane, Rebecca K. Põder, Sven Smirnov, Juri Trotta, Roberto Tartu Observatory University of Tartu Observatooriumi 1 Tõravere61602 Estonia Theoretical and Scientific Data Science SISSA Trieste Italy SLAC National Accelerator Laboratory Stanford University StanfordCA94039 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94039 United States National Institute of Chemical Physics and Biophysics Rävala 10 Tallinn10143 Estonia Department of Mathematical Sciences University of Liverpool LiverpoolL69 7ZL United Kingdom Imperial College London Physics Department Blackett Laboratory Prince Consort Rd LondonSW7 2AZ United Kingdom Italian Research Center on High Performance Computing Big Data and Quantum Computing & National Institute for Nuclear Physics Sezione di Trieste Italy

Dark Matter (DM) can become captured, deposit annihilation energy, and hence increase the heat flow in exoplanets and brown dwarfs. Detecting such a DM-induced heating in a population of exoplanets in the inner kpc of the Milky Way thus provides potential sensitivity to the galactic DM halo parameters. We develop a Bayesian Hierarchical Model to investigate the feasibility of DM discovery with exoplanets and examine future prospects to recover the spatial distribution of DM in the Milky Way. We reconstruct from mock exoplanet datasets observable parameters such as exoplanet age, temperature, mass, and location, together with DM halo parameters, for representative choices of measurement uncertainty and the number of exoplanets detected. We find that detection of O(100) exoplanets in the inner Galaxy can yield quantitative information on the galactic DM density profile, under the assumption of 10% measurement uncertainty. Even as few as O(10) exoplanets can deliver meaningful sensitivities if the DM density and inner slope are sufficiently large. © 2024, CC BY.

关键词： Hierarchical systems

来源：评论

学校读者我要写书评

暂无评论

Cosmic ray-driven bioenergetics for Life in Molecular Clouds

arXiv

引用

arXiv 2022年

作者： Feng, Lei Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei230026 China Joint Center for Particle Nuclear Physics and Cosmology Nanjing University Purple Mountain Observatory Nanjing210093 China

According to models such as panspermia or the Nebula-Relay hypothesis, the ancestors of life on Earth once lived in molecular clouds. Then what are the energy source and bioenergetics for such lifeforms? In this paper, we propose a new bioenergetic mechanism powered by cosmic ray ionization of hydrogen molecules and we argue that it may relate to or be the origin of chemiosmosis. Based on this mechanism, we suggest that the Last Universal Common Ancestor is a type of lifeform that utilize hydrogen molecules as donors of electron transport chains. Copyright © 2022, The Authors. All rights reserved.

关键词： cosmology

来源：评论

学校读者我要写书评

暂无评论

Simulating emission line galaxies for the next generation of large-scale structure surveys

arXiv

引用

arXiv 2024年

作者： Pei, Wenxiang Guo, Qi Li, Ming Wang, Qiao Han, Jiaxin Hu, Jia Su, Tong Gao, Liang Wang, Jie Luo, Yu Wei, Chengliang Key Laboratory for Computational Astrophysics National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University Beijing102206 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing10049 China Department of Astronomy Shanghai Jiao Tong University Shanghai200240 China Shanghai200240 China Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China School of Physics and Microelectronics Zhengzhou University Zhengzhou450001 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008 China National Basic Science Data Center Zhongguancun South 4th Street Beijing100190 China

We investigate emission line galaxies across cosmic time by combining the modified L-Galaxies semi-analytical galaxy formation model with the JiuTian cosmological simulation. We improve the tidal disruption model of satellite galaxies in L-Galaxies to address the time dependence problem. We utilise the public code CLOUDY to compute emission line ratios for a grid of HII region models. The emission line models assume the same initial mass function as that used to generate the spectral energy distribution of semi-analytical galaxies, ensuring a coherent treatment for modelling the full galaxy spectrum. By incorporating these emission line ratios with galaxy properties, we reproduce observed luminosity functions for Hα, Hβ, [OII], and [OIII] in the local Universe and at high redshifts. We also find good agreement between model predictions and observations for auto-correlation and cross-correlation functions of [OII]-selected galaxies, as well as their luminosity dependence. The bias of emission line galaxies depends on both luminosity and redshift. At lower redshifts, it remains constant with increasing luminosity up to around ∼ 1042.5 erg · s−1 and then rises steeply for higher luminosities. The transition luminosity increases with redshift and becomes insignificant above z=1.5. Generally, galaxy bias shows an increasing trend with redshift. However, for luminous galaxies, the bias is higher at low redshifts, as the strong luminosity dependence observed at low redshifts diminishes at higher redshifts. We provide a fitting formula for the bias of emission line galaxies as a function of luminosity and redshift, which can be utilised for large-scale structure studies with future galaxy surveys. Copyright © 2024, The Authors. All rights reserved.

关键词： Galaxies

来源：评论

学校读者我要写书评

暂无评论

Position reconstruction and surface background model for the PandaX-4T detector

arXiv

引用

arXiv 2025年

作者： Qian, Zhicheng Gu, Linhui Cheng, Chen Bo, Zihao Chen, Wei Chen, Xun Chen, Yunhua Cheng, Zhaokan Cui, Xiangyi Fan, Yingjie Fang, Deqing Gao, Zhixing Geng, Lisheng Giboni, Karl Guo, Xunan Guo, Xuyuan Guo, Zichao Han, Chencheng Han, Ke He, Changda He, Jinrong Huang, Di Huang, Houqi Huang, Junting Hou, Ruquan Hou, Yu Ji, Xiangdong Ji, Xiangpan Ju, Yonglin Li, Chenxiang Li, Jiafu Li, Mingchuan Li, Shuaijie Li, Tao Li, Zhiyuan Lin, Qing Liu, Jianglai Lu, Congcong Lu, Xiaoying Luo, Lingyin Luo, Yunyang Ma, Wenbo Ma, Yugang Mao, Yajun Meng, Yue Ning, Xuyang Pang, Binyu Qi, Ningchun Ren, Xiangxiang Shan, Dong Shang, Xiaofeng Shao, Xiyuan Shen, Guofang Shen, Manbin Sun, Wenliang Tao, Yi Wang, Anqing Wang, Guanbo Wang, Hao Wang, Jiamin Wang, Lei Wang, Meng Wang, Qiuhong Wang, Shaobo Wang, Siguang Wang, Wei Wang, Xiuli Wang, Xu Wang, Zhou Wei, Yuehuan Wu, Weihao Wu, Yuan Xiao, Mengjiao Xiao, Xiang Xiong, Kaizhi Xu, Yifan Yao, Shunyu Yan, Binbin Yan, Xiyu Yang, Yong Ye, Peihua Yu, Chunxu Yuan, Ying Yuan, Zhe Yun, Youhui Zeng, Xinning Zhang, Minzhen Zhang, Peng Zhang, Shibo Zhang, Shu Zhang, Tao Zhang, Wei Zhang, Yang Zhang, Yingxin Zhang, Yuanyuan Zhao, Li Zhou, Jifang Zhou, Jiaxu Zhou, Jiayi Zhou, Ning Zhou, Xiaopeng Zhou, Yubo Zhou, Zhizhen Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China School of Physics Beihang University Beijing102206 China New Cornerstone Science Laboratory Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai201210 China Shanghai Jiao Tong University Sichuan Research Institute Chengdu610213 China Jinping Deep Underground Frontier Science and Dark Matter Key Laboratory of Sichuan Province China Yalong River Hydropower Development Company Ltd. 288 Shuanglin Road Chengdu610051 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Zhuhai519082 China Department of Physics Yantai University Yantai264005 China Institute of Modern Physics Fudan University Shanghai200433 China Huanwu Collaborative Center for Research and Education Beihang University Beijing100191 China International Research Center for Nuclei and Particles in the Cosmos "& Beijing Key Laboratory of Advanced Nuclear Materials and Physics Beihang University Beijing100191 China Institute of Modern Physics Chinese Academy of Sciences Huizhou516000 China SJTU Paris Elite Institute of Technology Shanghai Jiao Tong University Shanghai200240 China School of Mechanical Engineering Shanghai Jiao Tong University Shanghai200240 China Department of Physics University of Maryland College ParkMD20742 United States School of Physics Nankai University Tianjin300071 China School of Physics Sun Yat-Sen University Guangzhou510275 China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei230026 China Department of Modern Physics University of Science and Technology of China Hefei230026 China Research Center for Particle Science and Technology Institute of Frontier and Interdisciplinary Science Shandong University Qingdao266237 China Key Laboratory of Particle Physics and Particle Irradiation of Ministry of Education Shandong University Qingdao266237 China School of Physics Peking University Beiji

We report the position reconstruction methods and surface background model for the PandaX-4T dark matter direct search experiment. This work develops two position reconstruction algorithms: template matching (TM) method and photon acceptance function (PAF) method. Both methods determine the horizontal position of events based on the light pattern of secondary scintillation collected by the light sensors. After a comprehensive evaluation of resolution, uniformity, and robustness, the PAF method was selected for position reconstruction, while the TM method was employed for verification. The PAF method achieves a bulk event resolution of 1.0 mm and a surface event resolution of 4.4 mm for a typical S2 signal with a bottom charge of 1500 PE (about 14 keV). The uniformity is around 20%. Robustness studies reveal average deviations of 5.1 mm and 8.8 mm for the commissioning run (Run0) and the first science run (Run1), respectively, due to the deactivation of certain PMTs. A data-driven surface background model is developed based on the PAF method. The surface background is estimated to be 0.09 ± 0.06 events for Run0 (0.54 tonne·year) and 0.17 ± 0.11 events for Run1 (1.00 tonne·year). © 2025, CC BY.

关键词： Template matching

来源：评论

学校读者我要写书评

暂无评论

Quark Transverse Spin-Momentum Correlation of the Nucleon from Lattice QCD: The Boer-Mulders Function

arXiv

引用

arXiv 2025年

作者： Ma, Lingquan Hua, Jun Schäfer, Andreas Shu, Hai-Tao Su, Yushan Sun, Peng Walter, Lisa Wang, Wei Xiong, Xiaonu Yang, Yi-Bo Zhang, Jian-Hui Zhang, Qi-An Center of Advanced Quantum Studies Department of Physics Beijing Normal University Beijing100875 China School of Science and Engineering The Chinese University of Hong Kong Shenzhen518172 China Guangdong Basic Research Center of Excellence for Structure and Fundamental Interactions of Matter Institute of Quantum Matter South China Normal University Guangzhou510006 China Guangdong-Hong Kong Joint Laboratory of Quantum Matter Guangdong Provincial Key Laboratory of Nuclear Science Southern Nuclear Science Computing Center South China Normal University Guangzhou510006 China Institut für Theoretische Physik Universität Regensburg RegensburgD-93040 Germany Institute of Particle Physics Central China Normal University Wuhan430079 China Department of Physics University of Maryland College ParkMD20742 United States Institute of Modern Physics Chinese Academy of Sciences Gansu Province Lanzhou730000 China Shanghai Key Laboratory for Particle Physics and Cosmology School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Institute of Modern Physics Chinese Academy of Sciences Guangdong Province Huizhou516000 China School of Physics Central South University Changsha418003 China CAS Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences Beijing100190 China School of Fundamental Physics and Mathematical Sciences Hangzhou Institute for Advanced Study UCAS Hangzhou310024 China International Centre for Theoretical Physics Asia-Pacific Hangzhou Beijing China University of Chinese Academy of Sciences School of Physical Sciences Beijing100049 China School of Physics Beihang University Beijing102206 China

We present the first lattice QCD calculation of the quark transverse spin-momentum correlation, i.e., the naive time-reversal-odd Boer-Mulders function, of the nucleon, using large-momentum effective theory (LaMET). The calculation is carried out on an ensemble with lattice spacing a = 0.098 fm and pion mass 338 MeV, at various proton momenta up to 2.11 GeV. We have implemented perturbative matching up to the next-to-next-to-leading order together with a renormalization-group resummation improvement. The result exhibits a decay behavior with increasing transverse separation b̝. We also compare the results in the nucleon and pion. Copyright © 2025, The Authors. All rights reserved.

关键词： Momentum

来源：评论

学校读者我要写书评

暂无评论

Dark matter direct detection with quantum dots

引用

Physical Review D 2023年第9期107卷 095035-095035页

作者： Carlos Blanco Rouven Essig Marivi Fernandez-Serra Harikrishnan Ramani Oren Slone Department of Physics Princeton University Princeton New Jersey 08544 USA Stockholm University and The Oskar Klein Centre for Cosmoparticle Physics Alba Nova 10691 Stockholm Sweden C. N. Yang Institute for Theoretical Physics Stony Brook University Stony Brook New York 11794 USA Department of Physics and Astronomy Stony Brook University Stony Brook New York 11794-3800 USA Institute for Advanced Computational Science Stony Brook University Stony Brook New York 11794-3800 USA Stanford Institute for Theoretical Physics Department of Physics Stanford University Stanford California 94305 USA Center for Cosmology and Particle Physics Department of Physics New York University New York New York 10003 USA

We propose using quantum dots as novel targets to probe sub-GeV dark matter-electron interactions. Quantum dots are nanocrystals of semiconducting material, which are commercially available, with gram-scale quantities suspended in liter-scale volumes of solvent. Quantum dots can be efficient scintillators, with near unity single-photon quantum yields, and their band-edge electronic properties are determined by their characteristic size, which can be precisely tuned. Examples include lead sulfide and lead selenide quantum dots, which can be tuned to have sub-eV optical gaps. A dark-matter interaction can generate one or more electron-hole pairs (excitons), with the multiexciton state decaying via the emission of two photons with an efficiency of about 10% of the single-photon quantum yield. An experimental setup using commercially available quantum dots and two photomultiplier-tubes for detecting the coincident two-photon signal can already improve on existing dark-matter bounds, while using photodetectors with lower dark-count rates can improve on current constraints by orders of magnitude.

关键词： Dark matter particle dark matter Quantum dots Dark matter detectors

来源：评论

学校读者我要写书评

暂无评论

Alternating current conductivity and superconducting properties of the holographic effective theory

arXiv

引用

arXiv 2022年

作者： Liu, Yan Wang, Xi-Jing Wu, Jian-Pin Zhang, Xin Department of Physics College of Sciences Northeastern University Shenyang110819 China Center for Gravitation and Cosmology College of Physical Science and Technology Yangzhou University Yangzhou225009 China Frontiers Science Center for Industrial Intelligence and Systems Optimization Northeastern University Shenyang110819 China Key Laboratory of Data Analytics and Optimization for Smart Industry Ministry of Education Northeastern University Shenyang110819 China

We construct a holographic effective superconducting theory by considering a special gauge-axion higher derivative term. The gauge-axion coupling results in the transport behavior similar to the vortex response in the dual boundary field theory leading to non-Drude behavior of alternating current (AC) conductivity at the weak momentum dissipation. With the momentum dissipation increasing, a dip exhibits in the AC conductivity at low frequency. It is thought to be the result of a combination of the strong momentum dissipation and the gauge-axion coupling. In the superconducting phase, this gauge-axion coupling also plays a key role leading to a more evident gap at the low frequency conductivity. In addition, we also study the combined effects of the strength of momentum dissipation and various couplings among the gauge field, axion fields and the complex scalar field. Copyright © 2022, The Authors. All rights reserved.

关键词： Momentum

来源：评论

学校读者我要写书评

暂无评论

Search for Double Beta Decay of 136Xe to the 0+1 Excited State of 136Ba with PandaX-4T

arXiv

引用

arXiv 2025年

作者： Luo, Lingyin Bo, Zihao Chen, Wei Chen, Xun Chen, Yunhua Cheng, Zhaokan Cui, Xiangyi Fan, Yingjie Fang, Deqing Gao, Zhixing Geng, Lisheng Giboni, Karl Guo, Xunan Guo, Xuyuan Guo, Zichao Han, Chencheng Han, Ke He, Changda He, Jinrong Huang, Di Huang, Houqi Huang, Junting Hou, Ruquan Hou, Yu Ji, Xiangdong Ji, Xiangpan Ju, Yonglin Li, Chenxiang Li, Tao Li, Jiafu Li, Mingchuan Li, Shuaijie Li, Zhiyuan Lin, Qing Liu, Jianglai Lu, Congcong Lu, Xiaoying Luo, Yunyang Ma, Wenbo Ma, Yugang Mao, Yajun Meng, Yue Ning, Xuyang Pang, Binyu Qi, Ningchun Qian, Zhicheng Ren, Xiangxiang Shan, Dong Shang, Xiaofeng Shao, Xiyuan Shen, Guofang Shen, Manbin Sun, Wenliang Tao, Yi Wang, Anqing Wang, Guanbo Wang, Hao Wang, Jiamin Wang, Lei Wang, Meng Wang, Qiuhong Wang, Shaobo Wang, Siguang Wang, Wei Wang, Xiuli Wang, Xu Wang, Zhou Wei, Yuehuan Wu, Weihao Wu, Yuan Xiao, Mengjiao Xiao, Xiang Xiong, Kaizhi Xu, Yifan Yao, Shunyu Yan, Binbin Yan, Xiyu Yang, Yong Ye, Peihua Yu, Chunxu Yuan, Ying Yuan, Zhe Yun, Youhui Zeng, Xinning Zhang, Minzhen Zhang, Peng Zhang, Shibo Zhang, Shu Zhang, Tao Zhang, Wei Zhang, Yang Zhang, Yingxin Zhang, Yuanyuan Zhao, Li Zhou, Jifang Zhou, Jiaxu Zhou, Ning Zhou, Xiaopeng Zhou, Yubo Zhou, Zhizhen New Cornerstone Science Laboratory Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai201210 China State Key Laboratory of Nuclear Physics and Technology School of Physics Peking University Beijing100871 China Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China Jinping Deep Underground Frontier Science and Dark Matter Key Laboratory of Sichuan Province China Yalong River Hydropower Development Company Ltd. 288 Shuanglin Road Chengdu610051 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Zhuhai519082 China Department of Physics Yantai University Yantai264005 China Institute of Modern Physics Fudan University Shanghai200433 China School of Physics Beihang University Beijing102206 China Peng Huanwu Collaborative Center for Research and Education Beihang University Beijing100191 China International Research Center for Nuclei and Particles in the Cosmos Beijing Key Laboratory of Advanced Nuclear Materials and Physics Beihang University Beijing100191 China Institute of Modern Physics Chinese Academy of Sciences Huizhou516000 China SJTU Paris Elite Institute of Technology Shanghai Jiao Tong University Shanghai200240 China Shanghai Jiao Tong University Sichuan Research Institute Chengdu610213 China School of Mechanical Engineering Shanghai Jiao Tong University Shanghai200240 China Department of Physics University of Maryland College ParkMD20742 United States School of Physics Nankai University Tianjin300071 China School of Physics Sun Yat-Sen University Guangzhou510275 China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei230026 China Department of Modern Physics University of Science and Technology of China Hefei230026 China Research Center for Particle Science and Technology Institute of Frontier and Interdisciplinary Science Shandong University Shandong Qingdao266237 China Key Laboratory o

We perform a search of double beta decay of 136Xe to the excited state, 0+1 , of 136Ba (2νββ-0+1 ), using the dual-phase xenon detector of PandaX-4T with the first 94.9-day commissioning data. The multi-site events are reconstructed up to the MeV energy scale, which helps to improve the background model significantly. The background contribution from the stainless steel platform outside PandaX-4T cryostat is evaluated for the first time. No significant evidence for 2νββ-0+1 is observed, resulting in a lower limit on half-life of 7.5×1022 yr at the 90% confidence level. This is the first experimental limit on such a rare decay in a natural xenon-based detector. © 2025, CC BY.

关键词：

来源：评论

学校读者我要写书评

暂无评论

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案：

请选择收藏分类：

通借通还

建议与咨询 留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案： 新增检索档案 确定 取消

请选择收藏分类： 新增自定义分类 确定 取消

通借通还

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

请选择保存的检索档案：

请选择收藏分类：