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Forecasting the constraints on optical selection bias and projection effects of galaxy cluster lensing with multiwavelength data

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Physical Review D 2024年第10期110卷 103508页

作者： Conghao Zhou Hao-Yi Wu Andrés N. Salcedo Sebastian Grandis Tesla Jeltema Alexie Leauthaud Matteo Costanzi Tomomi Sunayama David H. Weinberg Tianyu Zhang Eduardo Rozo Chun-Hao To Sebastian Bocquet Tamas Varga Matthew Kwiecien Physics Department Department of Physics Steward Observatory Institut für Astro- und Teilchenphysik Technikerstr. 25/8 6020 Innsbruck Austria Department of Astronomy and Astrophysics Dipartimento di Fisica—Sezione di Astronomia Center for Cosmology and AstroParticle Physics (CCAPP) Department of Statistics and Data Science University Observatory Faculty of Physics Gießenbachstrasse 1 85748 Garching German Excellence Cluster Origins Boltzmannstrasse 2 85748 Garching Germany and Universitäts-Sternwarte Fakultät für Physik Ludwig-Maximilians Universität München Scheinerstrasse 1 81679 München Germany

Galaxy clusters identified with optical imaging tend to suffer from projection effects, which impact richness (the number of member galaxies in a cluster) and lensing coherently. Physically unassociated galaxies can be mistaken as cluster members due to the significant uncertainties in their line-of-sight distances, thereby changing the observed cluster richness; at the same time, projection effects alter the weak gravitational lensing signals of clusters, leading to a correlated scatter between richness and lensing at a given halo mass. As a result, the lensing signals for optically selected clusters tend to be biased high. This optical selection bias problem of cluster lensing is one of the key challenges in cluster cosmology. Fortunately, recently available multiwavelength observations of clusters provide a solution. We analyze a simulated dataset mimicking the observed lensing of clusters identified by both optical photometry and gas properties, aiming to constrain this selection bias. Assuming a redMaPPer sample from the Dark Energy Survey with South Pole Telescope Sunyaev-Zeldovich effect observations, we find that an overlapping survey of 1300 deg2, 0.2cosmology analyses.

关键词： Cosmological parameters Gravitational lenses Large scale structure of the Universe Sky surveys Galaxy clusters Monte Carlo methods

Cosmological search for sterile neutrinos after DESI 2024

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arXiv 2025年

作者： Du, Guo-Hong Li, Tian-Nuo Wu, Peng-Ju Feng, Lu Zhou, Sheng-Han Zhang, Jing-Fei Zhang, Xin Liaoning Key Laboratory of Cosmology and Astrophysics College of Sciences Northeastern University Shenyang110819 China School of Physics Ningxia University Yinchuan750021 China College of Physical Science and Technology Shenyang Normal University Shenyang110034 China MOE Key Laboratory of Data Analytics and Optimization for Smart Industry Northeastern University Shenyang110819 China National Frontiers Science Center for Industrial Intelligence and Systems Optimization Northeastern University Shenyang110819 China

The question of whether the massive sterile neutrinos exist remains a crucial unresolved issue in both particle physics and cosmology. We explore the cosmological constraints on the massive sterile neutrinos using the latest observational data, including the baryon acoustic oscillations data from DESI, the cosmic microwave background data from Planck satellite and ACT, and the 5-year Type Ia supernova data and the 3-year weak-lensing data from DES. We search for the massive sterile neutrinos within the ΛCDM, wCDM, and w0waCDM models. Our analysis shows that when considering massive sterile neutrinos within the w0waCDM model, the combined datasets allow us to infer a non-zero sterile neutrino mass at approximately 2σ confidence level. Specifically, in the w0waCDM+Sterile model, the effective mass of sterile neutrinos and the effective number of relativistic species are constrained to be meffν,sterile = 0.50+0.33−0.27 eV and Neff = 3.076+0.011−0.017, respectively. However, the ΛCDM+Sterile and wCDM+Sterile models could not provide evidence supporting the existence of massive sterile neutrinos. Copyright © 2025, The Authors. All rights reserved.

关键词： cosmology

Erratum to: One-loop matching for quark dipole operators in a gradient-flow scheme

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Journal of High Energy physics 2025年第3期2025卷 1-5页

作者： Mereghetti, Emanuele Monahan, Christopher J. Rizik, Matthew D. Shindler, Andrea Stoffer, Peter Theoretical Division Los Alamos National Laboratory Los Alamos USA Department of Physics The College of William & Mary Williamsburg USA Theory Center Thomas Jefferson National Accelerator Facility Newport News USA Department of Physics Colorado College Colorado Springs USA Facility for Rare Isotope Beams & Physics Department Michigan State University East Lansing USA Institute for Theoretical Particle Physics and Cosmology TTK RWTH Aachen University Aachen Germany Nuclear Science Division Lawrence Berkeley National Laboratory Berkeley USA Physik-Institut Universität Zürich Zürich Switzerland Paul Scherrer Institut Villigen Switzerland Faculty of Physics University of Vienna Vienna Austria

Determination of the cross section from 10 to 200 keV at the Back-n facility at CSNS

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The European Physical Journal A 2023年第10期59卷 1-11页

作者： Wang, Jincheng Ren, Jie Jiang, Wei Ruan, Xichao Sun, Qi Hu, Jifeng Jiang, Bing Bao, Jie Zhang, Qiwei Luan, Guangyuan Huang, Hanxiong Nie, Yangbo Ge, Zhigang An, Qi Bai, Haofan Bai, Jiangbo Cao, Ping Chen, Qiping Chen, Yonghao Chen, Zhen Cui, Zengqi Fan, Anchuan Fan, Ruirui Feng, Changqing Feng, Fanzhen Gao, Keqing Gu, Minhao Han, Changcai Han, Zijie He, Guozhu He, Yongcheng Hong, Yang Hu, Yiwei Jia, Weihua Jiang, Haoyu Jiang, Zhijie Jin, Zhengyao Kang, Ling Li, Bo Li, Chao Li, Gong Li, Jiawen Li, Qiang Li, Yang Liu, Jie Liu, Rong Liu, Shubin Ning, Changjun Qi, Binbin Ren, Zhizhou Song, Zhaohui Sun, Kang Tan, Zhixin Tang, Jingyu Tang, Shengda Wang, Lijiao Wang, Pengcheng Wang, Zhaohui Wen, Zhongwei Wu, Xiaoguang Wu, Xuan Xie, Likun Yang, Yiwei Yi, Han Yu, Yongji Zhang, Guohui Zhang, Linhao Zhang, Mohan Zhang, Xianpeng Zhang, Yuliang Zhang, Yue Zhang, Zhiyong Zhao, Maoyuan Zhou, Luping Zhu, Kejun Zhang, Jie Key Laboratory of Nuclear Data China Institute of Atomic Energy Beijing China Institute of High Energy Physics Chinese Academy of Sciences (CAS) Beijing China Spallation Neutron Source Science Center Dongguan China Shanghai Institute of Applied Physics Chinese Academy of Sciences Shanghai China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei China Department of Modern Physics University of Science and Technology of China Hefei China State Key Laboratory of Nuclear Physics and Technology School of Physics Peking University Beijing China Institute of Nuclear Physics and Chemistry China Academy of Engineering Physics Mianyang China School of Nuclear Science and Technology University of Science and Technology of China Hefei China USTC Archaeometry Lab University of Science and Technology of China Hefei China State Key Laboratory of Particle Detection and Electronics Institute of High Energy Physics Chinese Academy of Sciences Beijing China Northwest Institute of Nuclear Technology Xi’an China University of Chinese Academy of Sciences Beijing China

The neutron capture cross section of $$^{232}Th$$ has been measured with the time-of-flight technique in the energy range from 10 to 200 keV at the back-streaming white neutron beam-line (Back-n) of China Spallation Neutron Source (CSNS). The pulse height weighting technique (PHWT) was applied with four C $$_{6}$$ D $$_{6}$$ liquid scintillators to measure the prompt gamma-ray energy release following neutron capture. The measurement data, corrected with the PHWT, have been normalized to the saturated resonances at 21.8 eV. The background was determined by a lead sample measurement and detailed Monte Carlo simulations. The $$^{232}Th(n,\gamma )$$ average cross sections have been determined relative to the $$^{197}Au(n,\gamma )$$ reaction cross sections. The results are consistent with the evaluation values of CENDL-3.2 and JENDL-5. The total uncertainties, including the PHWT, normalization, background subtraction, corrections, and relative measurement, are in the range of 4.5–4.8%.

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Tracing the imprints of large-scale magnetized structure on γ rays from GRB 221009A

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arXiv 2025年

作者： Das, Saikat Razzaque, Soebur Mirabal, Nestor Omodei, Nicola Murase, Kohta Martinez-Castellanos, Israel Center for Gravitational Physics and Quantum Information Yukawa Institute for Theoretical Physics Kyoto University Kyoto606-8502 Japan Department of Physics University of Florida GainesvilleFL32611 United States Department of Physics University of Johannesburg PO Box 524 Auckland Park2006 South Africa Department of Physics The George Washington University WashingtonDC20052 United States Private Bag X1 Matieland South Africa Center for Space Sciences and Technology University of Maryland Baltimore County BaltimoreMD21250 United States Astroparticle Physics Laboratory NASA Goddard Space Flight Center Mail Code 661 GreenbeltMD20771 United States Center for Research and Exploration in Space Science and Technology NASA Goddard Space Flight Center GreenbeltMD20771 United States W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States Department of Physics Department of Astronomy & Astrophysics Center for Multimessenger Astrophysics Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Dept. of Physics University of Maryland College ParkMD20742 United States

We search for possible GeV-TeV gamma-ray imprints of ultrahigh-energy (UHE;0.1 EeV) cosmic ray (CR) acceleration in the large-scale structures surrounding the brightest gamma-ray burst (GRB) explosion, GRB 221009A. Using 1.25 years of post-event Fermi Large Area Telescope (LAT) data, we construct a 1 GeV – 1 TeV test-statistic (TS) map within 15 Mpc of the burst. We identify two peaks in the TS map with TS ≥ 9. The most significant peak, J1911.8+2044, exhibits gamma-ray emission in pre-burst LAT data. The other peak, J1913.2+1901, coincides with a 664.6 GeV photon recorded ∼ 191.9 days after the GRB trigger and located at about 0.75◦ from the GRB localization. The per-photon 95% containment angle for the LAT is about 0.25◦ in the 100 GeV – 1 TeV energy range. We explore two possible origins for the γ-ray emission: (1) UHECRs from GRB 221009A propagating through a magnetized cosmological volume in its vicinity, and (2) UHE or very-high-energy (VHE;100 GeV) γ-ray emission from GRB 221009A, propagating in the same volume. In both cases, electromagnetic cascade emission is induced in the structured region embedding the burst. If any TS features are related to large-scale imprints induced by cosmic rays, it might be further evidence that GRB 221009A accelerated UHECRs. However, our results show that alternative scenarios without invoking UHECRs cannot be ruled out, and the observed high-energy photon could be unrelated to GRB 221009A. Copyright © 2025, The Authors. All rights reserved.

关键词： Gamma radiography

How well do we know the primordial black hole abundance: The crucial role of nonlinearities when approaching the horizon

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Physical Review D 2023年第6期108卷 063531-063531页

作者： Valerio De Luca Alex Kehagias Antonio Riotto Center for Particle Cosmology Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street Philadelphia Pennsylvania 19104 USA Physics Division National Technical University of Athens 15780 Zografou Campus Athens Greece CERN Theoretical Physics Department Geneva 1211 Switzerland Département de Physique Théorique and Gravitational Wave Science Center (GWSC) Université de Genève CH-1211 Geneva Switzerland

We discuss the nonlinear corrections entering in the calculation of the primordial black hole abundance from the nonlinear radiation transfer function and the determination of the true physical horizon crossing. We show that the current standard techniques to calculate the abundance of primordial black holes suffer from uncertainties and argue that the primordial black hole abundance may be much smaller than what routinely considered. This would imply, among other consequences, that the interpretation of the recent pulsar timing arrays data from scalar-induced gravitational waves may not be ruled out because of an overproduction of primordial black holes.

关键词： Classical black holes Inflation

Measurement of the cosmic ray proton spectrum around the knee region with LHAASO 38

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Measurement of the cosmic ray proton spectrum around the kne...

38th International Cosmic Ray Conference, ICRC 2023

作者： Zhiyong, You Shoushan, Zhang Liqiao, Yin Lingling, Ma Zhen, Cao Yudong, Wang Cao, Zhen Aharonian, F. An, Q. Axikegu Bai, L.X. Bai, Y.X. Bai, L.X. Bai, Y.X. Bao, Y.W. Bastieri, D. Bi, X.J. Bi, Y.J. Cai, H. Cai, J.T. Cao, Zhe Chang, J. Chang, J.F. Chen, B.M. Chen, E.S. Chen, J. Chen, Liang Chen, Liang Chen, Long Chen, M.J. Chen, M.L. Chen, Q.H. Chen, S.H. Chen, S.Z. Chen, T.L. Chen, X.L. Chen, Y. Cheng, N. Cheng, Y.D. Cui, S.W. Cui, X.H. Cui, Y.D. D’Ettorre Piazzoli, B. Dai, B.Z. Dai, H.L. Dai, Z.G. Danzengluobu della Volpe, D. Dong, X.J. Duan, K.K. Fan, J.H. Fan, Y.Z. Fan, Z.X. Fang, J. Fang, K. Feng, C.F. Feng, L. Feng, S.H. Feng, Y.L. Gao, B. Gao, C.D. Gao, L.Q. Gao, Q. Gao, W. Ge, M.M. Geng, L.S. Gong, G.H. Gou, Q.B. Gu, M.H. Guo, F.L. Guo, J.G. Guo, X.L. Guo, Y.Q. Guo, Y.Y. Han, Y.A. He, H.H. He, H.N. He, J.C. He, S.L. He, X.B. He, Y. Heller, M. Hor, Y.K. Hou, C. Hu, H.B. Hu, S. Hu, S.C. Hu, X.J. Huang, D.H. Huang, Q.L. Huang, W.H. Huang, X.T. Huang, X.Y. Huang, Z.C. Ji, F. Ji, X.L. Jia, H.Y. Jiang, K. Jiang, Z.J. Jin, C. Ke, T. Kuleshov, D. Levochkin, K. Li, B.B. Li, Cheng Li, Cong Li, F. Li, H.B. Li, H.C. Li, H.Y. Li, J. Li, K. Li, W.L. Li, X.R. Li, Xin Li, Xin Li, Y. Li, Y.Z. Li, Zhe Li, Zhuo Liang, E.W. Liang, Y.F. Lin, S.J. Liu, B. Liu, C. Liu, D. Liu, H. Liu, H.D. Liu, J. Liu, J.L. Liu, J.S. Liu, J.Y. Liu, M.Y. Liu, R.Y. Liu, S.M. Liu, W. Liu, Y. Liu, Y.N. Liu, Z.X. Long, W.J. Lu, R. Lv, H.K. Ma, B.Q. Ma, L.L. Ma, X.H. Mao, J.R. Masood, A. Min, Z. Mitthumsiri, W. Montaruli, T. Nan, Y.C. Pang, B.Y. Pattarakijwanich, P. Pei, Z.Y. Qi, M.Y. Qi, Y.Q. Qiao, B.Q. Qin, J.J. Ruffolo, D. Rulev, V. Sáiz, A. Shao, L. Shchegolev, O. Sheng, X.D. Shi, J.Y. Song, H.C. Stenkin, Yu.V. Stepanov, V. Su, Y. Sun, Q.N. The Institute of High Energy Physics The Chinese Academy of Sciences YuQuan Road.19B shijingshan district Beijing China University of Chinese Academy of Sciences Department YuQuan Road.19A shijingshan district Beijing100049 China TIANFU Cosmic Ray Research Center Sichuan Chengdu China Key Laboratory of Particle Astrophyics & Experimental Physics Division & Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Dublin Institute for Advanced Studies 31 Fitzwilliam Place Dublin 2 Ireland Max-Planck-Institut for Nuclear Physics P.O. Box 103980 Heidelberg69029 Germany State Key Laboratory of Particle Detection and Electronics China University of Science and Technology of China Anhui Hefei230026 China School of Physical Science and Technology School of Information Science and Technology Southwest Jiaotong University Sichuan Chengdu610031 China College of Physics Sichuan University Sichuan Chengdu610065 China School of Astronomy and Space Science Nanjing University Jiangsu Nanjing210023 China Center for Astrophysics Guangzhou University Guangdong Guangzhou510006 China School of Physics and Technology Wuhan University Hubei Wuhan430072 China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Jiangsu Nanjing210023 China Hebei Normal University Hebei Shijiazhuang050024 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Ministry of Education Tibet Lhasa850000 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Sun Yat-sen University Guangdong Zhuhai519000 China Dipartimento di Fisica dell’Università di Napoli ‘Federico II" Complesso Universitario di Monte Sant’Angelo via Cinthia Napoli80126 Italy School of Physics and Astronomy Yunnan University Yunnan Kunming650091 China Departement de Physique Nucleair

One of the main scientific aims of LHAASO is to measure the energy spectra of cosmic rays for individual mass compositions. LHAASO is made up of three detector arrays, which are WFCTA, KM2A, and WCDA. The three detector arrays can achieve hybrid observation, so several extensive air shower observables that are sensitive to mass compositions can be measured simultaneously. ROOT-TMVA package is used to combine these component-sensitive parameters for selecting proton events. The selected proton events have a purity of over 90%. In this paper, we have selected simulated events with shower cores located in the KM2A array to investigate the feasibility of the analysis method for studying the proton energy spectrum. We have also studied the associated systematic uncertainties, including those introduced by the composition models, proton selection, energy reconstruction method, and hadronic interaction models. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Cosmic rays

On the effects of parameters on galaxy properties in CAMELS and the predictability of Ωm

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arXiv 2025年

作者： Contardo, Gabriella Trotta, Roberto Gioia, Serafina Di Hogg, David W. Villaescusa-Navarro, Francisco Center for Astrophysics and Cosmology University of Nova Gorica Ajdovščina Slovenia Trieste Italy ICSC - Centro Nazionale di Ricerca in High Performance Computing Big Data e Quantum Computing Via Magnanelli 2 Bologna Italy Astrophysics Group Physics Department Blackett Lab Imperial College London Prince Consort Road LondonSW7 2AZ United Kingdom INAF – Osservatorio Astronomico di Trieste Via G. B. Tiepolo 11 TriesteI-34143 Italy Trieste Italy Center for Cosmology and Particle Physics Department of Physics New York University New YorkNY United States Max-Planck-Institut für Astronomie Heidelberg Germany Center for Computational Astrophysics Flatiron Institute New YorkNY United States Department of Astrophysical Sciences Peyton Hall Princeton University NJ08544-0010 United States

Recent analyses of cosmological hydrodynamic simulations from CAMELS have shown that machine learning models can predict the parameter describing the total matter content of the universe, Ωm, from the features of a single galaxy. We investigate the statistical properties of two of these simulation suites, IllustrisTNG and ASTRID, confirming that Ωm induces a strong displacement on the distribution of galaxy features. We also observe that most other parameters have little to no effect on the distribution, except for the stellar-feedback parameter ASN1, which introduces some near-degeneracies that can be broken with specific features. These two properties explain the predictability of Ωm. We use Optimal Transport to further measure the effect of parameters on the distribution of galaxy properties, which is found to be consistent with physical expectations. However, we observe discrepancies between the two simulation suites, both in the effect of Ωm on the galaxy properties and in the distributions themselves at identical parameter values. Thus, although Ωm’s signature can be easily detected within a given simulation suite using just a single galaxy, applying this result to real observational data may prove significantly more challenging. © 2025, CC BY.

关键词： Galaxies

Phase-resolved Spectroscopy of Low-frequency Quasi-periodic Oscillations from the Newly Discovered Black Hole X-ray Binary Swift J1727.8–1613

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arXiv 2024年

作者： Shui, Qing-Cang Zhang, Shu Peng, Jing-Qiang Zhang, Shuang-Nan Chen, Yu-Peng Ji, Long Kong, Ling-Da Feng, Hua Yu, Zhuo-Li Wang, Peng-Ju Chang, Zhi Yin, Hong-Xing Qu, Jin-Lu Tao, Lian Ge, Ming-Yu Zhang, Liang Li, Jian Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China University of Chinese Academy of Sciences Chinese Academy of Sciences Beijing100049 China School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 China Institut für Astronomie und Astrophysik Kepler Center for Astro and Particle Physics Eberhard Karls Universität Sand 1 TübingenD-72076 Germany Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment School of Space Science and Physics Institute of Space Sciences Shandong University Shandong Weihai264209 China CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China

Low-frequency quasi-periodic oscillations (LFQPOs) are commonly observed in X-ray light curves of black hole X-ray binaries (BHXRBs);however, their origin remains a topic of debate. In order to thoroughly investigate variations in spectral properties on the QPO timescale, we utilized the Hilbert-Huang transform technique to conduct phase-resolved spectroscopy across a broad energy band for LFQPOs in the newly discovered BHXRB Swift J1727.8–1613. This is achieved through quasi-simultaneous observations from Neutron star Interior Composition ExploreR (NICER), Nuclear Spectroscopic Telescope ARray (NuSTAR), and Hard X-ray Modulation Telescope (Insight-HXMT). Our analysis reveals that both the non-thermal and disk-blackbody components exhibit variations on the QPO timescale, with the former dominating the QPO variability. For the spectral parameters, we observe modulation of the disk temperature, spectral indices, and reflection fraction with the QPO phase with high statistical significance ( 5σ). Notably, the variation in the disk temperature is found to precede the variations in the non-thermal and disk fluxes by ∼ 0.4 − 0.5 QPO cycles. We suggest that these findings offer further evidence that the type-C QPO variability is a result of geometric effects of the accretion flow. © 2024, CC BY.

关键词： Hilbert-Huang transform