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Anisotropic evolution of 4-brane in a 6D generalized Randall-Sundrum model

Chinese physics C 2019年第9期43卷 101-107页

作者： Guang-Zhen Kang De-Sheng Zhang Long Du Jun Xu Hong-Shi Zong School of Science Yangzhou Polytechnic InstituteYangzhou 225127China Department of Physics Nanjing UniversityNanjing 210093China School of Science Changzhou Institute of TechnologyChangzhou 213032China School of Science Guangxi University of Science and TechnologyLiuzhou 545006China Joint Center for Particle Nuclear Physics and CosmologyNanjing 210093China State Key Laboratory of Theoretical Physics Institute of Theoretical PhysicsCASBeijing 100190China

We investigate a 6 D generalized Randall-Sundrum brane world scenario with a bulk cosmological *** stress-energy tensor Tabi on the brane is shown to be similar to a constant vacuum *** is consistent with the Randall-Sundrum model,in which each 3-brane Lagrangian yielded a constant vacuum *** adopting an anisotropic metric ansatz,we obtain the 5 D Friedmann-Robertson-Walker field *** a slightly later period,the expansion of the universe is proportional to the square root of time,t1/2,which is similar to the period of the radiation-dominated ***,we investigate the case with two a（t） and two b（t）.In a large range of t,we obtain the 3 D effective cosmological constant Λeff=-2Ω/3>0,which is independent of the integral ***,the scale factor is an exponential expansion,which is consistent with our present observation of the *** results demonstrate that it is possible to construct a model that solves the dark energy problem,while guaranteeing a positive brane tension.

关键词： brane induced cosmological constants anisotropy

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Fine tuning problem of the cosmological constant in a generalized Randall-Sundrum model

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Chinese physics C 2020年第12期44卷 210-214页

作者： Guang-Zhen Kang De-Sheng Zhang Li Jun Hong-Shi Zong School of Science Yangzhou Polytechnic InstituteYangzhou 225127China Department of Physics Nanjing UniversityNanjing 210093China School of Science Changzhou Institute of TechnologyChangzhou 213032China Joint Center for Particle Nuclear Physics and CosmologyNanjing 210093China State Key Laboratory of Theoretical Physics Institute of Theoretical PhysicsCASBeijing 100190China

To solve the cosmological constant fine tuning problem,we investigate an(n+1)-dimensional generalized Randall-Sundrum brane world scenario with two(n−1)-branes instead of two *** an anisotropic metric ansatz,we obtain the positive effective cosmological constantΩeff of order 10−124 and only require a solution≃50−***,both the visible and hidden branes are stable because their tensions are ***,the fine tuning problem can be solved quite ***,the Hubble parameter H1(z)as a function of redshift z is in good agreement with the cosmic chronometers *** evolution of the universe naturally shifts from deceleration to *** suggests that the evolution of the universe is intrinsically an extra-dimensional *** can be regarded as a dynamic model of dark energy that is driven by the evolution of the extra dimensions on the brane.

关键词： cosmological constant fine tuning extra dimensions Hubble parameter

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Simons Observatory: Characterization of the Large Aperture Telescope Receiver

arXiv

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arXiv 2025年

作者： Bhandarkar, Tanay Haridas, Saianeesh K. Iuliano, Jeff Kofman, Anna Manduca, Alex Sarmiento, Karen Perez Orlowski-Scherer, John Satterthwaite, Thomas P. Wang, Yuhan Ahmed, Zeeshan Austermann, Jason E. Bae, Kyuyoung Coppi, Gabriele Devlin, Mark J. Dicker, Simon R. Dow, Peter N. Duff, Shannon M. Dutcher, Daniel Galitzki, Nicholas Gudmundsson, Jon E. Henderson, Shawn W. Hubmayr, Johannes Johnson, Bradley R. Koc, Matthew A. Koopman, Brian J. Limon, Michele Link, Michael J. Lucas, Tammy J. Moore, Jenna E. Nati, Federico Niemack, Michael D. Sierra, Carlos E. Silva-Feaver, Max Singh, Robinjeet Staggs, Suzanne T. Sonka, Rita F. Thornton, Robert J. Tsan, Tran Van Lanen, Jeff L. Vavagiakis, Eve M. Vissers, Michael R. Walters, Liam Zannoni, Mario Zheng, Kaiwen Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Department of Physics Stanford University StanfordCA94305 United States Kavli Institute for Particle Astrophysics and Cosmology StanfordCA94305 United States Department of Physics Cornell University IthacaNY14853 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States National Institute of Standards and Technology Quantum Sensors Division 325 Broadway BoulderCO80305 United States Department of Physics University of Colorado BoulderCO80309 United States Department of Physics University of Milano-Bicocca Milano Italy Istituto Nazionale di Fisica Nucleare INFN Sezione Milano-Bicocca Italy Department of Astronomy University of Virginia 530 McCormick Rd CharlottesvilleVA22904 United States Department of Physics Princeton University PrincetonNJ08540 United States Department of Physics University of Texas at Austin AustinTX78712 United States Weinberg Institute for Theoretical Physics Texas Center for Cosmology and Astroparticle Physics AustinTX78712 United States Science Institute University of Iceland Reykjavik107 Iceland The Oskar Klein Centre Department of Physics Stockholm University AlbaNova StockholmSE-10691 Sweden Wright Laboratory Department of Physics Yale University New HavenCT06511 United States Department of Physics Duke University DurhamNC27708 United States Department of Physics University of Milano-Bicocca MI Milano20126 Italy Department of Physics West Chester University of Pennsylvania West ChesterPA19383 United States Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States

The Simons Observatory (SO) is a ground-based cosmic microwave background (CMB) survey experiment that currently consists of three 0.42 m small-aperture telescopes (SATs) and one 6 m large-aperture telescope (LAT), located at an elevation of 5200 m in the Atacama Desert in Chile. At the LAT's focal plane, SO will install >62,000 transition-edge sensor detectors across 13 optics tubes (OTs) within the Large Aperture Telescope Receiver (LATR), the largest cryogenic camera ever built to observe the CMB. Here we report on the validation of the LATR in the laboratory and the subsequent dark testing and validation within the LAT. We show that the LATR meets cryogenic, optical, and detector specifications required for high-sensitivity measurements of the CMB. At the time of writing, the LATR is installed in the LAT with six OTs (corresponding to >31,000 detectors), and the LAT mirrors and remaining seven OTs are undergoing development. Copyright © 2025, The Authors. All rights reserved.

关键词： cosmology

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MadMiner: Machine Learning-Based Inference for particle physics

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Computing and Software for Big science 2020年第1期4卷 1-25页

作者： Brehmer, Johann Kling, Felix Espejo, Irina Cranmer, Kyle Center for Data Science and Center for Cosmology and Particle Physics New York University New York 10003 NY United States Department of Physics and Astronomy University of California Irvine 92697 CA United States SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo Park 94025 CA United States

Precision measurements at the LHC often require analyzing high-dimensional event data for subtle kinematic signatures, which is challenging for established analysis methods. Recently, a powerful family of multivariate inference techniques that leverage both matrix element information and machine learning has been developed. This approach neither requires the reduction of high-dimensional data to summary statistics nor any simplifications to the underlying physics or detector response. In this paper, we introduce MadMiner , a Python module that streamlines the steps involved in this procedure. Wrapping around MadGraph5_aMC and Pythia 8, it supports almost any physics process and model. To aid phenomenological studies, the tool also wraps around Delphes 3, though it is extendable to a full Geant4-based detector simulation. We demonstrate the use of MadMiner in an example analysis of dimension-six operators in ttH production, finding that the new techniques substantially increase the sensitivity to new physics. © 2020, Springer Nature Switzerland AG.

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On the renormalization of entanglement entropy

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AAPPS Bulletin 2021年第1期31卷 1-7页

作者： Pang, Jin-Yi Chen, Jiunn-Wei College of Science University of Shanghai for Science and Technology Shanghai 200093 China Helmholtz-Institut für Strahlen- und Kernphysik and Bethe Center for Theoretical Physics Universität Bonn Bonn 53115 Germany Department of Physics Center for Theoretical Physics and Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei Taiwan Physics Division National Center for Theoretical Sciences Taipei Taiwan

The renormalization of entanglement entropy of quantum field theories is investigated in the simplest setting with a λ ϕ 4 scalar field theory. The 3+1 dimensional spacetime is separated into two regions by an infini... 详细信息

The renormalization of entanglement entropy of quantum field theories is investigated in the simplest setting with a λ ϕ ⁴ scalar field theory. The 3+1 dimensional spacetime is separated into two regions by an infinitely flat 2-dimensional interface. The entanglement entropy of the system across the interface has an elegant geometrical interpretation using the replica trick, which requires putting the field theory on a curved spacetime background. We demonstrate that the theory, and hence the entanglement entropy, is renormalizable at order λ once all the relevant operators up to dimension 4 are included in the action. This exercise has a one-to-one correspondence to entanglement entropy interpretation of the black hole entropy which suggests that our treatment is sensible. Our study suggests that entanglement entropy is renormalizable and is a physical quantity. © 2021, The Author(s).

关键词： Back hole Entanglement entropy Quantum field theory Renormalization

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Discovery potentials of doubly charmed baryons

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Chinese physics C 2018年第5期42卷 1-8页

作者：于福升蒋华玉李润辉吕才典王伟赵振兴 School of Nuclear Science and Technology Lanzhou University Research Center for Hadron and CSR Physics Lanzhou University and Institute of Modern Physics of Chinese Academy of Sciences School of Physical Science and Technology Inner Mongolia University Institute of High Energy Physics Chinese Academy of Sciences School of Physics University of Chinese Academy of Sciences INPAC Shanghai Key Laboratory for Particle Physics and Cosmology School of Physics and Astronomy Shanghai Jiao-Tong University

The existence of doubly heavy flavor baryons has not been well established experimentally so far. In this Letter we systematically investigate the weak decays of the doubly charmed baryons, Ξ;and Ξ;, which should be helpful for experimental searches for these particles. The long-distance contributions are first studied in the doubly heavy baryon decays, and found to be significantly enhanced. Comparing all the processes, Ξ;→Λ;K;π;π;andΞ;π;are the most favorable decay modes for experiments to search for doubly heavy baryons.

关键词： doubly charmed baryon weak decay branching fraction factorization final-state interaction

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Development of an analysis method for neutrino-induced air showers with the Telescope Array surface detectors 7

Development of an analysis method for neutrino-induced air s...

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7th International Symposium on Ultra-High-Energy Cosmic Rays, UHECR 2024

作者： Takahashi, K. Sako, T. Fujisue, K. Fujita, K. Kawata, K. Ogio, S. Oshima, H. Sagawa, H. Takeda, M. Abbasi, R.U. Abu-Zayyad, T. Allen, M. Belz, J.W. Bergman, D.R. Buckland, I. Campbell, W. Cheon, B.G. Endo, K. Fedynitch, A. Fujii, T. Fujisue, K. Fujita, K. Fukushima, M. Furlich, G. Gerber, Z. Globus, N. Hanlon, W. Hayashida, N. He, H. Hibino, K. Higuchi, R. Ikeda, D. Ishii, T. Ivanov, D. Jeong, S. Jui, C.C.H. Kadota, K. Kakimoto, F. Kalashev, O. Kasahara, K. Kawachi, Y. Kawata, K. Kharuk, I. Kido, E. Kim, H.B. Kim, J.H. Kim, S.W. Kobo, R. Komae, I. Komatsu, K. Komori, K. Koyama, C. Kudenko, M. Kuroiwa, M. Kusumori, Y. Kuznetsov, M. Kwon, Y.J. Lee, K.H. Lee, M.J. Lubsandorzhiev, B. Lundquist, J.P. Matsuzawa, A. Matthews, J.A. Matthews, J.N. Mizuno, K. Mori, M. Murakami, M. Nagataki, S. Nakahara, M. Nakamura, T. Nakayama, T. Nakayama, Y. Nonaka, T. Ogio, S. Ohoka, H. Okazaki, N. Onishi, M. Oshima, A. Oshima, H. Ozawa, S. Park, I.H. Park, K.Y. Potts, M. Przybylak, M. Pshirkov, M.S. Remington, J. Rott, C. Rubtsov, G.I. Ryu, D. Sagawa, H. Sakaki, N. Sakamoto, R. Sako, T. Sakurai, N. Sakurai, S. Sato, D. Sato, S. Sekino, K. Shibata, T. Shikita, J. Shimodaira, H. Shin, B.K. Shin, H.S. Shinozaki, K. Smith, J.D. Sokolsky, P. Stokes, B.T. Stroman, T.A. Takagi, Y. Takahashi, K. Takeda, M. Takeishi, R. Taketa, A. Takita, M. Tameda, Y. Tanaka, K. Tanaka, M. Thomas, S.B. Thomson, G.B. Tinyakov, P. Tkachev, I. Tomida, T. Troitsky, S. Tsunesada, Y. Udo, S. Urban, F. Vaiman, I.A. Vrabel, M. Warren, D. Yamazaki, K. Zhezher, Y. Zundel, Z. Zvirzdin, J. ICRR University of Tokyo 5-1-5 Kashiwa-no-Ha Chiba Kashiwa City277-8582 Japan Institute of Physics Academia Sinica No.128 Sec.2 Academia Rd. Taipei115 Taiwan Department of Physics Loyola University Chicago ChicagoIL60660 United States High Energy Astrophysics Institute Department of Physics and Astronomy University of Utah Salt Lake CityUT84112-0830 United States Department of Physics The Research Institute of Natural Science Hanyang University Seongdong-gu Seoul426-791 Korea Republic of Graduate School of Science Osaka Metropolitan University Sugimoto Sumiyoshi Osaka558-8585 Japan Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa277-8582 Japan Institute of Physics Academia Sinica Taipei City115201 Taiwan Nambu Yoichiro Institute of Theoretical and Experimental Physics Osaka Metropolitan University Sugimoto Sumiyoshi Osaka558-8585 Japan Astrophysical Big Bang Laboratory RIKEN Saitama Wako351-0198 Japan Faculty of Engineering Kanagawa University Kanagawa Yokohama221-8686 Japan Interdisciplinary Graduate School of Medicine and Engineering University of Yamanashi Yamanashi Kofu400-8511 Japan Department of Physics Sungkyunkwan University Jang-an-gu Suwon16419 Korea Republic of Department of Physics Tokyo City University Tokyo158-8557 Japan Institute for Nuclear Research Russian Academy of Sciences Moscow117312 Russia Faculty of Systems Engineering and Science Shibaura Institute of Technology Tokyo337-8570 Japan Academic Assembly School of Science and Technology Institute of Engineering Shinshu University Nagano Nagano380-8554 Japan Graduate School of Engineering Osaka Electro-Communication University Neyagawa-shi Osaka572-8530 Japan Service de Physique Theorique Universite Libre de Bruxelles Brussels1050 Belgium Department of Physics Yonsei University Seodaemun-gu Seoul120-749 Korea Republic of Center for Astrophysics and Cosmology University of Nova Gorica Nova Gorica5297 Slovenia Faculty o

The origins of Ultra High Energy Cosmic Rays (UHECRs) remain unclear. A significant difficulty in identifying their sources is the complex deflection of charged particles by galactic and intergalactic magnetic fields. Our goal is to detect high-energy neutrinos produced through interactions between UHECRs and matter near astrophysical objects, to help elucidate their origins. In this study, we utilize data from the Telescope Array surface detector (TA SD) to search for neutrino-induced air showers. To achieve this, we have developed an analysis method using Monte Carlo (MC) simulations. Our approach focuses on inclined air showers, as both the probability of interaction and the efficiency of background rejection increase at larger zenith angles. Since standard TA analyses limit zenith angles below 55 degrees, this study rigorously examines the validity of thinning and dethinning processes in MC simulations at larger zenith angles. To minimize variations in shower characteristics, we concentrate on showers produced by electron neutrinos through charged current interactions. This study will not only present a detailed analysis method but also discuss the characteristics of neutrino-induced air showers, which are essential for distinguishing them from background events. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0) All rights for text and data mining, AI training, and similar technologies for commercial purposes, are reserved.

关键词： Cosmic rays

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Narrowband Imaging of a z = 3.24 Protocluster: Insights from [O III] Emitting Galaxies

arXiv

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arXiv 2025年

作者： Shi, Ke Toshikawa, Jun Zheng, Xianzhong Cai, Zheng Shi, Dongdong School of Physical Science and Technology Southwest University Chongqing400715 China Nishi-Harima Astronomical Observatory Center for Astronomy University of Hyogo 407-2 Nishigaichi Sayo-cho Sayo Hyogo 679-5313 Japan Tsung-Dao Lee Institute Key Laboratory for Particle Physics Astrophysics and Cosmology Ministry of Education Shanghai Jiao Tong University Shanghai201210 China Department of Astronomy Tsinghua University Beijing100084 China Center for Fundamental Physics School of Mechanics & Optoelectronic Physics Anhui University of Science & Technology Huainan232001 China

We present a narrowband imaging on a spectroscopically confirmed protocluster "D4UD01" at z = 3.24 using CFHT/WIRCam. We identify a sample of 24 [O iii] emission line galaxies in the field, which forms a large overdensity in the protocluster region. The protocluster is expected to evolve into a Virgo-like cluster by z = 0. Utilizing multiwavelength data, we derive the physical properties of these [O iii] emitters and find they are medium mass normal star-forming galaxies (∼ 1010M☉) roughly following the star-forming main sequence. The [O iii] emitters trace an overdensity spatially offset from that of photometric-redshift and quiescent galaxies, suggesting these distinct galaxy populations may inhabit dark matter halos that formed at different epochs. A comparative analysis of [O iii] emitter properties shows similar characteristics in both protocluster and field environments. This protocluster likely represents an evolved structure that has progressed beyond its peak star-formation phase, although our limited sample size may prevent detection of subtle environmental effects. Copyright © 2025, The Authors. All rights reserved.

关键词： Dark Matter

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Anisotropies, large and small 38

Anisotropies, large and small

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38th International Cosmic Ray Conference, ICRC 2023

作者： Bister, Teresa Farrar, Glennys Institute for Mathematics Astrophysics and Particle Physics Radboud University Nijmegen Nijmegen Netherlands Science Park Amsterdam Netherlands Center for Cosmology and Particle Physics New York University New YorkNY10003 United States

We report on several new results using anisotropies of UHECRs. We improve and extend the work of Ding, Globus and Farrar, who modeled the UHECR dipole assuming sources follow the dark matter distribution, accounting for deflections in the Galactic and extragalactic magnetic fields but using a simplified treatment of interactions during propagation. The work presented here employs an accurate and self-consistent treatment of the evolution of composition during propagation, allows for and explores the impact of "bias" in the relation between UHECR sources and the dark matter distribution, and investigates the possible generation of arrival-direction-dependent composition anisotropies. Limits on the source number density consistent with the observed anisotropies are derived for the case where UHECR sources follow the dark matter distribution, and compared to a homogeneous source distribution case. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Anisotropy

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Calibration of the TA Fluorescence Detectors and Systematic Uncertainties in UHECR Analysis 7

Calibration of the TA Fluorescence Detectors and Systematic ...

引用

7th International Symposium on Ultra-High-Energy Cosmic Rays, UHECR 2024

作者： Tomida, Takayuki Sato, Daiki Mizuno, Kota Matsuzawa, Aoi Tameda, Yuichiro Yamazaki, Katsuya Fujita, Keitaro Ikeda, Daisuke Matthews, John Abbasi, R.U. Abu-Zayyad, T. Allen, M. Belz, J.W. Bergman, D.R. Buckland, I. Campbell, W. Cheon, B.G. Endo, K. Fedynitch, A. Fujii, T. Fujisue, K. Fujita, K. Fukushima, M. Furlich, G. Gerber, Z. Globus, N. Hanlon, W. Hayashida, N. He, H. Hibino, K. Higuchi, R. Ikeda, D. Ishii, T. Ivanov, D. Jeong, S. Jui, C.C.H. Kadota, K. Kakimoto, F. Kalashev, O. Kasahara, K. Kawachi, Y. Kawata, K. Kharuk, I. Kido, E. Kim, H.B. Kim, J.H. Kim, S.W. Kobo, R. Komae, I. Komatsu, K. Komori, K. Koyama, C. Kudenko, M. Kuroiwa, M. Kusumori, Y. Kuznetsov, M. Kwon, Y.J. Lee, K.H. Lee, M.J. Lubsandorzhiev, B. Lundquist, J.P. Matsuzawa, A. Matthews, J.A. Matthews, J.N. Mizuno, K. Mori, M. Murakami, M. Nagataki, S. Nakahara, M. Nakamura, T. Nakayama, T. Nakayama, Y. Nonaka, T. Ogio, S. Ohoka, H. Okazaki, N. Onishi, M. Oshima, A. Oshima, H. Ozawa, S. Park, I.H. Park, K.Y. Potts, M. Przybylak, M. Pshirkov, M.S. Remington, J. Rott, C. Rubtsov, G.I. Ryu, D. Sagawa, H. Sakaki, N. Sakamoto, R. Sako, T. Sakurai, N. Sakurai, S. Sato, D. Sato, S. Sekino, K. Shibata, T. Shikita, J. Shimodaira, H. Shin, B.K. Shin, H.S. Shinozaki, K. Smith, J.D. Sokolsky, P. Stokes, B.T. Stroman, T.A. Takagi, Y. Takahashi, K. Takeda, M. Takeishi, R. Taketa, A. Takita, M. Tameda, Y. Tanaka, K. Tanaka, M. Thomas, S.B. Thomson, G.B. Tinyakov, P. Tkachev, I. Tomida, T. Troitsky, S. Tsunesada, Y. Udo, S. Urban, F. Vaiman, I.A. Vrabel, M. Warren, D. Yamazaki, K. Zhezher, Y. Zundel, Z. Zvirzdin, J. Academic Assembly School of Science and Technology Institute of Engineering Shinshu University Nagano Nagano Japan Department of Engineering Science Faculty of Engineering Osaka Electro-Communication University Osaka Neyagawa Japan Chubu University Aichi Kasugai Japan Institute for Cosmic Ray Research The University of Tokyo Chiba Kashiwa Japan Faculty of Engineering Kanagawa University Kanagawa Yokohama Japan High Energy Astrophysics Institute Department of Physics and Astronomy University of Utah Salt Lake CityUT United States Department of Physics Loyola University Chicago ChicagoIL60660 United States High Energy Astrophysics Institute Department of Physics and Astronomy University of Utah Salt Lake CityUT84112-0830 United States Department of Physics The Research Institute of Natural Science Hanyang University Seongdong-gu Seoul426-791 Korea Republic of Graduate School of Science Osaka Metropolitan University Sugimoto Sumiyoshi Osaka558-8585 Japan Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa277-8582 Japan Institute of Physics Academia Sinica Taipei City115201 Taiwan Nambu Yoichiro Institute of Theoretical and Experimental Physics Osaka Metropolitan University Sugimoto Sumiyoshi Osaka558-8585 Japan Astrophysical Big Bang Laboratory RIKEN Saitama Wako351-0198 Japan Faculty of Engineering Kanagawa University Kanagawa Yokohama221-8686 Japan Interdisciplinary Graduate School of Medicine and Engineering University of Yamanashi Yamanashi Kofu400-8511 Japan Department of Physics Sungkyunkwan University Jang-an-gu Suwon16419 Korea Republic of Department of Physics Tokyo City University Setagaya-ku Tokyo158-8557 Japan Institute for Nuclear Research Russian Academy of Sciences Moscow117312 Russia Faculty of Systems Engineering and Science Shibaura Institute of Technology Minato-ku Tokyo337-8570 Japan Academic Assembly School of Science and Technology Institute of Engineering Shinshu University Na

Accurate calibration of the Telescope Array Fluorescence Detector (TA-FD) and the atmosphere is crucial for precise analysis of Ultra High Energy Cosmic Rays (UHECRs) using the atmospheric fluorescence method. This paper focuses on two key aspects of calibration: the pointing direction of the TA-FD and the atmospheric transparency as measured by the Vertical Aerosol Optical Depth (VAOD). The pointing direction of the TA-FD was analyzed with an accuracy of ±0.03 degrees using the Opt-copter, a drone-mounted LED light source. The impact of this pointing accuracy on cosmic ray analysis, including the biases and systematic uncertainties it introduces, is estimated. Additionally, the TA experiment continuously observes UHECRs with the FD, capturing air showers induced by primary UHECRs. Monthly VAOD values, determined through Central Laser Facility (CLF) operation, exhibit a seasonal dependence. Incorporating this seasonal variation into air shower analysis can improve the accuracy of primary energy and Xmax measurements, along with the associated systematic uncertainties. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). All rights for text and data mining, AI training, and similar technologies for commercial purposes, are reserved.

关键词： Cosmic rays

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