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38th International Cosmic Ray Conference, ICRC 2023

作者： Abbasi, R. Ackermann, M. Adams, J. Agarwalla, S.K. Aguilar, J.A. Ahlers, M. Alameddine, J.M. Amin, N.M. Andeen, K. Anton, G. Argüelles, C. Ashida, Y. Athanasiadou, S. Audehm, J. Axani, S.N. Bai, X. Balagopal, A.V. Baricevic, M. Barwick, S.W. Basu, V. Bay, R. Becker Tjus, J. Beise, J. Bellenghi, C. Benning, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Bishop, A. Blaufuss, E. Blot, S. Bohmer, M. Bontempo, F. Book, J.Y. Borowka, J. Boscolo Meneguolo, C. Böser, S. Botner, O. Böttcher, J. Bouma, S. Bourbeau, E. Braun, J. Brinson, B. Brostean-Kaiser, J. Burley, R.T. Busse, R.S. Butterfield, D. Campana, M.A. Carloni, K. Carnie-Bronca, E.G. Cataldo, M. Chattopadhyay, S. Chau, N. Chen, C. Chen, Z. Chirkin, D. Choi, S. Clark, B.A. Clark, R. Classen, L. Coleman, A. Collin, G.H. Conrad, J.M. Cowen, D.F. Dasgupta, B. Dave, P. Deaconu, C. De Clercq, C. De Kockere, S. DeLaunay, J.J. Delgado, D. Deng, S. Deoskar, K. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. DeYoung, T. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Domi, A. Dujmovic, H. DuVernois, M.A. Ehrhardt, T. Eller, P. Ellinger, E. El Mentawi, S. Elsässer, D. Engel, R. Erpenbeck, H. Evans, J. Evans, J.J. Evenson, P.A. Fan, K.L. Fang, K. Farrag, K. Farrag, K. Fazely, A.R. Fedynitch, A. Feigl, N. Fiedlschuster, S. Finley, C. Fischer, L. Flaggs, B. Fox, D. Franckowiak, A. Fritz, A. Fujii, T. Fürst, P. Gallagher, J. Ganster, E. Garcia, A. Gerhardt, L. Gernhaeuser, R. Ghadimi, A. Giri, P. Glaser, C. Glauch, T. Glüsenkamp, T. Goehlke, N. Goswami, S. Grant, D. Gray, S.J. Gries, O. Griffin, S. Griswold, S. Guevel, D. Günther, C. Gutjahr, P. Haack, C. Haji Azim, T. Hallgren, A. Halliday, R. Hallmann, S. Halve, L. Halzen, F. Hamdaoui, H. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Hatch, P. Haugen, J. Haungs, A. Heinen, D. Helbing, K. Hellrung, J. Hendricks, B. Henningsen, F. Henrichs, J. Heuermann, L. Heyer, N. Hickford, S. Hidvegi, A. Hignight, J. Hill, C. III. Physikalisches Institut RWTH Aachen University AachenD-52056 Germany Department of Physics University of Adelaide Adelaide5005 Australia Dept. of Physics and Astronomy University of Alaska Anchorage 3211 Providence Dr. AnchorageAK99508 United States Dept. of Physics University of Texas at Arlington 502 Yates St. Science Hall Rm 108 Box 19059 ArlingtonTX76019 United States CTSPS Clark-Atlanta University AtlantaGA30314 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA30332 United States Dept. of Physics Southern University Baton RougeLA70813 United States Dept. of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institut für Physik Humboldt-Universität zu Berlin BerlinD-12489 Germany Fakultät für Physik & Astronomie Ruhr-Universität Bochum BochumD-44780 Germany Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dienst ELEM BrusselsB-1050 Belgium Department of Physics Laboratory for Particle Physics and Cosmology Harvard University CambridgeMA02138 United States Dept. of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Dept. of Physics The International Center for Hadron Astrophysics Chiba University Chiba263-8522 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Dept. of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Dept. of Physics University of Chicago ChicagoIL60637 United States Enrico Fermi Institute University of Chicago ChicagoIL60637 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Dept. of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Astronomy Ohio Sta

The planned in-ice radio array of IceCube-Gen2 at the South Pole will provide unprecedented sensitivity to ultra-high-energy (UHE) neutrinos in the EeV range. The ability of the detector to measure the neutrino’s energy and direction is of crucial importance. This contribution presents an end-to-end reconstruction of both of these quantities for both detector components of the hybrid radio array (’shallow’ and’deep’) using deep neural networks (DNNs). We are able to predict the neutrino’s direction and energy precisely for all event topologies, including the electron neutrino charged-current (νe-CC) interactions, which are more complex due to the LPM effect. This highlights the advantages of DNNs for modeling the complex correlations in radio detector data, thereby enabling a measurement of the neutrino energy and direction. We discuss how we can use normalizing flows to predict the PDF for each individual event which allows modeling the complex non-Gaussian uncertainty contours of the reconstructed neutrino direction. Finally, we discuss how this work can be used to further optimize the detector layout to improve its reconstruction performance. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Neutrons

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Sensitivity of IceCube-Gen2 to measure flavor composition of Astrophysical neutrinos 38

Sensitivity of IceCube-Gen2 to measure flavor composition of...

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38th International Cosmic Ray Conference, ICRC 2023

作者： Lad, Neha Abbasi, R. Ackermann, M. Adams, J. Agarwalla, S.K. Aguilar, J.A. Ahlers, M. Alameddine, J.M. Amin, N.M. Andeen, K. Anton, G. Argüelles, C. Ashida, Y. Athanasiadou, S. Audehm, J. Axani, S.N. Bai, X. Balagopal, A.V. Baricevic, M. Barwick, S.W. Basu, V. Bay, R. Becker Tjus, J. Beise, J. Bellenghi, C. Benning, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Bishop, A. Blaufuss, E. Blot, S. Bohmer, M. Bontempo, F. Book, J.Y. Borowka, J. Boscolo Meneguolo, C. Böser, S. Botner, O. Böttcher, J. Bouma, S. Bourbeau, E. Braun, J. Brinson, B. Brostean-Kaiser, J. Burley, R.T. Busse, R.S. Butterfield, D. Campana, M.A. Carloni, K. Carnie-Bronca, E.G. Cataldo, M. Chattopadhyay, S. Chau, N. Chen, C. Chen, Z. Chirkin, D. Choi, S. Clark, B.A. Clark, R. Classen, L. Coleman, A. Collin, G.H. Conrad, J.M. Cowen, D.F. Dasgupta, B. Dave, P. Deaconu, C. De Clercq, C. De Kockere, S. DeLaunay, J.J. Delgado, D. Deng, S. Deoskar, K. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. DeYoung, T. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Domi, A. Dujmovic, H. DuVernois, M.A. Ehrhardt, T. Eller, P. Ellinger, E. El Mentawi, S. Elsässer, D. Engel, R. Erpenbeck, H. Evans, J. Evans, J.J. Evenson, P.A. Fan, K.L. Fang, K. Farrag, K. Farrag, K. Fazely, A.R. Fedynitch, A. Feigl, N. Fiedlschuster, S. Finley, C. Fischer, L. Flaggs, B. Fox, D. Franckowiak, A. Fritz, A. Fujii, T. Fürst, P. Gallagher, J. Ganster, E. Garcia, A. Gerhardt, L. Gernhaeuser, R. Ghadimi, A. Giri, P. Glaser, C. Glauch, T. Glüsenkamp, T. Goehlke, N. Goswami, S. Grant, D. Gray, S.J. Gries, O. Griffin, S. Griswold, S. Guevel, D. Günther, C. Gutjahr, P. Haack, C. Haji Azim, T. Hallgren, A. Halliday, R. Hallmann, S. Halve, L. Halzen, F. Hamdaoui, H. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Hatch, P. Haugen, J. Haungs, A. Heinen, D. Helbing, K. Hellrung, J. Hendricks, B. Henningsen, F. Henrichs, J. Heuermann, L. Heyer, N. Hickford, S. Hidvegi, A. Hignight, J. III. Physikalisches Institut RWTH Aachen University AachenD-52056 Germany Department of Physics University of Adelaide Adelaide5005 Australia Dept. of Physics and Astronomy University of Alaska Anchorage 3211 Providence Dr. AnchorageAK99508 United States Dept. of Physics University of Texas at Arlington 502 Yates St. Science Hall Rm 108 Box 19059 ArlingtonTX76019 United States CTSPS Clark-Atlanta University AtlantaGA30314 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA30332 United States Dept. of Physics Southern University Baton RougeLA70813 United States Dept. of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institut für Physik Humboldt-Universität zu Berlin BerlinD-12489 Germany Fakultät für Physik & Astronomie Ruhr-Universität Bochum BochumD-44780 Germany Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dienst ELEM BrusselsB-1050 Belgium Department of Physics Laboratory for Particle Physics and Cosmology Harvard University CambridgeMA02138 United States Dept. of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Dept. of Physics The International Center for Hadron Astrophysics Chiba University Chiba263-8522 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Dept. of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Dept. of Physics University of Chicago ChicagoIL60637 United States Enrico Fermi Institute University of Chicago ChicagoIL60637 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Dept. of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Astronomy Ohio Stat

The observation of an astrophysical neutrino flux in IceCube and its detection capability to separate between the different neutrino flavors has led IceCube to constraint the flavor content of this flux. IceCube-Gen2 is the planned extension of the current IceCube detector, which will be about 8 times larger than the current instrumented volume. In this work, we study the sensitivity of IceCubeGen2 to the astrophysical neutrino flavor composition and investigate its tau neutrino identification capabilities. We apply the IceCube analysis on a simulated IceCube-Gen2 dataset that mimics the High Energy Starting Event (HESE) classification. Reconstructions are performed using sensors that have 3 times higher quantum efficiency and isotropic angular acceptance compared to the current IceCube optical modules. We present the projected sensitivity for 10 years of data on constraining the flavor ratio of the astrophysical neutrino flux at Earth by IceCube-Gen2. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Astrophysics

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Estimating the coincidence rate between the optical and radio array of IceCube-Gen2 38

Estimating the coincidence rate between the optical and radi...

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38th International Cosmic Ray Conference, ICRC 2023

The IceCube-Gen2 Neutrino Observatory is proposed to extend the all-flavour energy range of IceCube beyond PeV energies. It will comprise two key components: I) An enlarged 8 km3 in-ice optical Cherenkov array to measure the continuation of the IceCube astrophysical neutrino flux and improve IceCube’s point source sensitivity above ∼ 100 TeV;and II) A very large in-ice radio array with a surface area of about 500 km2. Radio waves propagate through ice with a kilometer-long attenuation length, hence a sparse radio array allows us to instrument a huge volume of ice to achieve a sufficient sensitivity to detect neutrinos with energies above tens of PeV. The different signal topologies for neutrino-induced events measured by the optical and in-ice radio detector - the radio detector is mostly sensitive to the cascades produced in the neutrino interaction, while the optical detector can detect long-ranging muon and tau leptons with high accuracy - yield highly complementary information. When detected in coincidence, these signals will allow us to reconstruct the neutrino energy and arrival direction with high fidelity. Furthermore, if events are detected in coincidence with a sufficient rate, they resemble the unique opportunity to study systematic uncertainties and to cross-calibrate both detector components. We present the expected rate of coincidence events for 10 years of operation. Furthermore, we analyzed possible detector optimizations to increase the coincidence rate. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Neutrons

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Search for the lepton favor violating decay J/ψ→eμ

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science China(physics,Mechanics & Astronomy) 2023年第2期66卷 24-33页

作者： BESII Collaboratio Institute of High Energy Physics Beijing 100049 China Beihang University Beijing 100191 China Beijing Institute of Petrochemical Technology Beijing 102617 China Bochum Ruhr-University Bochum D-44780 Germany Carnegie Mellon University Pittsburgh 15213 USA Central China Normal University Wuhan 430079 China Central South University Changsha 410083 China China Center of Advanced Science and Technology Beijing 100190 China COMSATS University Islamabad Lahore Campus Defence Road Off Raiwind Road Lahore 54000 Pakistan Fudan University Shanghai 200433 China G.I. Budker Institute of Nuclear Physics SB RAS (BINP) Novosibirsk 630090 Russia GSI Helmholtzcentre for Heavy Ion Research GmbH Darmstadt D-64291 Germany Guangxi Normal University Guilin 541004 China Guangxi University Nanning 530004 China Hangzhou Normal University Hangzhou 310036 China Hebei University Baoding 071002 China Helmholtz Institute Mainz Staudinger Weg 18 Mainz D-55099 Germany Henan Normal University Xinxiang 453007 China Henan University of Science and Technology Luoyang 471003 China Henan University of Technology Zhengzhou 450001 China Huangshan College Huangshan 245000 China Hunan Normal University Changsha 410081 China Hunan University Changsha 410082 China Indian Institute of Technology Madras Chennai 600036 India Indiana University Bloomington 47405 USA INFN Laboratori Nazionali di Frascati INFN Laboratori Nazionali di Frascati Frascati I-00044 Italy INFN Laboratori Nazionali di Frascati INFN Sezione di Perugia Perugia I-06100 Italy INFN Laboratori Nazionali di Frascati University of Perugia Perugia I-06100 Italy INFN Sezione di Ferrara INFN Sezione di Ferrara Ferrara I-44122 Italy INFN Sezione di Ferrara University of Ferrara Ferrara I-44122 Italy Institute of Modern Physics Lanzhou 730000 China Institute of Physics and Technology Peace Avenue 54B Ulaanbaatar 13330 Mongolia Jilin University Changchun 130012 China Johannes Gutenberg Univers

We present a search for the lepton flavor violating decay J/ψ→e±μ?using 8.998×109J/ψevents collected with the BESⅢdetector at the BEPCⅡe+e-storage *** excess of signal above background is observed;we therefore set an upper limit on the branching fraction of B(J/ψ→e±μ?)<4.5×10-9at the 90%confidence *** the previous best result by a factor of more than 30,this measurement places the most stringent limit to date on lepton flavor violation in the heavy quarkonium sector.

关键词： BESⅢ decay limit

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Performance studies on new 4" photomultiplier types intended for IceCube-Gen2 optical modules 38

Performance studies on new 4" photomultiplier types intended...

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38th International Cosmic Ray Conference, ICRC 2023

In the upcoming IceCube-Gen2 extension, the newly developed optical modules will include 4–inch PMTs. For this purpose, the manufacturers Hamamatsu and North Night Vision Technology have developed new PMT models to meet the requirements of the IceCube-Gen2 science case. The specifications include strict requirements on temporal resolution, detection efficiency, and dark noise. We summarize the efforts to measure these performance characteristics and show that both PMT models meet the performance specifications set by IceCube-Gen2. Prototype optical modules based on both PMT models will be deployed with the IceCube Upgrade in order to test them in situ and help decide on a vendor for the Gen2 extension. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Night vision devices

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Scale-invariant enhancement of gravitational waves during inflation

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Modern physics Letters A 2023年第12-13期38卷

作者： Ota, Atsuhisa Sasaki, Misao Wang, Yi HKUST Jockey Club Institute for Advanced Study Hong Kong University of Science and Technology Clear Water Bay Hong Kong Hong Kong Kavli Institute for the Physics and Mathematics of the Universe (WPI) University of Tokyo Chiba 277-8583 Japan Center for Gravitational Physics and Quantum Information Yukawa Institute for Theoretical Physics Kyoto University Kyoto 606-8502 Japan Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei 10617 Taiwan Department of Physics Hong Kong University of Science and Technology Clear Water Bay Hong Kong Hong Kong

The inflationary 1-loop tensor power spectrum from a spectator scalar field with a sharp peak is calculated. Recent studies on primordial black holes suggest that the inflationary curvature perturbation may be huge on small scales. An enhanced curvature perturbation may arise from a drastic enhancement of spectator scalar field fluctuations. In this paper, using the in-in formalism, we calculate 1-loop quantum corrections to primordial gravitational waves by such a spectator field with a sharp peak in momentum space. We find scale-invariant loop corrections in this full quantum setup, in contrast to the sharply peaked corrections in the previously calculated scalar-induced tensor modes. Especially on super Hubble scales, the primordial gravitational waves are also amplified, which can be understood as a Bogoliubov transformation of the vacuum due to the enhanced scalar field. This mechanism allows us to probe the scalar field properties on extremely short-distance scales with the current and future cosmic microwave background and gravitational wave experiments, opening a novel window for inflationary cosmology. © 2023 World Scientific Publishing Company.

关键词： Inflation primordial black holes primordial graviational waves

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New insight into the hard X-ray emission influenced by the type-I bursts observed by Insight-HXMT during outburst of 4U 1636–536

arXiv

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arXiv 2025年

作者： Peng, J.Q. Zhang, S. Chen, Y.P. Kong, L.D. Wang, P.J. Zhang, S.N. Shui, Q.C. Ji, L. Zhang, G.B. Yan, Z. Tao, L. Qu, J.L. Ge, M.Y. Yu, Z.L. Li, J. Chang, Z. Li, Z.S. Zhang, P. Xiao, Y.X. Zhao, S.J. 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 Institute für Astronomie und Astrophysik Kepler Center for Astro and Particle Physics Eberhard Karls Universität Sand 1 TübingenD-72076 Germany School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 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 Key Laboratory of Stars and Interstellar Medium Xiangtan University Hunan Xiangtan411105 China College of Science China Three Gorges University Yichang443002 China Center for Astronomy and Space Sciences China Three Gorges University Yichang443002 China

Context. Thermonuclear bursts, also known as type-I X-ray bursts, result from unstable nuclear burning of H/He accreted to the surface of neutron stars, lasting from tens of seconds to hundreds of seconds. Thermonuclear bursts have an important impact on accretion environments around the neutron stars, such as their disks and corona, and are therefore a subject of extensive research. Thermonuclear bursts can be used as probes to gain a deeper understanding of the properties of their disks and corona. Aims. By analyzing the data from Insight-HXMT and NICER, we can determine the evolution of the significance of the hard shortage in 4U 1636–536 with its spectral state, as well as the evolution of the fraction of deficit with energy. Additionally, we investigate the possible geometry and evolution of the corona in 4U 1636–536 by combining our findings with the results of spectral analysis. Methods. Extracting the light curves from the Insight-HXMT LE, ME, and HE data and subtracting their pre-burst emission allows us to estimate the significance of the hard shortages during the bursts. By fitting the spectra, the correlation between the persistent spectral parameters and the significance of the hard shortages can be established. The bursts are then grouped according to the spectral state in which they occurred, and the significance of the hard shortages is estimated. These in turn help to investigate the evolution of the fraction of deficit with energy. Results. We find that during the soft state, the significance of possible hard X-ray shortage in bursts is almost zero. However, in the hard state, some bursts exhibit significant shortages (>3 σ), while others do not. We attempt to establish a correlation between the significance of the hard X-ray shortage and the spectral parameters, but the data quality and the limited number of bursts prevent us from finding a strong correlation. For bursts with insignificant shortages in the soft state, their fraction of the deficit

关键词： Stars

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Exploring entanglement and spectral split correlations in three-flavor collective neutrino oscillations

arXiv

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arXiv 2024年

作者： Siwach, Pooja Balantekin, A. Baha Patwardhan, Amol V. Suliga, Anna M. Nuclear and Chemical Science Division Lawrence Livermore National Laboratory LivermoreCA94551 United States Department of Physics University of Wisconsin–Madison MadisonWI53706 United States Department of Physics New York Institute of Technology New YorkNY10023 United States School of Physics and Astronomy University of Minnesota MinneapolisMN55455 United States Center for Cosmology and Particle Physics New York University New YorkNY10003 United States Department of Physics University of California Berkeley BerkeleyCA94720 United States Department of Physics University of California La Jolla San DiegoCA92093-0319 United States

In environments with prodigious numbers of neutrinos, such as core-collapse supernovae, neutron star mergers, or the early universe, neutrino-neutrino interactions are dynamically significant. They can dominate neutrino flavor evolution and force it to be nonlinear, causing collective neutrino oscillations. Such collective oscillations have been studied numerically, for systems with up to millions of neutrinos, using mean-field or one-particle effective approximations. However, such a system of interacting neutrinos is a quantum many-body system, wherein quantum correlations could play a significant in the flavor evolution–thereby motivating the exploration of many-body treatments which follow the time evolution of these correlations. In many-body flavor evolution calculations with two neutrino flavors, the emergence of spectral splits in the neutrino energy distributions has been found to be correlated with the degree of quantum entanglement across the spectrum. In this work, for the first time, we investigate the emergence of spectral-splits in the three-flavor many-body collective neutrino oscillations. We find that the emergence of spectral splits resembles the number and location found in the mean-field approximation but not in the width. Moreover, unlike in the two-flavor many-body calculations, we find that additional degrees of freedom make it more difficult to establish a correlation between the location of the spectral splits and the degree of quantum entanglement across the neutrino energy spectrum. Copyright © 2024, The Authors. All rights reserved.

关键词： Quantum entanglement

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Nanohertz gravitational waves from a quasar-based supermassive black hole binary population model as dark sirens

arXiv

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arXiv 2024年

作者： Xiao, Si-Ren Shao, Yue Wang, Ling-Feng Song, Ji-Yu Feng, Lu Zhang, Jing-Fei Zhang, Xin Liaoning Key Laboratory of Cosmology and Astrophysics College of Sciences Northeastern University Shenyang110819 China School of Physics and Optoelectronic Engineering Hainan University Haikou570228 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

Recently, several pulsar timing array (PTA) projects have detected evidence of the existence of a stochastic gravitational wave background (SGWB) in the nanohertz frequency band, providing confidence in detecting individual supermassive black hole binaries (SMBHBs) in the future. Nanohertz GWs emitted by inspiraling SMBHBs encode the luminosity distances of SMBHBs. They can serve as dark sirens to explore the cosmic expansion history via a statistical method to obtain the redshift information of GW sources’ host galaxies using galaxy catalogs. The theoretical analysis of the dark siren method relies on the modeling of the population of SMBHBs. Using a population model consistent with the latest SGWB observations is essential, as the SGWB provides significant information about the distribution of SMBHBs. In this work, we employ a quasar-based model, which can self-consistently account for the SGWB amplitude, to estimate the population of SMBHBs. We constrain the Hubble constant using the mock GW data from different detection cases of PTAs in the future. Our results show that a PTA consisting of 100 pulsars with a white noise level of 20 ns could measure the Hubble constant with a precision close to 1% over a 10-year observation period, and a PTA with 200 pulsars may achieve this goal over a 5-year observation period. The results indicate that modeling the SMBHB population significantly influences the analysis of dark sirens, and SMBHB dark sirens have the potential to be developed as a valuable cosmological probe. Copyright © 2024, The Authors. All rights reserved.

关键词： White noise

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Back to business: SLX 1746–331 after 13 years of silence

arXiv

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arXiv 2025年

作者： Peng, Jing-Qiang Zhang, Shu Wang, Peng-Ju Zhang, Shuang-Nan Kong, Ling-Da Chen, Yu-Peng Shui, Qing-Cang Ji, Long Qu, Jin-Lu Tao, Lian Ge, Ming-Yu Ma, Rui-Can Chang, Zhi Li, Jian Li, Zhao-Sheng Yu, Zhuo-Li Yan, Zhe Zhang, Peng Xiao, Yun-Xiang Zhao, Shu-Jie 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 Institute für Astronomie und Astrophysik Kepler Center for Astro and Particle Physics Eberhard Karls Universität Sand 1 TübingenD-72076 Germany School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 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 Key Laboratory of Stars and Interstellar Medium Xiangtan University Hunan Xiangtan411105 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China College of Science China Three Gorges University Yichang443002 China Center for Astronomy and Space Sciences China Three Gorges University Yichang443002 China

The black hole candidate system SLX 1746–331 was back to business in 2023, after a long silence of roughly 13 years. An outburst was observed thoroughly by Insight-HXMT and NICER. The outburst is characterized by spectral dominance of the soft state, where the joint Insight-HXMT and NICER spectral analysis shows the temperature dependence of the disk flux follows Tin3.98, and thus suggests that the inner disk reaches to ISCO during almost the entire outburst. By assuming 0.3 LEdd for the peak flux and an inclination angle of zero degrees, the lower limit of the compact object hosted in this system is estimated as 3.28±2.14M☉. We also look into the relation of the disk temperature and disk flux for a sample of black hole systems, and by taking the disk temperature derived in the outburst of SLX 1746–331, such a relation results in a mass estimation of 5.2 ± 4.5M☉. Finally, the spin of the compact object is constrained to larger than 0.8 with a spectral model of kerrbb. Copyright © 2025, The Authors. All rights reserved.

关键词： Black holes

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