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37th International Cosmic Ray Conference, ICRC 2021

作者： Abbasi, R. Ackermann, M. Adams, J. Aguilar, J.A. Ahlers, M. Ahrens, M. Alispach, C. Allison, P. Alves, A.A. Amin, N.M. An, R. Andeen, K. Anderson, T. Anton, G. Argüelles, C. Arlen, T.C. Ashida, Y. Axani, S. Bai, X. Balagopal, A.V. Barbano, A. Bartos, I. Barwick, S.W. Bastian, B. Basu, V. Baur, S. Bay, R. Beatty, J.J. Becker, K.-H. Becker Tjus, J. Bellenghi, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Binder, G. Bindig, D. Bishop, A. Blaufuss, E. Blot, S. Boddenberg, M. Bohmer, M. Bontempo, F. Borowka, J. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Bradascio, F. Braun, J. Bron, S. Brostean-Kaiser, J. Browne, S. Burgman, A. Burley, R.T. Busse, R.S. Campana, M.A. Carnie-Bronca, E.G. Cataldo, M. Chen, C. Chirkin, D. Choi, K. Clark, B.A. Clark, K. Clark, R. Classen, L. Coleman, Alan Collin, G.H. Connolly, A. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Cross, R. Dappen, C. Dave, P. Deaconu, C. De Clercq, C. De Kockere, S. DeLaunay, J.J. Dembinski, H. Deoskar, K. De Ridder, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. de With, M. DeYoung, T. Dharani, S. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Dujmovic, H. Dunkman, M. DuVernois, M.A. Dvorak, E. Ehrhardt, T. Eller, P. Engel, R. Erpenbeck, H. Evans, J. Evans, J.J. Evenson, P.A. Fan, K.L. Farrag, K. Fazely, A.R. Fiedlschuster, S. Fienberg, A.T. Filimonov, K. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Friedman, E. Fritz, A. Fürst, P. Gaisser, T.K. Gallagher, J. Ganster, E. Garcia, A. Garrappa, S. Gartner, A. Gerhardt, L. Gernhaeuser, R. Ghadimi, A. Giri, P. Glaser, C. Glauch, T. Glüsenkamp, T. Goldschmidt, A. Gonzalez, J.G. Goswami, S. Grant, D. Grégoire, T. Griswold, S. Gündüz, M. Günther, C. Haack, C. Hallgren, A. Halliday, R. Hallmann, S. Halve, L. Halzen, F. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Haugen, J. Haungs, A. Hauser, S. Hebecker, D. Heinen, D. Helbing, K. Hendricks, B. Henningsen, F. Hettinger, E.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 Institute for Global Prominent Research 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 State Univer

The next generation of the IceCube Neutrino Observatory, IceCube-Gen2, will constitute a much larger detector, increasing the rate of high-energy neutrinos. IceCube-Gen2 will address the long-standing questions about astrophysical accelerators. The experiment will also include a surface air-shower detector which will allow for measurements of cosmic rays in the energy region where a transition between Galactic and extragalactic accelerators is expected. As a baseline design for the surface detector, we consider a surface array above the optical in-ice array consisting of the same type of stations used for the IceTop enhancement, i.e., scintillation detectors and radio antennas. In order to better understand the capabilities of such an array, we performed simulations of its response to air showers, including both detector types. We will show the results of this simulation study and discuss the prospects for the surface array of IceCube-Gen2. © 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)

关键词： Cosmic rays

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A First-look at Spatially-resolved Infrared Supernova remnants in M33 with JWST

arXiv

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arXiv 2024年

作者： Sarbadhicary, Sumit K. Rosolowsky, Erik Leroy, Adam K. Williams, Thomas G. Koch, Eric W. Peltonen, Joshua Smercina, Adam Dalcanton, Julianne J. Glover, Simon C.O. Lazzarini, Margaret Chown, Ryan Meyer, Jennifer Donovan Sandstrom, Karin Williams, Benjamin F. Tarantino, Elizabeth Department of Physics The Ohio State University ColumbusOH43210 United States Center for Cosmology & Astro-Particle Physics The Ohio State University ColumbusOH43210 United States Department of Astronomy The Ohio State University ColumbusOH43210 United States Department of Physics University of Alberta EdmontonABT6G 2E1 Canada Sub-department of Astrophysics Department of Physics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Center for Astrophysics Harvard & Smithsonian 60 Garden St. CambridgeMA02138 United States Space Telescope Science Institute 3700 San Martin Dr. BaltimoreMD21218 United States Department of Astronomy University of Washington Box 351580 SeattleWA98195 United States Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue New YorkNY10010 United States Universität Heidelberg Zentrum fur Astronomie Institut fur Theoretische Astrophysik Albert-Ueberle-Str. 2 Heidelberg69120 Germany Department of Physics & Astronomy California State University Los Angeles 5151 State University Drive Los AngelesCA90032 United States National Radio Astronomy Observatory 520 Edgemont Rd. CharlottesvilleVA22903 United States Department of Astronomy & Astrophysics University of California San Diego 9500 Gilman Drive >La Jolla CA92093 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States

We present the first spatially-resolved infrared images of supernova remnants (SNRs) in M33 with the unprecedented sensitivity and resolution of JWST. We analyze 43 SNRs in four JWST fields: two covering central and southern M33 with separate NIRCam (F335M, F444W) and MIRI (F560W, F2100W) observations, one ∼5 kpc-long radial strip observed with MIRI F770W, and one covering the giant HII region NGC 604 with multiple NIRCam and MIRI broad/narrowband filters. Of the 21 SNRs in the MIRI field, we found three clear detections (i.e., identical infrared and Hα morphologies), and six partial-detections, implying a detection fraction of 43% in these bands. In contrast, only one SNR (out of 16) is detectable in the NIRCam field. One of the SNRs, L10-080, is a potential candidate for having freshly-formed ejecta dust, based on its size and centrally-concentrated 21 µm emission. Two SNRs near NGC 604 have strong evidence of molecular (H2) emission at 4.7 µm, making them the farthest known SNRs with visible molecular shocks. Five SNRs have F770W observations, with the smaller younger objects showing tentative signs of emission, while the older, larger ones have voids. Multi-wavelength data indicate that the clearly-detected SNRs are also among the smallest, brightest at other wavelengths (Hα, radio and X-ray), have the broadest line widths (Hα FWHM∼250-350 km/s), and the densest environments. No strong correlation with star-formation histories are seen, with the clearly-detected SNRs having both high-mass (∼35 M☉) and low-mass (10 M☉) progenitors. © 2024, CC BY.

关键词： Supernovae

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Magnetar emergence in a peculiar gamma-ray burst from a compact star merger

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National science Review 2025年第3期 125-131页

作者： Hui Sun Chenwei Wang Jun Yang Bin-Bin Zhang Shaolin Xiong Yi-Han Iris Yin Yuan Liu Ye Li Wangchen Xue Zhen-Yu Yan Chen Zhang Wenjun Tan Haiwu Pan Jiacong Liu Huaqing Cheng Yanqiu Zhang Jingwei Hu Chao Zheng Zhenghua An Ce Cai Zhiming Cai Lei Hu Chichuan Jin Dongyue Li Xinqiao Li Heyang Liu Mingjun Liu Wenxi Peng Liming Song Shengli Sun Xiaojin Sun Xilu Wang Xiangyang Wen Shuo Xiao Shuxu Yi Fan Zhang Wenda Zhang Xiaofeng Zhang Yonghe Zhang Donghua Zhao Shijie Zheng Zhixing Ling Shuang-Nan Zhang Weimin Yuan Bing Zhang National Astronomical Observatories Chinese Academy of Sciences Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences University of Chinese Academy of Sciences Chinese Academy of Sciences School of Astronomy and Space Science Nanjing University Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University) Ministry of Education Purple Mountain Observatory Chinese Academy of Sciences College of Physics and Hebei Key Laboratory of Photophysics Research and Application Hebei Normal University Innovation Academy for Microsatellites Chinese Academy of Sciences Shanghai Institute of Technical Physics Chinese Academy of Sciences Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal University Nevada Center for Astrophysics University of Nevada Department of Physics and Astronomy University of Nevada

The central engine that powers gamma-ray bursts（GRBs）, the most powerful explosions in the universe, is still not identified. Besides hyper-accreting black holes, rapidly spinning and highly magnetized neutron stars, known as millisecond magnetars, have been suggested to power both long and short GRBs. The presence of a magnetar engine following compact star mergers is of particular interest as it would provide essential constraints on the poorly understood equation of state for neutron stars. Indirect indications of a magnetar engine in these merger sources have been observed in the form of plateau features present in the X-ray afterglow light curves of some short GRBs. Additionally, some X-ray transients lacking gamma-ray bursts have been identified as potential magnetar candidates originating from compact star ***, smoking-gun evidence is still lacking for a magnetar engine in short GRBs, and associated theoretical challenges have been raised. Here we present a comprehensive analysis of the broad-band prompt emission data of the peculiar, very bright GRB 230307A. Despite its apparently long duration, the prompt emission and host galaxy properties are consistent with a compact star merger origin, as suggested by its association with a kilonova. Intriguingly, an extended X-ray emission component shows up as theγ-ray emission dies out, signifying the likely emergence of a magnetar central engine. We also identify an achromatic temporal break in the high-energy band during the prompt emission phase, which was never observed in previous bursts and reveals a narrow jet with a half opening angle of ~ 3.4°(RGRB/1015cm)-1/2,where RGRBis the GRB prompt emission radius.

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Observation of Cosmic-Ray Anisotropy in the Southern Hemisphere with Twelve Years of data Collected by the IceCube Neutrino Observatory

arXiv

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arXiv 2024年

作者： Abbasi, R. Ackermann, M. Adams, J. Agarwalla, S.K. Aguado, T. Aguilar, J.A. Ahlers, M. Alameddine, J.M. Amin, N.M. Andeen, K. Argüelles, C. Ashida, Y. Athanasiadou, S. Axani, S.N. Babu, R. Bai, X. Baricevic, M. Barwick, S.W. Bash, S. Basu, V. Bay, R. Beatty, J.J. Becker Tjus, J. Beise, J. Bellenghi, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Blaufuss, E. Bloom, L. Blot, S. Bontempo, F. Book Motzkin, J.Y. Boscolo Meneguolo, C. Böser, S. Botner, O. Böttcher, J. Braun, J. Brinson, B. Brisson-Tsavoussis, Z. Brostean-Kaiser, J. Brusa, L. Burley, R.T. Butterfield, D. Campana, M.A. Caracas, I. Carloni, K. Carpio, J. Chattopadhyay, S. Chau, N. Chen, Z. Chirkin, D. Choi, S. Clark, B.A. Cochling, C. Coleman, A. Coleman, P. Collin, G.H. Connolly, A. Conrad, J.M. Corley, R. Cowen, D.F. De Clercq, C. DeLaunay, J.J. Delgado, D. Deng, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. DeYoung, T. Diaz, A. Díaz-Vélez, J.C. Dierichs, P. Dittmer, M. Domi, A. Draper, L. Dujmovic, H. Durnford, D. Dutta, K. DuVernois, M.A. Ehrhardt, T. Eidenschink, L. Eimer, A. Eller, P. Ellinger, E. El Mentawi, S. Elsässer, D. Engel, R. Erpenbeck, H. Evans, J. Evenson, P.A. Fan, K.L. Fang, K. Farrag, K. Fazely, A.R. Fedynitch, A. Feigl, N. Fiedlschuster, S. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Fukami, S. Fürst, P. Gallagher, J. Ganster, E. Garcia, A. Garcia, M. Garg, G. Genton, E. Gerhardt, L. Ghadimi, A. Girard-Carillo, C. Glaser, C. Glüsenkamp, T. Gonzalez, J.G. Goswami, S. Granados, A. Grant, D. Gray, S.J. Griffin, S. Griswold, S. Groth, K.M. Gruchot, K. Guevel, D. Günther, C. Gutjahr, P. Ha, C. Haack, C. Hallgren, A. Halve, L. Halzen, F. Hamacher, L. Hamdaoui, H. Hardy, A. Hayes, W. Ha Minh, M. Handt, M. Hanson, K. Hardin, J. Harnisch, A.A. Hatch, P. Haungs, A. Häußler, J. Helbing, K. Hellrung, J. Hermannsgabner, J. Heuermann, L. Heyer, N. Hickford, S. Hidvegi, A. Hill, C. Hill, G.C. Hmaid, R. Hoffman, K.D. 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 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 Dept. of Physics Simon Fraser University BurnabyBCV5A 1S6 Canada 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 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 State University ColumbusOH43210 United States Dept. of Physics Center for Cosmology and Astro-Particle Physics Ohio State University ColumbusOH43210 United States Niels Bohr Institute University of Copenhagen CopenhagenDK-2100 Denmark Dept. of Physics TU Dortmund University DortmundD-44221 Germany Dept. of Physics and

We analyzed the 7.92×1011 cosmic-ray-induced muon events collected by the IceCube Neutrino Observatory from May 13, 2011, when the fully constructed experiment started to take data, to May 12, 2023. This dataset provides an up-to-date cosmic-ray arrival direction distribution in the Southern Hemisphere with unprecedented statistical accuracy covering more than a full period length of a solar cycle. Improvements in Monte Carlo event simulation and better handling of year-to-year differences in data processing significantly reduce systematic uncertainties below the level of statistical fluctuations compared to the previously published results. We confirm the observation of a change in the angular structure of the cosmic-ray anisotropy between 10 TeV and 1 PeV, more specifically in the 100–300 TeV energy range. For the first time, we analyzed the angular power spectrum at different energies. The observed variations of the power spectra with energy suggest relatively reduced large-scale features at high energy compared to those of medium and small scales. The large volume of data enhances the statistical significance at higher energies, up to the PeV scale, and smaller angular scales, down to approximately 6◦ compared to previous findings. © 2024, CC BY.

关键词： cosmology

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Optimization of the optical array geometry for IceCube-Gen2 37

Optimization of the optical array geometry for IceCube-Gen2

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37th International Cosmic Ray Conference, ICRC 2021

作者： Abbasi, R. Ackermann, M. Adams, J. Aguilar, J.A. Ahlers, M. Ahrens, M. Alispach, C. Allison, P. Alves, A.A. Amin, N.M. An, R. Andeen, K. Anderson, T. Anton, G. Argüelles, C. Arlen, T.C. Ashida, Y. Axani, S. Bai, X. Balagopal, A.V. Barbano, A. Bartos, I. Barwick, S.W. Bastian, B. Basu, V. Baur, S. Bay, R. Beatty, J.J. Becker, K.-H. Becker Tjus, J. Bellenghi, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Binder, G. Bindig, D. Bishop, A. Blaufuss, E. Blot, S. Boddenberg, M. Bohmer, M. Bontempo, F. Borowka, J. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Bradascio, F. Braun, J. Bron, S. Brostean-Kaiser, J. Browne, S. Burgman, A. Burley, R.T. Busse, R.S. Campana, M.A. Carnie-Bronca, E.G. Cataldo, M. Chen, C. Chirkin, D. Choi, K. Clark, B.A. Clark, K. Clark, R. Classen, L. Coleman, A. Collin, G.H. Connolly, A. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Cross, R. Dappen, C. Dave, P. Deaconu, C. De Clercq, C. De Kockere, S. DeLaunay, J.J. Dembinski, H. Deoskar, K. De Ridder, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. de With, M. DeYoung, T. Dharani, S. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Dujmovic, H. Dunkman, M. DuVernois, M.A. Dvorak, E. Ehrhardt, T. Eller, P. Engel, R. Erpenbeck, H. Evans, J. Evans, J.J. Evenson, P.A. Fan, K.L. Farrag, K. Fazely, A.R. Fiedlschuster, S. Fienberg, A.T. Filimonov, K. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Friedman, E. Fritz, A. Fürst, P. Gaisser, T.K. Gallagher, J. Ganster, E. Garcia, A. Garrappa, S. Gartner, A. Gerhardt, L. Gernhaeuser, R. Ghadimi, A. Giri, P. Glaser, C. Glauch, T. Glüsenkamp, T. Goldschmidt, A. Gonzalez, J.G. Goswami, S. Grant, D. Grégoire, T. Griswold, S. Gündüz, M. Günther, C. Haack, C. Hallgren, A. Halliday, R. Hallmann, S. Halve, L. Halzen, F. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Haugen, J. Haungs, A. Hauser, S. Hebecker, D. Heinen, D. Helbing, K. Hendricks, B. Henningsen, F. Hettinger, E.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 Institute for Global Prominent Research 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 State Univers

IceCube-Gen2 is a planned extension of the IceCube Neutrino Observatory at the South Pole designed to study the high-energy neutrino sky from TeV to EeV energies with a five times better point source sensitivity than the current IceCube detector. This is achieved by deploying 120 new strings with attached optical sensors in a pattern around IceCube that features considerably larger distances between individual strings than the ∼125 m for the existing detector. Here, we present the results of an optimization study searching for the best point source sensitivity while varying the IceCube-Gen2 string spacing between 150 m and 350 m. © Copyright owned by the author(s).

关键词： Tellurium compounds

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Performance of the low-latency GstLAL inspiral search towards LIGO, Virgo, and KAGRA’s fourth observing run

arXiv

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arXiv 2023年

作者： Ewing, Becca Huxford, Rachael Singh, Divya Tsukada, Leo Hanna, Chad Huang, Yun-Jing Joshi, Prathamesh Li, Alvin K.Y. Magee, Ryan Messick, Cody Pace, Alex Ray, Anarya Sachdev, Surabhi Sakon, Shio Tapia, Ron Adhicary, Shomik Baral, Pratyusava Baylor, Amanda Cannon, Kipp Caudill, Sarah Chaudhary, Sushant Sharma Coughlin, Michael W. Cousins, Bryce Creighton, Jolien D.E. Essick, Reed Fong, Heather George, Richard N. Godwin, Patrick Harada, Reiko Kennington, James Kuwahara, Soichiro Meacher, Duncan Morisaki, Soichiro Mukherjee, Debnandini Niu, Wanting Posnansky, Cort Toivonen, Andrew Tsutsui, Takuya Ueno, Koh Viets, Aaron Wade, Leslie Wade, Madeline Waratkar, Gaurav Department of Physics The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Astronomy and Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States LIGO Laboratory California Institute of Technology PasadenaCA91125 United States MIT Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Leonard E. Parker Center for Gravitation Cosmology and Astrophysics University of Wisconsin-Milwaukee MilwaukeeWI53201 United States School of Physics Georgia Institute of Technology AtlantaGA30332 United States RESCEU The University of Tokyo Tokyo113-0033 Japan Department of Physics University of Massachusetts DartmouthMA02747 United States Center for Scientific Computing and Data Science Research University of Massachusetts DartmouthMA02747 United States Institute of Multi-messenger Astrophysics and Cosmology Missouri University of Science and Technology Physics Building 1315 N. Pine St. RollaMO65409 United States School of Physics and Astronomy University of Minnesota MinneapolisMN55455 United States Department of Physics University of Illinois UrbanaIL61801 United States Canadian Institute for Theoretical Astrophysics 60 St George St TorontoONM5S 3H8 Canada Graduate School of Science The University of Tokyo Tokyo113-0033 Japan Center for Gravitational Physics University of Texas at Austin AustinTX78712 United States LIGO Laboratory California Institute of Technology MS 100-36 PasadenaCA91125 United States Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8582 Japan NASA Marshall Space Flight Center HuntsvilleAL35811 United States Center f

GstLAL is a stream-based matched-filtering search pipeline aiming at the prompt discovery of gravitational waves from compact binary coalescences such as the mergers of black holes and neutron stars. Over the past three observation runs by the LIGO, Virgo, and KAGRA (LVK) collaboration, the GstLAL search pipeline has participated in several tens of gravitational wave discoveries. The fourth observing run (O4) is set to begin in May 2023 and is expected to see the discovery of many new and interesting gravitational wave signals which will inform our understanding of astrophysics and cosmology. We describe the current configuration of the GstLAL low-latency search and show its readiness for the upcoming observation run by presenting its performance on a mock data challenge. The mock data challenge includes 40 days of LIGO Hanford, LIGO Livingston, and Virgo strain data along with an injection campaign in order to fully characterize the performance of the search. We find an improved performance in terms of detection rate and significance estimation as compared to that observed in the O3 online analysis. The improvements are attributed to several incremental advances in the likelihood ratio ranking statistic computation and the method of background estimation. © 2023, CC BY.

关键词： Gravity waves

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AT2023lli: A Tidal Disruption Event with Prominent Optical Early Bump and Delayed Episodic X-ray Emission

arXiv

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arXiv 2024年

作者： Huang, Shifeng Jiang, Ning Zhu, Jiazheng Wang, Yibo Wang, Tinggui Wang, Shan-Qin Gan, Wen-Pei Liang, En-Wei Qin, Yu-Jing Lin, Zheyu Xu, Lin-Na Cai, Min-Xuan Jiang, Ji-An Kong, Xu Li, Jiaxun Li, Long Wang, Jian-Guo Xu, Ze-Lin Xue, Yongquan Yuan, Ye-Fei Cheng, Jingquan Fan, Lulu Gao, Jie Hu, Lei Hu, Weida Li, Bin Li, Feng Liang, Ming Liu, Hao Liu, Wei Lou, Zheng Luo, Wentao Qian, Yuan Tang, Jinlong Wan, Zhen Wang, Hairen Wang, Jian Yang, Ji Yao, Dazhi Zhang, Hongfei Zhang, Xiaoling Zhao, Wen Zheng, Xianzhong Zhu, Qingfeng Zuo, Yingxi 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 Sciences University of Science and Technology of China Hefei230026 China Institute of Deep Space Sciences Deep Space Exploration Laboratory Hefei230026 China Guangxi Key Laboratory for Relativistic Astrophysics School of Physical Science and Technology Guangxi University Nanning530004 China Nanjing Hopes Technology Co. Ltd. Pukou District Nanjing210000 China Division of Physics Mathematics and Astronomy California Institute of Technology 1200 E California Blvd. PasadenaCA91125 United States National Astronomical Observatory of Japan National Institutes of Natural Sciences Tokyo181-8588 Japan Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Kunming650011 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei230026 China McWilliams Center for Cosmology Department of Physics Carnegie Mellon University 5000 Forbes Ave PittsburghPA15213 United States Department of Physics University of California Santa Barbara Santa BarbaraCA93106 United States 950 N Cherry Ave TucsonAZ85726 United States Institute of Optics and Electronics Chinese Academy of Sciences Chengdu610209 China

High-cadence, multiwavelength observations have continuously revealed the diversity of tidal disruption events (TDEs), thus greatly advancing our knowledge and understanding of TDEs. In this work, we conducted an intensive optical-UV and X-ray follow-up campaign of TDE AT2023lli, and found a remarkable month-long bump in its UV/optical light curve nearly two months prior to maximum brightness. The bump represents the longest separation time from the main peak among known TDEs to date. The main UV/optical outburst declines as t−4.10, making it one of the fastest decaying optically selected TDEs. Furthermore, we detected sporadic X-ray emission 30 days after the UV/optical peak, accompanied by a reduction in the period of inactivity. It is proposed that the UV/optical bump could be caused by the self-intersection of the stream debris, whereas the primary peak is generated by the reprocessed emission of the accretion process. In addition, our results suggest that episodic X-ray radiation during the initial phase of decline may be due to the patched obscurer surrounding the accretion disk, a phenomenon associated with the inhomogeneous reprocessing process. The double TDE scenario, in which two stars are disrupted in sequence, is also a possible explanation for producing the observed early bump and main peak. We anticipate that the multicolor light curves of TDEs, especially in the very early stages, and the underlying physics can be better understood in the near future with the assistance of dedicated surveys such as the deep high-cadence survey of the 2.5-meter Wide Field Survey Telescope (WFST). © 2024, CC BY.

关键词： Luminance

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Carbon and Iron Deficiencies in Quiescent Galaxies at z = 1 − 3 from JWST-SUSPENSE: Implications for the Formation Histories of Massive Galaxies

arXiv

引用

arXiv 2024年

作者： Beverage, Aliza G. Slob, Martje Kriek, Mariska Conroy, Charlie Barro, Guillermo Bezanson, Rachel Brammer, Gabriel Cheng, Chloe M. de Graaff, Anna Förster Schreiber, Natascha M. Franx, Marijn Lorenz, Brian Mancera Piña, Pavel E. Marchesini, Danilo Muzzin, Adam Newman, Andrew B. Price, Sedona H. Shapley, Alice E. Stefanon, Mauro Suess, Katherine A. van Dokkum, Pieter Weinberg, David Weisz, Daniel R. Department of Astronomy University of California BerkeleyCA94720 United States Leiden Observatory Leiden University P.O. Box 9513 Leiden2300 RA Netherlands Center for Astrophysics Harvard & Smithsonian CambridgeMA02138 United States Department of Physics University of the Pacific StocktonCA90340 United States Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen NDK2200 Denmark Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Max-Planck-Institut für extraterrestrische Physik Giessenbachstrasse 1 GarchingD-85748 Germany Department of Physics & Astronomy Tufts University MA02155 United States Department of Physics and Astronomy York University 4700 Keele Street ON TorontoONMJ3 1P3 Canada Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States Department of Physics & Astronomy University of California Los AngelesCA90095 United States Departament d’Astronomia i Astrofìsica Universitat de València C. Dr. Moliner 50 Burjassot ValènciaE-46100 Spain Spain Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States Astronomy Department Yale University 52 Hillhouse Ave New HavenCT06511 United States The Department of Astronomy Center of Cosmology and AstroParticle Physics The Ohio State University ColumbusOH43210 United States

We present the stellar metallicities and multi-element abundances (C, Mg, Si, Ca, Ti, Cr, and Fe) of 15 massive (log M/M☉ = 10.2 − 11.2) quiescent galaxies at z = 1 − 3, derived from ultradeep JWSTSUSPENSE spectra. Compared to quiescent galaxies at z ∼ 0, these galaxies exhibit a deficiency of 0.26±0.04 dex in [C/H], 0.16±0.03 dex in [Fe/H], and 0.07±0.04 dex in [Mg/H], implying rapid formation and quenching before significant enrichment from asymptotic giant branch stars and Type Ia supernovae. Additionally, we find that galaxies forming at higher redshift consistently show higher [Mg/Fe] and lower [Fe/H] and [Mg/H], regardless of their observed redshift. The evolution in [Fe/H] and [C/H] is therefore primarily driven by lower-redshift samples naturally including galaxies with longer star-formation timescales. In contrast, the lower [Mg/H] likely reflects earlier-forming galaxies expelling larger gas reservoirs during their quenching phase. Consequently, the mass-metallicity relation, primarily reflecting [Mg/H], is somewhat lower at z = 1 − 3 compared to the lower redshift relation. Finally, we compare our results to standard stellar population modeling approaches employing solar abundance patterns and non-parametric star-formation histories (using Prospector). Our SSP-equivalent ages agree with the mass-weighted ages from Prospector, while the metallicities disagree significantly. Nonetheless, the metallicities better reflect [Fe/H] than total [Z/H]. We also find that star-formation timescales inferred from elemental abundances are significantly shorter than those from Prospector, and we discuss the resulting implications for the early formation of massive galaxies. Copyright © 2024, The Authors. All rights reserved.

关键词： Quenching

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Simulation and sensitivities for a phased IceCube-Gen2 deployment 37

Simulation and sensitivities for a phased IceCube-Gen2 deplo...

引用

37th International Cosmic Ray Conference, ICRC 2021

作者： Abbasi, R. Ackermann, M. Adams, J. Aguilar, J.A. Ahlers, M. Ahrens, M. Alispach, C. Allison, P. Alves, A.A. Amin, N.M. An, R. Andeen, K. Anderson, T. Anton, G. Argüelles, C. Arlen, T.C. Ashida, Y. Axani, S. Bai, X. Balagopal, A.V. Barbano, A. Bartos, I. Barwick, S.W. Bastian, B. Basu, V. Baur, S. Bay, R. Beatty, J.J. Becker, K.-H. Becker Tjus, J. Bellenghi, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Binder, G. Bindig, D. Bishop, A. Blaufuss, E. Blot, S. Boddenberg, M. Bohmer, M. Bontempo, F. Borowka, J. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Bradascio, F. Braun, J. Bron, S. Brostean-Kaiser, J. Browne, S. Burgman, A. Burley, R.T. Busse, R.S. Campana, M.A. Carnie-Bronca, E.G. Cataldo, M. Chen, C. Chirkin, D. Choi, K. Clark, B.A. Clark, K. Clark, R. Classen, L. Coleman, A. Collin, G.H. Connolly, A. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Cross, R. Dappen, C. Dave, P. Deaconu, C. De Clercq, C. De Kockere, S. DeLaunay, J.J. Dembinski, H. Deoskar, K. De Ridder, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. de With, M. DeYoung, T. Dharani, S. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Dujmovic, H. Dunkman, M. DuVernois, M.A. Dvorak, E. Ehrhardt, T. Eller, P. Engel, R. Erpenbeck, H. Evans, J. Evans, J.J. Evenson, P.A. Fan, K.L. Farrag, K. Fazely, A.R. Fiedlschuster, S. Fienberg, A.T. Filimonov, K. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Friedman, E. Fritz, A. Fürst, P. Gaisser, T.K. Gallagher, J. Ganster, E. Garcia, A. Garrappa, S. Gartner, A. Gerhardt, L. Gernhaeuser, R. Ghadimi, A. Giri, P. Glaser, C. Glauch, T. Glüsenkamp, T. Goldschmidt, A. Gonzalez, J.G. Goswami, S. Grant, D. Grégoire, T. Griswold, S. Gündüz, M. Günther, C. Haack, C. Hallgren, A. Halliday, R. Hallmann, S. Halve, L. Halzen, F. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Haugen, J. Haungs, A. Hauser, S. Hebecker, D. Heinen, D. Helbing, K. Hendricks, B. Henningsen, F. 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 Institute for Global Prominent Research 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 State Univers

The IceCube Neutrino Observatory opened the window on high-energy neutrino astronomy by confirming the existence of PeV astrophysical neutrinos and identifying the first compelling astrophysical neutrino source in the blazar TXS0506+056. Planning is underway to build an enlarged detector, IceCube-Gen2, which will extend measurements to higher energies, increase the rate of observed cosmic neutrinos and provide improved prospects for detecting fainter sources. IceCube-Gen2 is planned to have an extended in-ice optical array, a radio array at shallower depths for detecting ultra-high-energy (>100 PeV) neutrinos, and a surface component studying cosmic rays. In this contribution, we will discuss the simulation of the in-ice optical component of the baseline design of the IceCube-Gen2 detector, which foresees the deployment of an additional ∼ 120 new detection strings to the existing 86 in IceCube over ∼ 7 Antarctic summer seasons. Motivated by the phased construction plan for IceCube-Gen2, we discuss how the reconstruction capabilities and sensitivities of the instrument are expected to progress throughout its deployment. © Copyright owned by the author(s).

关键词： Cosmic rays

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Search for dark matter from the center of the Earth with ten years of IceCube data

arXiv

引用

arXiv 2024年

作者： Abbasi, R. Ackermann, M. Adams, J. Agarwalla, S.K. Aguilar, J.A. Ahlers, M. Alameddine, J.M. Amin, N.M. Andeen, K. Argüelles, C. Ashida, Y. Athanasiadou, S. Axani, S.N. Babu, R. Bai, X. Balagopal, A.V. Baricevic, M. Barwick, S.W. Bash, S. Basu, V. Bay, R. Beatty, J.J. Tjus, J. Becker Beise, J. Bellenghi, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Blaufuss, E. Bloom, L. Blot, S. Bontempo, F. Motzkin, J.Y. Book Meneguolo, C. Boscolo Böser, S. Botner, O. Böttcher, J. Braun, J. Brinson, B. Brisson-Tsavoussis, Z. Brostean-Kaiser, J. Brusa, L. Burley, R.T. Butterfield, D. Campana, M.A. Caracas, I. Carloni, K. Carpio, J. Chattopadhyay, S. Chau, N. Chen, Z. Chirkin, D. Choi, S. Clark, B.A. Coleman, A. Coleman, P. Collin, G.H. Connolly, A. Conrad, J.M. Corley, R. Cowen, D.F. De Clercq, C. DeLaunay, J.J. Delgado, D. Deng, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. DeYoung, T. Diaz, A. Díaz-Vélez, J.C. Dierichs, P. Dittmer, M. Domi, A. Draper, L. Dujmovic, H. Durnford, D. Dutta, K. Du Vernois, M.A. Ehrhardt, T. Eidenschink, L. Eimer, A. Eller, P. Ellinger, E. El Mentawi, S. Elsässer, D. Engel, R. Erpenbeck, H. Esmail, W. Evans, J. Evenson, P.A. Fan, K.L. Fang, K. Farrag, K. Fazely, A.R. Fedynitch, A. Feigl, N. Fiedlschuster, S. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Fukami, S. Fürst, P. Gallagher, J. Ganster, E. Garcia, A. Garcia, M. Garg, G. Genton, E. Gerhardt, L. Ghadimi, A. Girard-Carillo, C. Glaser, C. Glüsenkamp, T. Gonzalez, J.G. Goswami, S. Granados, A. Grant, D. Gray, S.J. Griffin, S. Griswold, S. Groth, K.M. Guevel, D. Günther, C. Gutjahr, P. Ha, C. Haack, C. Hallgren, A. Halve, L. Halzen, F. Hamacher, L. Hamdaoui, H. Ha Minh, M. Handt, M. Hanson, K. Hardin, J. Harnisch, A.A. Hatch, P. Haungs, A. Häußler, J. Helbing, K. Hellrung, J. Hermannsgabner, J. Heuermann, L. Heyer, N. Hickford, S. Hidvegi, A. Hill, C. Hill, G.C. Hmaid, R. Hoffman, K.D. Hori, S. Hoshina, K. Hostert, M. 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 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 Dept. of Physics Simon Fraser University BurnabyBCV5A 1S6 Canada 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 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 State University ColumbusOH43210 United States Dept. of Physics Center for Cosmology and Astro-Particle Physics Ohio State University ColumbusOH43210 United States Niels Bohr Institute University of Copenhagen CopenhagenDK-2100 Denmark Dept. of Physics TU Dortmund University DortmundD-44221 Germany Dept. of Physics and

The nature of dark matter remains unresolved in fundamental physics. Weakly Interacting Massive particles (WIMPs), which could explain the nature of dark matter, can be captured by celestial bodies like the Sun or Earth, leading to enhanced self-annihilation into Standard Model particles including neutrinos detectable by neutrino telescopes such as the IceCube Neutrino Observatory. This article presents a search for muon neutrinos from the center of the Earth performed with 10 years of IceCube data using a track-like event selection. We considered a number of WIMP annihilation channels (χχ → τ+τ−/W+W−/bb¯) and masses ranging from 10 GeV to 10 TeV. No significant excess over background due to a dark matter signal was found while the most significant result corresponds to the annihilation channel χχ → bb¯ for the mass mχ = 250 GeV with a post-trial significance of 1.06σ. Our results are competitive with previous such searches and direct detection experiments. Our upper limits on the spin-independent WIMP scattering are world-leading among neutrino telescopes for WIMP masses mχ > 100 GeV. © 2024, CC BY.

关键词： Neutrons

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