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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

The IceCube Neutrino Observatory has discovered a diffuse astrophysical flux up to 10 PeV and is now planning a large extension with IceCube-Gen2, including an optical array and a large radio array at shallow depth [1]. Neutrino searches for energies >100 PeV are best done with such shallow radio detectors like the Askaryan Radio Array (ARA) or similar (buried as deep as 200 meters below the surface) as they are cheaper to deploy. This poster explores the potential of opportunistically burying radio antennas within the planned IceCube-Gen2 detector volume (between 1350 meters and 2600 meters below the surface). A hybrid detection of events in optical and radio could substantially improve the uncertainty of neutrino cascade direction as radio signals do not scatter in ice. We show the first results of simulating neutrinos from an astrophysical and a cosmogenic flux interacting with 9760 ARA-style vertically polarized radio antennas distributed evenly across 122 strings. © Copyright owned by the author(s).

关键词： Neutrons

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Search for neutrino doublets and triplets using 11.4 years of IceCube data

arXiv

引用

arXiv 2025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. 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. DuVernois, M.A. Ehrhardt, T. Eidenschink, L. Eimer, A. Eller, P. Ellinger, E. Mentawi, S. El 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. Minh, M. Ha 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. 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 report a search for high-energy astrophysical neutrino multiplets, detections of multiple neutrino clusters in the same direction within 30 days, based on an analysis of 11.4 years of IceCube data. A new search method optimized for transient neutrino emission with a monthly time scale is employed, providing a higher sensitivity to neutrino fluxes. This result is sensitive to neutrino transient emission, reaching per-flavor flux of approximately 10−10 erg cm−2 sec−1 from the Northern sky in the energy range E 50 TeV. The number of doublets and triplets identified in this search is compatible with the atmospheric background hypothesis, which leads us to set limits on the nature of neutrino transient sources with emission timescales of one month. © 2025, CC BY.

关键词： Electromagnetic transients

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IceCube Search for Neutrino Emission from X-ray Bright Seyfert Galaxies

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. Ausborm, L. Axani, S.N. Bai, X. Balagopal, A.V. Baricevic, M. Barwick, S.W. Bash, S. Basu, V. Bay, R. Beatty, J.J. Becker Tjus, J. Beise, J. Bellenghi, C. Benning, 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. 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. Collin, G.H. Connolly, A. Conrad, J.M. Coppin, P. Corley, R. Correa, P. Cowen, D.F. Dave, P. 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. 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. Glauch, T. Glüsenkamp, T. Gonzalez, J.G. Goswami, S. Granados, A. Grant, D. Gray, S.J. Gries, O. Griffin, S. Griswold, S. Groth, K.M. Günther, C. Gutjahr, P. Ha, C. Haack, C. Hallgren, A. Halve, L. Halzen, F. 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. Hoffman, K.D. Hori, S. Hoshina, K. Hostert, M. Hou, W. 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 Science Hall Rm 108 502 Yates St. 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 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 Astro

The recent IceCube detection of TeV neutrino emission from the nearby active galaxy NGC 1068 suggests that active galactic nuclei (AGN) could make a sizable contribution to the diffuse flux of astrophysical neutrinos. The absence of TeV γ-rays from NGC 1068 indicates neutrino production in the vicinity of the supermassive black hole, where the high radiation density leads to γ-ray attenuation. Therefore, any potential neutrino emission from similar sources is not expected to correlate with high-energy γ-rays. Disk-corona models predict neutrino emission from Seyfert galaxies to correlate with keV X-rays, as they are tracers of coronal activity. Using through-going track events from the Northern Sky recorded by IceCube between 2011 and 2021, we report results from a search for individual and aggregated neutrino signals from 27 additional Seyfert galaxies that are contained in the BAT AGN Spectroscopic Survey (BASS). Besides the generic single power-law, we evaluate the spectra predicted by the disk-corona model. Assuming all sources to be intrinsically similar to NGC 1068, our findings constrain the collective neutrino emission from X-ray bright Seyfert galaxies in the Northern Hemisphere, but, at the same time, show excesses of neutrinos that could be associated with the objects NGC 4151 and CGCG 420-015. These excesses result in a 2.7σ significance with respect to background expectations. Copyright © 2024, The Authors. All rights reserved.

关键词： Active Galactic Nuclei

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Sensitivity studies for the IceCube-Gen2 radio array 37

Sensitivity studies for the IceCube-Gen2 radio array

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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. 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 at the South Pole has measured the diffuse astrophysical neutrino flux up to ∼PeV energies and is starting to identify first point source candidates. The next generation facility, IceCube-Gen2, aims at extending the accessible energy range to EeV in order to measure the continuation of the astrophysical spectrum, to identify neutrino sources, and to search for a cosmogenic neutrino flux. As part of IceCube-Gen2, a radio array is foreseen that is sensitive to detect Askaryan emission of neutrinos beyond ∼30 PeV. Surface and deep antenna stations have different benefits in terms of effective area, resolution, and the capability to reject backgrounds from cosmic-ray air showers and may be combined to reach the best sensitivity. The optimal detector configuration is still to be identified. This contribution presents the full-array simulation efforts for a combination of deep and surface antennas, and compares different design options with respect to their sensitivity to fulfill the science goals of IceCube-Gen2. © Copyright owned by the author(s).

关键词： Antennas

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A search for an eV-scale sterile neutrino using improved high-energy νµ event reconstruction in IceCube

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. Ausborm, L. Axani, S.N. Bai, X. Balagopal, A. Baricevic, M. Barwick, S.W. Bash, S. Basu, V. Bay, R. Beatty, J.J. Tjus, J. Becker Beise, J. Bellenghi, C. Benning, 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. 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. Collin, G.H. Connolly, A. Conrad, J.M. Coppin, P. Corley, R. Correa, P. Cowen, D.F. Dave, P. De Clercq, C. DeLaunay, J.J. Delgado, D. Deng, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. Diaz, A. Díaz-Vélez, J.C. Dierichs, P. Dittmer, M. Domi, A. Draper, L. Dujmovic, H. Dutta, K. DuVernois, M.A. Ehrhardt, T. Eidenschink, L. Eimer, A. Eller, P. Ellinger, E. Mentawi, S. El 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. Gries, O. Griffin, S. Griswold, S. Groth, K.M. Günther, C. Gutjahr, P. Ha, C. Haack, C. Hallgren, A. Halve, L. Halzen, F. Hamdaoui, H. Minh, M. Ha 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. Hoffman, K.D. Hori, S. Hoshina, K. Hostert, M. Hou, W. Huber, T. Hultqvist, K. 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 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 Astro

This Letter presents the result of a 3+1 sterile neutrino search using 10.7 years of IceCube data. We analyze atmospheric muon neutrinos that traverse the Earth with energies ranging from 0.5 to 100 TeV, incorporating significant improvements in modeling neutrino flux and detector response compared to earlier studies. Notably, for the first time, we categorize data into starting and through-going events, distinguishing neutrino interactions with vertices inside or outside the instrumented volume, to improve energy resolution. The best-fit point for a 3+1 model is found to be at sin2(2θ24) = 0.16 and ∆m241 = 3.5 eV2, which agrees with previous iterations of this study. The result is consistent with the null hypothesis of no sterile neutrinos with a p-value of 3.1%. Copyright © 2024, The Authors. All rights reserved.

关键词： Neutron flux

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Towards Equitable, Diverse, and Inclusive science collaborations: The Multimessenger Diversity Network 37

Towards Equitable, Diverse, and Inclusive science collaborat...

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37th International Cosmic Ray Conference, ICRC 2021

作者： Bechtol, E. Bechtol, K. BenZvi, S. Bleve, C. Castro, D. Cenko, B. Corlies, L. Furniss, A. Hui, C.M. Kaplan, D.L. Key, J.S. Madsen, J. McNally, F. McLaughlin, M. Mukherjee, R. Ojha, R. Sanders, J. Santander, M. Schlieder, J. Shoemaker, D.H. Vigeland, S. Abbasi, R. Ackermann, M. Adams, J. Aguilar, J.A. Ahlers, M. Ahrens, M. Alispach, C. Alves, A.A. Amin, N.M. An, R. Andeen, K. Anderson, T. Anton, G. Argüelles, C. Ashida, Y. Axani, S. Bai, X. Balagopal V, A. Barbano, A. Barwick, S.W. Bastian, B. Basu, V. Baur, S. Bay, R. Beatty, J.J. Becker, K.-H. Becker Tjus, J. Bellenghi, C. Berley, D. Bernardini, E. Besson, D.Z. Binder, G. Bindig, D. Blaufuss, E. Blot, S. Boddenberg, 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. Chen, C. Chirkin, D. Choi, K. Clark, B.A. Clark, K. Classen, L. Coleman, A. Collin, G.H. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Cross, R. Dappen, C. Dave, P. De Clercq, C. 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. Evenson, P.A. Fan, K.L. 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. Gerhardt, L. Ghadimi, A. 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. Halve, L. Halzen, F. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Haungs, A. Hauser, S. Hebecker, D. Helbing, K. Laboratoire de Physique Subatomique et de Cosmologie Grenoble France Center for Astrophysics Harvard & Smithsonian MA United States NASA Goddard Space Flight Center MD United States AURA/Vera C. Rubin Observatory AZ United States California State University East Bay CA United States NASA Marshall Space Flight Center AL United States University of Wisconsin-Milwaukee WI United States University of Washington BothellWA United States West Virginia University WV United States Barnard College NY United States MIT Kavli Institute for Astrophysics and Space Research MA United States 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 Uni

The Multimessenger Diversity Network (MDN), formed in 2018, extends the basic principle of multimessenger astronomy - that working collaboratively with different approaches enhances understanding and enables previously impossible discoveries - to equity, diversity, and inclusion (EDI) in science research collaborations. With support from the National science Foundation INCLUDES program, the MDN focuses on increasing EDI by sharing knowledge, experiences, training, and resources among representatives from multimessenger science collaborations. Representatives to the MDN become engagement leads in their collaboration, extending the reach of the community of practice. An overview of the MDN structure, lessons learned, and how to join are presented. © Copyright owned by the author(s) under the terms of the Creative Commons.

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New CTEQ global analysis of quantum chromodynamics with high-precision data from the LHC

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Physical Review D 2021年第1期103卷 014013-014013页

作者： Tie-Jiun Hou Jun Gao T. J. Hobbs Keping Xie Sayipjamal Dulat Marco Guzzi Joey Huston Pavel Nadolsky Jon Pumplin Carl Schmidt Ibrahim Sitiwaldi Daniel Stump C.-P. Yuan Department of Physics College of Sciences Northeastern University Shenyang 110819 China INPAC Shanghai Key Laboratory for Particle Physics and Cosmology & School of Physics and Astronomy Shanghai Jiao Tong University Shanghai 200240 China Center for High Energy Physics Peking University Beijing 100871 China Department of Physics Southern Methodist University Dallas Texas 75275-0181 USA Jefferson Lab EIC Center Newport News Virginia 23606 USA PITT PACC Department of Physics and Astronomy University of Pittsburgh Pittsburgh Pennsylvania 15260 USA School of Physics Science and Technology Xinjiang University Urumqi Xinjiang 830046 China Department of Physics Kennesaw State University 370 Paulding Avenue 30144 Kennesaw Georgia 30061 USA Department of Physics and Astronomy Michigan State University East Lansing Michigan 48824 USA

We present the new parton distribution functions (PDFs) from the CTEQ-TEA collaboration, obtained using a wide variety of high-precision Large Hadron Collider (LHC) data, in addition to the combined HERA I+II deep-inelastic scattering dataset, along with the datasets present in the CT14 global QCD analysis. New LHC measurements in single-inclusive jet production with the full rapidity coverage, as well as production of Drell-Yan pairs, top-quark pairs, and high-pT Z bosons, are included to achieve the greatest sensitivity to the PDFs. The parton distributions are determined at next-to-leading order and next-to-next-to-leading order, with each of these PDFs accompanied by error sets determined using the Hessian method. Fast PDF survey techniques, based on the Hessian representation and the Lagrange multiplier method, are used to quantify the preference of each data set to quantities such as αs(mZ), and the gluon and strange quark distributions. We designate the main resulting PDF set as CT18. The ATLAS 7 TeV precision W/Z data are not included in CT18, due to their tension with other datasets in the global fit. Alternate PDF sets are generated including the ATLAS precision 7 TeV W/Z data (CT18A), a new scale choice for low-x DIS data (CT18X), or all of the above with a slightly higher choice for the charm mass (CT18Z). Theoretical calculations of standard candle cross sections at the LHC (such as the gg fusion Higgs boson cross section) are presented.

关键词： Electroweak interaction particle phenomena Quantum chromodynamics W & Z bosons Charm quark Higgs bosons Strange quark Top quark

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Accurately Estimating Redshifts from CSST Slitless Spectroscopic Survey using Deep Learning

arXiv

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arXiv 2024年

作者： Zhou, Xingchen Gong, Yan Zhang, Xin Li, Nan Meng, Xian-Min Chen, Xuelei Wen, Run Han, Yunkun Zou, Hu Zheng, Xian Zhong Yang, Xiaohu Guo, Hong Zhang, Pengjie National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Beijing100101 China Science Center for China Space Station Telescope National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Beijing100101 China University of Chinese Academy of Sciences Beijing100049 China Centre for High Energy Physiscs Peking University Beijing100871 China Purple Mountain Observatory Chinese Academy of Sciences 10 Yuanhua Road Nanjing210023 China School of Astronomy and Space Sciences University of Science and Technology of China Hefei230026 China Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Department of Astronomy School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Tsung-Dao Lee Institute Key Laboratory for Particle Physics Astrophysics and Cosmology Ministry of Education Shanghai201210 China Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China

Chinese Space Station Telescope (CSST) has the capability to conduct slitless spectroscopic survey simultaneously with photometric survey. The spectroscopic survey will measure slitless spectra, potentially providing more accurate estimations of galaxy properties, particularly redshifts, compared to using broadband photometry. CSST relies on these accurate redshifts to perform baryon acoustic oscilliation (BAO) and other probes to constrain the cosmological parameters. However, due to low resolution and signal-to-noise ratio of slitless spectra, measurement of redshifts is significantly challenging. In this study, we employ a Bayesian neural network (BNN) to assess the accuracy of redshift estimations from slitless spectra anticipated to be observed by CSST. The simulation of slitless spectra is based on real observational data from the early data release of the Dark Energy Spectroscopic Instrument (DESI-EDR) and the 16th data release of the Baryon Oscillation Spectroscopic Survey (BOSS-DR16), combined with the 9th data release of the DESI Legacy Survey (DESI LS DR9). The BNN is constructed employing transfer learning technique, by appending two Bayesian layers after a convolutional neural network (CNN), leveraging the features learned from the slitless spectra and corresponding redshifts. Our network can provide redshift estimates along with corresponding uncertainties, achieving an accuracy of σNMAD = 0.00063, outlier percentage η = 0.92% and weighted mean uncertainty E̅ = 0.00228. These results successfully fulfill the requirement of σNMAD © 2024, CC0.

关键词： Signal to noise ratio

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Search for Heavy Neutral Leptons with IceCube DeepCore

arXiv

引用

arXiv 2025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. 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. 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. Mentawi, S.El. 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. Minh, M.Ha. 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 observation of neutrino oscillations has established that neutrinos have non-zero masses. This phenomenon is not explained by the Standard Model of particle physics, but one viable explanation to this dilemma involves the existence of heavy neutral leptons in the form of right-handed neutrinos. This work presents the first search for heavy neutral leptons with the IceCube Neutrino Observatory. The standard three flavor neutrino model is extended by adding a fourth GeV-scale mass state allowing mixing with the τ sector through the parameter |Uτ4|2. The analysis is performed by searching for signatures of heavy neutral leptons that are directly produced via up-scattering of atmospheric ντ’s inside the IceCube detection volume. Three heavy neutral lepton mass values, m4, of 0.3 GeV, 0.6 GeV, and 1.0 GeV are tested using ten years of data, collected between 2011 and 2021. No significant signal of heavy neutral leptons is observed for any of the tested masses. The resulting constraints for the mixing parameter are |Uτ4|2 2 2 © 2025, CC BY.

关键词： Neutrons

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Emulating the impact of additional proton–proton interactions in the ATLAS simulation by presampling sets of inelastic Monte Carlo events

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Computing and Software for Big science 2022年第1期6卷 1-35页

作者： Aad, G. Abbott, B. Abbott, D.C. Abud, A. Abed Abeling, K. Abhayasinghe, D.K. Abidi, S.H. AbouZeid, O.S. Abraham, N.L. Abramowicz, H. Abreu, H. Abulaiti, Y. Hoffman, A. C. Abusleme Acharya, B.S. Achkar, B. Adam, L. Bourdarios, C. Adam Adamczyk, L. Adamek, L. Adelman, J. Adiguzel, A. Adorni, S. Adye, T. Affolder, A.A. Afik, Y. Agapopoulou, C. Agaras, M.N. Aggarwal, A. Agheorghiesei, C. Aguilar-Saavedra, J.A. Ahmad, A. Ahmadov, F. Ahmed, W.S. Ai, X. Aielli, G. Akatsuka, S. Akbiyik, M. Åkesson, T.P.A. Akilli, E. Akimov, A.V. Khoury, K. Al Alberghi, G.L. Albert, J. Verzini, M. J. Alconada Alderweireldt, S. Aleksa, M. Aleksandrov, I.N. Alexa, C. Alexopoulos, T. Alfonsi, A. Alfonsi, F. Alhroob, M. Ali, B. Ali, S. Aliev, M. Alimonti, G. Allaire, C. Allbrooke, B.M.M. Allport, P.P. Aloisio, A. Alonso, F. Alpigiani, C. Camelia, E. Alunno Estevez, M. Alvarez Alviggi, M.G. Coutinho, Y. Amaral Ambler, A. Ambroz, L. Amelung, C. Amidei, D. Santos, S. P. Amor Dos Amoroso, S. Amrouche, C.S. Anastopoulos, C. Andari, N. Andeen, T. Anders, J.K. Andrean, S.Y. Andreazza, A. Andrei, V. Anelli, C.R. Angelidakis, S. Angerami, A. Anisenkov, A.V. Annovi, A. Antel, C. Anthony, M.T. Antipov, E. Antonelli, M. Antrim, D.J.A. Anulli, F. Aoki, M. Pozo, J. A. Aparisi Aparo, M.A. Bella, L. Aperio Aranzabal, N. Ferraz, V. Araujo Arcangeletti, C. Arce, A.T.H. Arguin, J.-F. Argyropoulos, S. Arling, J.-H. Armbruster, A.J. Armstrong, A. Arnaez, O. Arnold, H. Tame, Z. P. Arrubarrena Artoni, G. Asada, H. Asai, K. Asai, S. Asbah, N.A. Asimakopoulou, E.M. Asquith, L. Assahsah, J. Assamagan, K. Astalos, R. Atkin, R.J. Atkinson, M. Atlay, N.B. Atmani, H. Atmasiddha, P.A. Augsten, K. Austrup, V.A. Avolio, G. Ayoub, M.K. Azuelos, G. Babal, D. Bachacou, H. Bachas, K. Backman, F. Bagnaia, P. Bahrasemani, H. Bailey, A.J. Bailey, V.R. Baines, J.T. Bakalis, C. Baker, O.K. Bakker, P.J. Bakos, E. Gupta, D. Bakshi Balaji, S. Balasubramanian, R. Baldin, E.M. Balek, P. Balli, F. Balunas, W.K. Balz, J. Banas, E. Bandieramonte, M. Bandyopadhyay, A. Barak, L. Barbe, W.M. Ba Department of Physics University of Adelaide Adelaide Australia Physics Department SUNY Albany Albany NY United States Department of Physics University of Alberta Edmonton AB Canada Department of Physics Ankara University Ankara Turkey Istanbul Aydin University Application and Research Center for Advanced Studies Istanbul Turkey Division of Physics TOBB University of Economics and Technology Ankara Turkey LAPP Univ. Savoie Mont Blanc CNRS/IN2P3 Annecy France High Energy Physics Division Argonne National Laboratory Argonne IL United States Department of Physics University of Arizona Tucson AZ United States Department of Physics University of Texas at Arlington Arlington TX United States Physics Department National and Kapodistrian University of Athens Athens Greece Physics Department National Technical University of Athens Zografou Greece Department of Physics University of Texas at Austin Austin TX United States Bahcesehir University Faculty of Engineering and Natural Sciences Istanbul Turkey Istanbul Bilgi University Faculty of Engineering and Natural Sciences Istanbul Turkey Department of Physics Bogazici University Istanbul Turkey Department of Physics Engineering Gaziantep University Gaziantep Turkey Institute of Physics Azerbaijan Academy of Sciences Baku Azerbaijan Institut de Física d’Altes Energies (IFAE) Barcelona Institute of Science and Technology Barcelona Spain Institute of High Energy Physics Chinese Academy of Sciences Beijing China Physics Department Tsinghua University Beijing China Department of Physics Nanjing University Nanjing China University of Chinese Academy of Science (UCAS) Beijing China Institute of Physics University of Belgrade Belgrade Serbia Department for Physics and Technology University of Bergen Bergen Norway Physics Division Lawrence Berkeley National Laboratory and University of California Berkeley CA United States Institut für Physik Humboldt Universität zu Berlin Berlin Germany Albert Ei

The accurate simulation of additional interactions at the ATLAS experiment for the analysis of proton–proton collisions delivered by the Large Hadron Collider presents a significant challenge to the computing resources. During the LHC Run 2 (2015–2018), there were up to 70 inelastic interactions per bunch crossing, which need to be accounted for in Monte Carlo (MC) production. In this document, a new method to account for these additional interactions in the simulation chain is described. Instead of sampling the inelastic interactions and adding their energy deposits to a hard-scatter interaction one-by-one, the inelastic interactions are presampled, independent of the hard scatter, and stored as combined events. Consequently, for each hard-scatter interaction, only one such presampled event needs to be added as part of the simulation chain. For the Run 2 simulation chain, with an average of 35 interactions per bunch crossing, this new method provides a substantial reduction in MC production CPU needs of around 20%, while reproducing the properties of the reconstructed quantities relevant for physics analyses with good accuracy. © 2022, The Author(s).

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