S. Polyakov, A. Demichev, A. Kryukov, E. Postnikov
TAIGAexperiment uses hybrid detection system for cosmic and gamma rays that currently includes three imaging atmospheric Cherenkov telescopes (IACTs). Previously we used convolutional neural networks to identify gamma ray events and estimate the energy of the gamma rays based on an image from a single telescope. Subsequently we adapted these techniques to use data from multiple telescopes, increasing the quality of selection and the accuracy of estimates. All the results have been obtained with the simulated data of TAIGA Monte Carlo software.
{"title":"The use of convolutional neural networks for processing images from multiple IACTs in the TAIGA experiment","authors":"S. Polyakov, A. Demichev, A. Kryukov, E. Postnikov","doi":"10.22323/1.395.0753","DOIUrl":"https://doi.org/10.22323/1.395.0753","url":null,"abstract":"TAIGAexperiment uses hybrid detection system for cosmic and gamma rays that currently includes three imaging atmospheric Cherenkov telescopes (IACTs). Previously we used convolutional neural networks to identify gamma ray events and estimate the energy of the gamma rays based on an image from a single telescope. Subsequently we adapted these techniques to use data from multiple telescopes, increasing the quality of selection and the accuracy of estimates. All the results have been obtained with the simulated data of TAIGA Monte Carlo software.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"29 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-09-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81336931","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Tidal Disruption Events (TDEs) occur when stars pass close to supermassive black holes, and have long been predicted to emit cosmic rays and neutrinos. Recently the TDE AT2109dsg was identified in spatial and temporal coincidence with high-energy neutrino IC191001A as part of the Zwicky Transient Facility (ZTF) neutrino follow-up program, providing the first direct observational evidence supporting these objects as multi-messenger sources. In these proceedings, I will place the recent results of our ZTF neutrino follow-up program into the broader context of developments in TDE and neutrino astronomy.
{"title":"Tidal Disruption Events and High-energy Neutrinos","authors":"R. Stein","doi":"10.22323/1.395.0009","DOIUrl":"https://doi.org/10.22323/1.395.0009","url":null,"abstract":"Tidal Disruption Events (TDEs) occur when stars pass close to supermassive black holes, and have long been predicted to emit cosmic rays and neutrinos. Recently the TDE AT2109dsg was identified in spatial and temporal coincidence with high-energy neutrino IC191001A as part of the Zwicky Transient Facility (ZTF) neutrino follow-up program, providing the first direct observational evidence supporting these objects as multi-messenger sources. In these proceedings, I will place the recent results of our ZTF neutrino follow-up program into the broader context of developments in TDE and neutrino astronomy.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"27 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-09-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73527741","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
J. Tomsick, S. Boggs, A. Zoglauer, E. Wulf, L. Mitchell, B. Phlips, C. Sleator, T. Brandt, A. Shih, Ja Roberts, P. Jean, P. Ballmoos, J. M. Oliveros, A. Smale, C. Kierans, D. Hartmann, M. Leising, M. Ajello, E. Burns, C. Fryer, P. Saint-Hilaire, J. Malzac, F. Tavecchio, V. Fioretti, A. Bulgarelli, G. Ghirlanda, Hsiang-Kuang Chang, Tadayuki Takahashi, K. Nakazawa, S. Matsumoto, Tom Melia, T. Siegert, A. Lowell, Hadar Lazar, J. Beechert, H. Gulick
The Compton Spectrometer and Imager (COSI) is a 0.2–5 MeV Compton telescope capable of imaging, spectroscopy, and polarimetry of astrophysical sources. Such capabilities are made possible by COSI’s germanium cross-strip detectors, which provide high efficiency, high resolution spectroscopy and precise 3D positioning of photon interactions. Science goals for COSI include studies of 0.511 MeV emission from antimatter annihilation in the Galaxy, mapping radioactive elements from nucleosynthesis, determining emission mechanisms and source geometries with polarization, and detecting and localizing multimessenger sources. The instantaneous field of view (FOV) for the germanium detectors is >25% of the sky, and they are surrounded on the sides and bottom by active shields, providing background rejection as well as allowing for detection of gamma-ray bursts or other gamma-ray flares over >50% of the sky. We have completed a Phase A concept study to consider COSI as a Small Explorer (SMEX) satellite mission, and here we discuss the advances COSI-SMEX provides for astrophysics in the MeV bandpass.
{"title":"The Compton Spectrometer and Imager Project for MeV Astronomy","authors":"J. Tomsick, S. Boggs, A. Zoglauer, E. Wulf, L. Mitchell, B. Phlips, C. Sleator, T. Brandt, A. Shih, Ja Roberts, P. Jean, P. Ballmoos, J. M. Oliveros, A. Smale, C. Kierans, D. Hartmann, M. Leising, M. Ajello, E. Burns, C. Fryer, P. Saint-Hilaire, J. Malzac, F. Tavecchio, V. Fioretti, A. Bulgarelli, G. Ghirlanda, Hsiang-Kuang Chang, Tadayuki Takahashi, K. Nakazawa, S. Matsumoto, Tom Melia, T. Siegert, A. Lowell, Hadar Lazar, J. Beechert, H. Gulick","doi":"10.22323/1.395.0652","DOIUrl":"https://doi.org/10.22323/1.395.0652","url":null,"abstract":"The Compton Spectrometer and Imager (COSI) is a 0.2–5 MeV Compton telescope capable of imaging, spectroscopy, and polarimetry of astrophysical sources. Such capabilities are made possible by COSI’s germanium cross-strip detectors, which provide high efficiency, high resolution spectroscopy and precise 3D positioning of photon interactions. Science goals for COSI include studies of 0.511 MeV emission from antimatter annihilation in the Galaxy, mapping radioactive elements from nucleosynthesis, determining emission mechanisms and source geometries with polarization, and detecting and localizing multimessenger sources. The instantaneous field of view (FOV) for the germanium detectors is >25% of the sky, and they are surrounded on the sides and bottom by active shields, providing background rejection as well as allowing for detection of gamma-ray bursts or other gamma-ray flares over >50% of the sky. We have completed a Phase A concept study to consider COSI as a Small Explorer (SMEX) satellite mission, and here we discuss the advances COSI-SMEX provides for astrophysics in the MeV bandpass.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"7 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-09-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"87947743","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The Tibet ASgamma experiment is located at 4,300m above sea level, in Tibet, China.The experiment is composed of a 65,700 m2 surface air shower array and 3,400 m2 underground water Cherenkov muon detectors. The surface air shower array is used for reconstructing the primary particle energy and direction, while the underground muon detectors are used for discriminating gamma-ray induced muon-poor air showers from cosmic-ray (proton, helium,...) induced muon-rich air showers.Recently,the Tibet ASgamma experiment successfully observed gamma rays in the 100 TeV region from some point/extended sources as well as sub-PeV diffuse gamma rays along the Galactic disk.In this talk, The observational results as well as their interpretations will be presented, followed by some future prospect.
{"title":"Highlights from gamma-ray observation by the Tibet ASgamma experiment.","authors":"M. Takita","doi":"10.22323/1.395.0015","DOIUrl":"https://doi.org/10.22323/1.395.0015","url":null,"abstract":"The Tibet ASgamma experiment is located at 4,300m above sea level, in Tibet, China.The experiment is composed of a 65,700 m2 surface air shower array and 3,400 m2 underground water Cherenkov muon detectors. The surface air shower array is used for reconstructing the primary particle energy and direction, while the underground muon detectors are used for discriminating gamma-ray induced muon-poor air showers from \u0000cosmic-ray (proton, helium,...) induced muon-rich air showers.Recently,the Tibet ASgamma experiment successfully observed gamma rays in the 100 TeV region from some point/extended sources as well as sub-PeV diffuse gamma rays along the Galactic disk.In this talk, The observational results as well as their interpretations will be presented,\u0000followed by some future prospect.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"64 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-09-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"88993095","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
M. Pesce-Rollins, N. Omodei, V. Petrosian, F. Longo
Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA Department of Physics, University of Trieste and INFN, sezione di Trieste, via Valerio 2, I-34127 Trieste, Italy E-mail: melissa.pesce.rollins@pi.infn.it
比萨国家核物理研究所,分庭I-56127比萨、意大利(W . W . Hansen实验物理实验室、研究所(Kavli Institute for Particle天体物理学和Cosmology, Department of物理和SLAC National达实验室,斯坦福大学(Stanford University),美国斯坦福大学,CA 94305 Department of Physics,的里雅斯特大学和特隆赫姆的里雅斯特、瓦莱里(2)节,I-34127意大利里雅斯特,电子邮件:梅丽莎。鱼rollins@pi特隆赫姆。it
{"title":"Probing particle acceleration through gamma-ray Solar flare observations","authors":"M. Pesce-Rollins, N. Omodei, V. Petrosian, F. Longo","doi":"10.22323/1.395.0034","DOIUrl":"https://doi.org/10.22323/1.395.0034","url":null,"abstract":"Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA Department of Physics, University of Trieste and INFN, sezione di Trieste, via Valerio 2, I-34127 Trieste, Italy E-mail: melissa.pesce.rollins@pi.infn.it","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"30 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76941974","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Galactic cosmic rays (CRs) are accelerated by astrophysical shocks, primarily supernova remnants (SNRs), via diffusive shock acceleration (DSA), an efficient mechanism that predicts power-law energy distributions of CRs. However, observations of both nonthermal SNR emission and Galactic CRs imply CR spectra that are steeper than the standard DSA prediction, ∝ −2. Recent kinetic hybrid simulations suggest that such steep spectra may be the result of a “postcursor”, or drift of CRs and magnetic structures with respect to the thermal plasma behind the shock. Using a semi-analytic model of non-linear DSA, we generalize this result to a wide range of astrophysical shocks. By accounting for the presence of a postcursor, we produce CR energy distributions that are substantially steeper than −2 and consistent with observations. Our formalism reproduces both modestly steep spectra of Galactic SNRs (∝ −2.2) and the very steep spectra of young radio supernovae (∝ −3).
{"title":"Galactic Cosmic Ray Acceleration with Steep Spectra","authors":"R. Diesing, D. Caprioli","doi":"10.22323/1.395.0029","DOIUrl":"https://doi.org/10.22323/1.395.0029","url":null,"abstract":"Galactic cosmic rays (CRs) are accelerated by astrophysical shocks, primarily supernova remnants (SNRs), via diffusive shock acceleration (DSA), an efficient mechanism that predicts power-law energy distributions of CRs. However, observations of both nonthermal SNR emission and Galactic CRs imply CR spectra that are steeper than the standard DSA prediction, ∝ −2. Recent kinetic hybrid simulations suggest that such steep spectra may be the result of a “postcursor”, or drift of CRs and magnetic structures with respect to the thermal plasma behind the shock. Using a semi-analytic model of non-linear DSA, we generalize this result to a wide range of astrophysical shocks. By accounting for the presence of a postcursor, we produce CR energy distributions that are substantially steeper than −2 and consistent with observations. Our formalism reproduces both modestly steep spectra of Galactic SNRs (∝ −2.2) and the very steep spectra of young radio supernovae (∝ −3).","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"252 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"72878690","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
H. Dembinski, J. Albrecht, L. Cazon, A. Fedynitch, K. Kampert, T. Pierog, W. Rhode, D. Soldin, B. Spaan, R. Ulrich, Michael Unger
High-energy cosmic rays are observed indirectly by detecting the extensive air showers initiated in Earth’s atmosphere. Air showers are hadronic cascades, which eventually decay into muons and the muon number is a key observable to infer the mass composition of cosmic rays. The interpretation of these observations relies on accurate models of air shower physics, which is a challenge and an opportunity to test QCD under extreme conditions. Air shower simulations with state-of-the-art QCD models show a significant muon deficit with respect to measurements; this is called the Muon Puzzle. The origin of this discrepancy has been traced to the composition of secondary particles in hadronic interactions.
{"title":"The Muon Puzzle in air showers and its connection to the LHC","authors":"H. Dembinski, J. Albrecht, L. Cazon, A. Fedynitch, K. Kampert, T. Pierog, W. Rhode, D. Soldin, B. Spaan, R. Ulrich, Michael Unger","doi":"10.22323/1.395.0037","DOIUrl":"https://doi.org/10.22323/1.395.0037","url":null,"abstract":"High-energy cosmic rays are observed indirectly by detecting the extensive air showers initiated in Earth’s atmosphere. Air showers are hadronic cascades, which eventually decay into muons and the muon number is a key observable to infer the mass composition of cosmic rays. The interpretation of these observations relies on accurate models of air shower physics, which is a challenge and an opportunity to test QCD under extreme conditions. Air shower simulations with state-of-the-art QCD models show a significant muon deficit with respect to measurements; this is called the Muon Puzzle. The origin of this discrepancy has been traced to the composition of secondary particles in hadronic interactions.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"55 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"90058628","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
This rapporteur paper summarizes the 118 contributed presentations on solar and heliospheric physics (i.e. the SH sessions) presented at the 37th International Cosmic Ray Conference. These presentations discussed various aspects of cosmic ray acceleration, transport, and modulation in the heliosphere. New and novel cosmic ray measurement techniques and related instrumentation were also presented.
{"title":"Rapporteur Talk: Solar and Heliospheric","authors":"D. Strauss","doi":"10.22323/1.395.0049","DOIUrl":"https://doi.org/10.22323/1.395.0049","url":null,"abstract":"This rapporteur paper summarizes the 118 contributed presentations on solar and heliospheric physics (i.e. the SH sessions) presented at the 37th International Cosmic Ray Conference. These presentations discussed various aspects of cosmic ray acceleration, transport, and modulation in the heliosphere. New and novel cosmic ray measurement techniques and related instrumentation were also presented.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"4 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"84629115","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
This document is based on a rapporteur talk given at the 37$^{rm{th}}$ International Cosmic Ray Conference (ICRC 2021). The article summarises the status of DM searches.
{"title":"News on Dark Matter from ICRC 2021","authors":"M. Taoso","doi":"10.22323/1.395.0047","DOIUrl":"https://doi.org/10.22323/1.395.0047","url":null,"abstract":"This document is based on a rapporteur talk given at the 37$^{rm{th}}$ International Cosmic Ray Conference (ICRC 2021).\u0000The article summarises the status of DM searches.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"37 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79827851","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
While biologists have not yet reached a consensus on the definition of life, homochirality - the specific molecular handedness of biomolecules - is a phenomenon only produced by life. The unraveling of its origin requires interdisciplinary research, by exploring fundamental physics, chemistry, astrophysics and biology. Here, we consider the origin of biological homochirality in the context of astrophysics and particle physics. The weak force, one of the fundamental forces operating in nature, is parity-violating. On Earth, at ground level, most of our cosmic radiation dose comes from polarized muons formed in a decay involving the weak force. We discuss how the magnetic polarization is transmitted in cosmic showers within several different environments which are prime targets in the search for the origin of life. We consider how this polarization could have induced a biological preference for one type of chirality over the other, and discuss the implications for the search of life in other worlds.
{"title":"Polarized muons and the origin of biological homochirality","authors":"N. Globus, R. Blandford, A. Fedynitch","doi":"10.22323/1.395.0031","DOIUrl":"https://doi.org/10.22323/1.395.0031","url":null,"abstract":"While biologists have not yet reached a consensus on the definition of life, homochirality - the specific molecular handedness of biomolecules - is a phenomenon only produced by life. The unraveling of its origin requires interdisciplinary research, by exploring fundamental physics, chemistry, astrophysics and biology. Here, we consider the origin of biological homochirality in the context of astrophysics and particle physics. The weak force, one of the fundamental forces operating in nature, is parity-violating. On Earth, at ground level, most of our cosmic radiation dose comes from polarized muons formed in a decay involving the weak force. We discuss how the magnetic polarization is transmitted in cosmic showers within several different environments which are prime targets in the search for the origin of life. We consider how this polarization could have induced a biological preference for one type of chirality over the other, and discuss the implications for the search of life in other worlds.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"39 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"72637014","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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