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arXiv 2024年

作者： Abe, H. Abe, S. Acciari, V.A. Agudo, I. Aniello, T. Ansoldi, S. Antonelli, L.A. Engels, A. Arbet Arcaro, C. Artero, M. Asano, K. Baack, d. Babić, A. Baquero, A. de Almeida, U. Barres Batković, I. Baxter, J. Bernardini, E. Bernardos, M. Bernete, J. Berti, A. Bigongiari, C. Biland, A. Blanch, O. Bonnoli, G. Bošnjak, Ž. Burelli, I. Busetto, G. Campoy-Ordaz, A. Carosi, A. Carosi, r. Carretero-Castrillo, M. Castro-Tirado, A.J. Chai, Y. Cifuentes, A. Cikota, S. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. d’Amico, G. d’Elia, V. da Vela, P. dazzi, F. de Angelis, A. de Lotto, B. del Popolo, A. delfino, M. delgado, J. Mendez, C. delgado depaoli, d. di Pierro, F. di Venere, L. Prester, d. dominis donini, A. dorner, d. doro, M. Elsaesser, d. Emery, G. Escudero, J. Fariña, L. Fattorini, A. Foffano, L. Font, L. Fukami, S. Fukazawa, Y. López, r.J. García Gasparyan, S. Gaug, M. Paiva, J.G. Giesbrecht Giglietto, N. Giordano, F. Gliwny, P. Grau, r. Green, J.G. Hadasch, d. Hahn, A. Heckmann, L. Herrera, J. Hrupec, d. Hütten, M. Imazawa, r. Inada, T. Iotov, r. Ishio, K. Martínez, I. Jiménez Jormanainen, J. Kerszberg, d. Kluge, G.W. Kobayashi, Y. Kubo, H. Kushida, J. Lezáun, M. Láinez Lamastra, A. Leone, F. Lindfors, E. Linhoff, L. Lombardi, S. Longo, F. López-Moya, M. López-Oramas, A. Loporchio, S. Lorini, A. de Oliveira Fraga, B. Machado Majumdar, P. Makariev, M. Maneva, G. Mang, N. Manganaro, M. Mangano, S. Mannheim, K. Mariotti, M. Martínez, M. Mas-Aguilar, A. Mazin, d. Menchiari, S. Mender, S. Mićanović, S. Miceli, d. Miranda, J.M. Mirzoyan, r. Molina, E. Mondal, H.A. Morcuende, d. Nanci, C. Neustroev, V. Nigro, C. Nishijima, K. Ekoume, T. Njoh Noda, K. Nozaki, S. Ohtani, Y. Otero-Santos, J. Paiano, S. Palatiello, M. Paneque, d. Paoletti, r. Paredes, J.M. Pavletić, L. Persic, M. Pihet, M. Pirola, G. Podobnik, F. Moroni, P.G. Prada Prandini, E. Principe, G. Priyadarshi, C. rhode, W. ribó, M. rico, J. righi, C. Sahakyan, N. Saito, T. Satalecka, K. The University of Tokyo Chiba Kashiwa277-8582 Japan Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna La Laguna TenerifeE-38200 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain RomeI-00136 Italy Università di Udine INFN Trieste UdineI-33100 Italy Rome Italy Max-Planck-Institut für Physik MünchenD-80805 Germany Università di Padova INFN PadovaI-35131 Italy Bellaterra BarcelonaE-08193 Spain Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain ETH Zürich ZürichCH-8093 Switzerland Departament de Física CERES-IEEC UniversitatAutònoma de Barcelona BellaterraE-08193 Spain Università di Pisa INFN Pisa PisaI-56126 Italy Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Department for Physics and Technology University of Bergen Allégaten 55 Bergen5007 Norway INFN MAGIC Group INFN Sezione di Catania Dipartimento di Fisica e Astronomia University of Catania CataniaI-95123 Italy Bellaterra BarcelonaE-08193 Spain INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino TorinoI-10125 Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica dell’Università e del Politecnico di Bari BariI-70125 Italy Croatian MAGIC Group University of Rijeka Faculty of Physics Rijeka51000 Croatia University of Geneva Chemin d’Ecogia 16 VersoixCH-1290 Switzerland Japanese MAGIC Group: Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Hiroshima739-8526 Japan Armenian MAGIC Group: ICRANet-Armenia Yerevan0019 Armenia University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland

OT 081 is a well-known, luminous blazar that is remarkably variable in many energy bands. We present the first broadband study of the source which includes very-high-energy (VHE, E >100 GeV) γ-ray data taken by the MAGIC and H.E.S.S. imaging Cherenkov telescopes. The discovery of VHE γ-ray emission happened during a high state of γ-ray activity in July 2016, observed by many instruments from radio to VHE γ-rays. We identify four states of activity of the source, one of which includes VHE γ-ray emission. Variability in the VHE domain is found on daily timescales. The intrinsic VHE spectrum can be described by a power-law with index 3.27 ± 0.44stat ± 0.15sys (MAGIC) and 3.39 ± 0.58stat ± 0.64sys (H.E.S.S.) in the energy range of 55–300 GeV and 120–500 GeV, respectively. The broadband emission cannot be sucessfully reproduced by a simple one-zone synchrotron self-Compton model. Instead, an additional external Compton component is required. We test a lepto-hadronic model that reproduces the dataset well and a proton-synchrotron dominated model that requires an extreme proton luminosity. Emission models that are able to successfully represent the data place the emitting region well outside of the Broad Line region (BLr) to a location at which the radiative environment is dominated by the infrared thermal radiation field of the dusty torus. In the scenario described by this flaring activity, the source appears to be an FSrQ, in contrast with past categorizations. This suggests that the source can be considered to be a transitional blazar, intermediate between BL Lac and FSrQ objects. Copyright © 2024, The Authors. All rights reserved.

关键词： Synchrotrons

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Multiple focal structure generation of incident beam in the focal region under tight focusing

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Materials Today: Proceedings 2021年 37卷 3775-3778页

作者： P. Suresh U. Muthuraman M. revathi K.B. rajesh U. Saravanakumar Z. Jaroszewicz Dept of ECE Vel Tech Rangarajan Dr Sagunthala R & D Institute of Science and Technology Chennai Tamil Nadu 600062 India Dept of EEE Francis Xavier Engineering College Tirunelveli 627003 Tamil Nadu India Engineering Department Scientific Society Group Tiruvannamalai Tamil Nadu 606805 India Dept of Physics Chikkanna Government Arts College Tiruppur Tamil Nadu 641602. India Dept of ECE Muthayammal Engineering College Rasipuram Namakkal Tamil Nadu 637408 India Institute of Applied Optics Department of Physical Optics Poland and National Institute of Telecommunications Warsaw 04894 Poland

The tight focusing investigation on spirally polarized axisymmetric Bessel-modulated Gaussian beam is studied based on vector diffraction theory is presented numerically. The optical intensity distribution of tightly focused through the high NA lens in the focal region is presented numerically for various beam parameter µ and spiral parameter C. It is observed that different focal structure is developed in the focal region which finds useful application in the wider range. The focal structure generated in the focal field has wide practical applications like optical scanning microscopy, optical tweezers , optical trapping, etc., the generated multiple focal structure will have useful application.

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Time-dependent modelling of short-term variability in the TeV-blazar VEr J0521+211 during the major flare in 2020

arXiv

引用

arXiv 2024年

作者： Abe, S. Abhir, J. Abhishek, A. Acciari, V.A. Aguasca-Cabot, A. Agudo, I. Aniello, T. Ansoldi, S. Antonelli, L.A. Arbet Engels, A. Arcaro, C. Artero, M. Asano, K. Baack, d. Babić, A. Barres de Almeida, U. Barrio, J.A. Batković, I. Bautista, A. Baxter, J. Becerra González, J. Bednarek, W. Bernardini, E. Bernete, J. Berti, A. Besenrieder, J. Bigongiari, C. Biland, A. Blanch, O. Bonnoli, G. Bošnjak, Ž. Bronzini, E. Burelli, I. Campoy-Ordaz, A. Carosi, A. Carosi, r. Carretero-Castrillo, M. Castro-Tirado, A.J. Cerasole, d. Ceribella, G. Chai, Y. Cifuentes, A. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. d'Amico, G. d'Elia, V. da Vela, P. dazzi, F. de Angelis, A. de Lotto, B. de Menezes, r. delfino, M. delgado, J. delgado Mendez, C. di Pierro, F. di Tria, r. di Venere, L. dominis Prester, d. donini, A. dorner, d. doro, M. Eisenberger, L. Elsaesser, d. Escudero, J. Fariña, L. Fattorini, A. Foffano, L. Font, L. Fröse, S. Fukami, S. Fukazawa, Y. García López, r.J. Garczarczyk, M. Gasparyan, S. Gaug, M. Giesbrecht Paiva, J.G. Giglietto, N. Giordano, F. Gliwny, P. Gradetzke, T. Grau, r. Green, d. Green, J.G. Günther, P. Hadasch, d. Hahn, A. Hassan, T. Heckmann, L. Herrera Llorente, J. Hrupec, d. Imazawa, r. Ishio, K. Jiménez Martínez, I. Jormanainen, J. Kankkunen, S. Kayanoki, T. Kerszberg, d. Kluge, G.W. Kobayashi, Y. Kouch, P.M. Kubo, H. Kushida, J. Láinez, M. Lamastra, A. Leone, F. Lindfors, E. Lombardi, S. Longo, F. López-Coto, r. López-Moya, M. López-Oramas, A. Loporchio, S. Lorini, A. Lyard, E. Machado de Oliveira Fraga, B. Majumdar, P. Makariev, M. Maneva, G. Manganaro, M. Mangano, S. Mannheim, K. Mariotti, M. Martínez, M. Martínez-Chicharro, M. Mas-Aguilar, A. Mazin, d. Menchiari, S. Mender, S. Miceli, d. Miener, T. Miranda, J.M. Mirzoyan, r. Molero González, M. Molina, E. Mondal, H.A. Moralejo, A. Morcuende, d. Nakamori, T. Nanci, C. Neustroev, V. Nickel, L. Nievas rosillo, M. Nigro, C. Nikolić, L. Nilsson, K. Nishijima, K. Njoh Ekoume, T. Noda, K. The University of Tokyo Kashiwa Chiba277-8582 Japan ETH Zürich ZürichCH-8093 Switzerland Università di Siena INFN Pisa SienaI-53100 Italy Bellaterra BarcelonaE-08193 Spain Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain RomeI-00136 Italy Università di Udine INFN Trieste UdineI-33100 Italy Max-Planck-Institut für Physik GarchingD-85748 Germany Università di Padova INFN PadovaI-35131 Italy Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia URCA RJ Rio de Janeiro22290-180 Brazil IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain Instituto de Astrofísica de Canarias and Dpto. de Astrofísica Universidad de La Laguna Tenerife La LagunaE-38200 Spain University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain Departament de Física CERES-IEEC Universitat Autònoma de Barcelona BellaterraE-08193 Spain Università di Pisa INFN Pisa PisaI-56126 Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica Università e del Politecnico di Bari BariI-70125 Italy Department for Physics and Technology University of Bergen Norway INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino TorinoI-10125 Italy Croatian MAGIC Group University of Rijeka Faculty of Physics Rijeka51000 Croatia Universität Würzburg WürzburgD-97074 Germany Japanese MAGIC Group: Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Hiroshima739-8526 Japan ZeuthenD-15738 Germany Armenian MAGIC Group: ICRANet-Armenia Yerevan0019 Armenia Croatian MAGIC Group Josip Juraj Strossmayer University of Osijek Department of Physics Osijek31000 Croatia Finnish MAGIC Group Finnish Centr

The BL Lacertae object VEr J0521+211 underwent a notable flaring episode in February 2020. A short-term monitoring campaign, led by the MAGIC (Major Atmospheric Gamma Imaging Cherenkov) collaboration, covering a wide energy range from radio to very-high-energy (VHE, 100 GeV 100 TeV). While the photon component, generated via decay of neutral pions, is not directly observable as it is subject to intense pair production (and therefore extinction) through interactions with the cosmic microwave background photons, neutrino detectors (e.g. IceCube) can probe the predicted neutrino component. Finally, the analysis of the gamma-ray spectra, as observed by MAGIC and the Fermi-LAT telescopes, yielded a conservative 95% confidence upper limit of z ≤ 0.244 for the redshift of this blazar. Copyright © 2024, The Authors. All rights reserved.

关键词： Photons

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The variability patterns of the TeV blazar PG 1553+113 from a decade of MAGIC and multi-band observations

arXiv

引用

arXiv 2024年

作者： Abe, H. Abe, S. Abhir, J. Acciari, V.A. Agudo, I. Aniello, T. Ansoldi, S. Antonelli, L.A. Engels, A. Arbet Arcaro, C. Artero, M. Asano, K. Baack, d. Babić, A. Baquero, A. de Almeida, U. Barres Batković, I. Baxter, J. González, J. Becerra Bernardini, E. Bernete, J. Berti, A. Besenrieder, J. Bigongiari, C. Biland, A. Blanch, O. Bonnoli, G. Bošnjak, Ž. Burelli, I. Busetto, G. Campoy-Ordaz, A. Carosi, A. Carosi, r. Carretero-Castrillo, M. Castro-Tirado, A.J. Chai, Y. Cifuentes, A. Cikota, S. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. d’Amico, G. d’Elia, V. da Vela, P. dazzi, F. de Angelis, A. de Lotto, B. del Popolo, A. delfino, M. delgado, J. Mendez, C. delgado depaoli, d. di Pierro, F. di Venere, L. Prester, d. dominis donini, A. dorner, d. doro, M. Elsaesser, d. Emery, G. Escudero, J. Farin͂a, L. Fattorini, A. Foffano, L. Font, L. Fukami, S. Fukazawa, Y. López, r.J. García Gasparyan, S. Gaug, M. Paiva, J.G. Giesbrecht Giglietto, N. Giordano, F. Gliwny, P. Grau, r. Green, J.G. Hadasch, d. Hahn, A. Heckmann, L. Herrera, J. Hovatta, T. Hrupec, d. Hütten, M. Imazawa, r. Inada, T. Iotov, r. Ishio, K. Martínez, I. Jiménez Jormanainen, J. Kerszberg, d. Kluge, G.W. Kobayashi, Y. Kouch, P.M. Kubo, H. Kushida, J. Lezáun, M. Láinez Lamastra, A. Leone, F. Lindfors, E. Liodakis, I. Lombardi, S. Longo, F. López-Moya, M. López-Oramas, A. Loporchio, S. Lorini, A. Fraga, B. Machado de Oliveira Majumdar, P. Makariev, M. Maneva, G. Mang, N. Manganaro, M. Mannheim, K. Mariotti, M. Martínez, M. Martínez-Chicharro, M. Mas-Aguilar, A. Mazin, d. Menchiari, S. Mender, S. Miceli, d. Miener, T. Miranda, J.M. Mirzoyan, r. González, M. Molero Molina, E. Mondal, H.A. Moralejo, A. Morcuende, d. Nakamori, T. Nanci, C. Neustroev, V. Nigro, C. Nikolić, L. Nilsson, K. Nishijima, K. Ekoume, T. Njoh Noda, K. Nozaki, S. Ohtani, Y. Okumura, A. Otero-Santos, J. Paiano, S. Palatiello, M. Paneque, d. Paoletti, r. Paredes, J.M. Pavlović, d. Persic, M. Pihet, M. Pirola, G. The University of Tokyo Chiba Kashiwa277-8582 Japan ETH Zürich ZürichCH-8093 Switzerland Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna Tenerife La LagunaE-38200 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain RomeI-00136 Italy Università di Udine INFN Trieste UdineI-33100 Italy Max-Planck-Institut für Physik MünchenD-80805 Germany Università di Padova INFN PadovaI-35131 Italy Bellaterra BarcelonaE-08193 Spain Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain Departament de Física CERES-IEEC Universitat Autònoma de Barcelona BellaterraE-08193 Spain Università di Pisa INFN Pisa PisaI-56126 Italy Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Department for Physics and Technology University of Bergen Norway INFN MAGIC Group INFN Sezione di Catania Dipartimento di Fisica e Astronomia University of Catania CataniaI-95123 Italy INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino TorinoI-10125 Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica dell’Università e del Politecnico di Bari BariI-70125 Italy Croatian MAGIC Group University of Rijeka Faculty of Physics Rijeka51000 Croatia University of Geneva Chemin d’Ecogia 16 VersoixCH-1290 Switzerland Japanese MAGIC Group: Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Hiroshima739-8526 Japan Armenian MAGIC Group: ICRANet-Armenia Yerevan0019 Armenia University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Croatian MAGIC Group Josip Juraj Strossmayer University of Osijek Department

PG 1553+113 is one of the few blazars with a convincing quasi-periodic emission in the gamma-ray band. The source is also a very high-energy (VHE;>100 GeV) gamma-ray emitter. To better understand its properties and identify the underlying physical processes driving its variability, the MAGIC Collaboration initiated a multiyear, multiwavelength monitoring campaign in 2015 involving the OVrO 40-m and Medicina radio telescopes, rEM, KVA, and the MAGIC telescopes, Swift and Fermi satellites, and the WEBT network. The analysis presented in this paper uses data until 2017 and focuses on the characterization of the variability. The gamma-ray data show a (hint of a) periodic signal compatible with literature, but the X-ray and VHE gamma-ray data do not show statistical evidence for a periodic signal. In other bands, the data are compatible with the gamma-ray period, but with a relatively high p-value. The complex connection between the low and high-energy emission and the non-monochromatic modulation and changes in flux suggests that a simple one-zone model is unable to explain all the variability. Instead, a model including a periodic component along with multiple emission zones is required. Copyright © 2024, The Authors. All rights reserved.

关键词： Gamma rays

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MAGIC detection of GrB 201216C at z = 1.1

arXiv

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arXiv 2023年

作者： Abe, H. Abe, S. Acciari, V.A. Agudo, I. Aniello, T. Ansoldi, S. Antonelli, L.A. Engels, A. Arbet Arcaro, C. Artero, M. Asano, K. Baack, d. Babić, A. Baquero, A. de Almeida, U. Barres Barrio, J.A. Batković, I. Baxter, J. González, J. Becerra Bednarek, W. Bernardini, E. Bernete, J. Berti, A. Besenrieder, J. Bigongiari, C. Biland, A. Blanch, O. Bonnoli, G. Bošnjak, Ž. Burelli, I. Busetto, G. Campoy-Ordaz, A. Carosi, A. Carosi, r. Carretero-Castrillo, M. Castro-Tirado, A.J. Ceribella, G. Chai, Y. Cifuentes, A. Cikota, S. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. d’Amico, G. d’Elia, V. da Vela, P. dazzi, F. de Angelis, A. de Lotto, B. del Popolo, A. delfino, M. delgado, J. Mendez, C. delgado depaoli, d. di Pierro, F. di Venere, L. Prester, d. dominis donini, A. dorner, d. doro, M. Elsaesser, d. Emery, G. Escudero, J. Fariña, L. Fattorini, A. Foffano, L. Font, L. Fukami, S. Fukazawa, Y. López, r.J. García Garczarczyk, M. Gasparyan, S. Gaug, M. Paiva, J.G. Giesbrecht Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Grau, r. Green, d. Green, J.G. Hadasch, d. Hahn, A. Hassan, T. Heckmann, L. Herrera, J. Hrupec, d. Hütten, M. Imazawa, r. Inada, T. Iotov, r. Ishio, K. Martínez, I. Jiménez Jormanainen, J. Kerszberg, d. Kluge, G.W. Kobayashi, Y. Kouch, P.M. Kubo, H. Kushida, J. Lezáun, M. Láinez Lamastra, A. Leone, F. Lindfors, E. Linhoff, L. Lombardi, S. Longo, F. López-Coto, r. López-Moya, M. López-Oramas, A. Loporchio, S. Lorini, A. Lyard, E. de Oliveira Fraga, B. Machado Majumdar, P. Makariev, M. Maneva, G. Mang, N. Manganaro, M. Mangano, S. Mannheim, K. Mariotti, M. Martínez, M. Mas-Aguilar, A. Mazin, d. Menchiari, S. Mender, S. Mićanović, S. Miceli, d. Miener, T. Miranda, J.M. Mirzoyan, r. González, M. Molero Molina, E. Mondal, H.A. Moralejo, A. Morcuende, d. Nanci, C. Nava, L. Neustroev, V. rosillo, M. Nievas Nigro, C. Nikolić, L. Nilsson, K. Nishijima, K. Ekoume, T. Njoh Noda, K. Nozaki, S. Ohtani, Y. Okumura, A. Otero-Santos, J. Paiano, S. The University of Tokyo Chiba Kashiwa277-8582 Japan Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna La Laguna TenerifeE-38200 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain RomeI-00136 Italy Università di Udine INFN Trieste UdineI-33100 Italy Max-Planck-Institut für Physik MünchenD-80805 Germany Università di Padova INFN PadovaI-35131 Italy Bellaterra BarcelonaE-08193 Spain Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain ETH Zürich ZürichCH-8093 Switzerland Departament de Física CERES-IEEC Universitat Autònoma de Barcelona BellaterraE-08193 Spain Università di Pisa INFN Pisa PisaI-56126 Italy Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Department for Physics and Technology University of Bergen Norway INFN MAGIC Group INFN Sezione di Catania Dipartimento di Fisica e Astronomia University of Catania CataniaI-95123 Italy INFN MAGIC Group INFN Sezione di Torino and Università degli Studi di Torino TorinoI-10125 Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica dell’Università e del Politecnico di Bari BariI-70125 Italy Croatian MAGIC Group University of Rijeka Faculty of Physics Rijeka51000 Croatia Universität Würzburg WürzburgD-97074 Germany University of Geneva Chemin d’Ecogia 16 VersoixCH-1290 Switzerland Japanese MAGIC Group: Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Hiroshima739-8526 Japan ZeuthenD-15738 Germany Armenian MAGIC Group: ICRANet-Armenia Yerevan0019 Armenia

Gamma-ray bursts (GrBs) are explosive transient events occurring at cosmological distances, releasing a large amount of energy as electromagnetic radiation over several energy bands. We report the detection of the long GrB 201216C by the MAGIC telescopes. The source is located at z = 1.1 and thus it is the farthest one detected at very high energies. The emission above 70 GeV of GrB 201216C is modelled together with multi-wavelength data within a synchrotron and synchrotron-self Compton (SSC) scenario. We find that SSC can explain the broadband data well from the optical to the very-high-energy band. For the late-time radio data, a different component is needed to account for the observed emission. differently from previous GrBs detected in the very-high-energy range, the model for GrB 201216C strongly favors a wind-like medium. The model parameters have values similar to those found in past studies of the afterglows of GrBs detected up to GeV energies. Copyright © 2023, The Authors. All rights reserved.

关键词： Stars

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Multiple focal structure generation of incident beam in the focal region under tight focusing

Multiple focal structure generation of incident beam in the ...

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International Conference on Newer trends and Innovations in Mechanical Engineering, ICONTIME 2020

作者： Suresh, P. Muthuraman, U. revathi, M. rajesh, K.B. Saravanakumar, U. Jaroszewicz, Z. Dept of ECE Vel Tech Rangarajan Dr Sagunthala R and D Institute of Science and Technology Chennai Tamil Nadu600062 India Dept of EEE Francis Xavier Engineering College Tirunelveli Tamil Nadu627003 India Engineering Department Scientific Society Group Tiruvannamalai Tamil Nadu606805 India Dept of Physics Chikkanna Government Arts College Tiruppur Tamil Nadu641602 India Dept of ECE Muthayammal Engineering College Rasipuram Namakkal Tamil Nadu637408 India Institute of Applied Optics Department of Physical Optics Poland National Institute of Telecommunications Warsaw04894 Poland

The tight focusing investigation on spirally polarized axisymmetric Bessel-modulated Gaussian beam is studied based on vector diffraction theory is presented numerically. The optical intensity distribution of tightly focused through the high NA lens in the focal region is presented numerically for various beam parameter m and spiral parameter C. It is observed that different focal structure is developed in the focal region which finds useful application in the wider range. The focal structure generated in the focal field has wide practical applications like optical scanning microscopy, optical tweezers, optical trapping, etc., the generated multiple focal structure will have useful application. © 2020 Elsevier Ltd. All rights reserved.

关键词： Focusing

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MAGIC observations provide compelling evidence of the hadronic multi-TeV emission from the putative PeVatron SNr G106.3+2.7

arXiv

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arXiv 2022年

作者： Abe, H. Abe, S. Acciari, V.A. Agudo, I. Aniello, T. Ansoldi, S. Antonelli, L.A. Engels, A. Arbet Arcaro, C. Artero, M. Asano, K. Baack, d. Babić, A. Baquero, A. de Almeida, U. Barres Barrio, J.A. Batković, I. Baxter, J. González, J. Becerra Bednarek, W. Bernardini, E. Bernardos, M. Berti, A. Besenrieder, J. Bhattacharyya, W. Bigongiari, C. Biland, A. Blanch, O. Bonnoli, G. Bošnjak, Ž. Burelli, I. Busetto, G. Carosi, r. Carretero-Castrillo, M. Castro-Tirado, A.J. Ceribella, G. Chai, Y. Chilingarian, A. Cikota, S. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. d’Amico, G. d’Elia, V. da Vela, P. dazzi, F. de Angelis, A. de Lotto, B. Popolo, A. del delfino, M. delgado, J. Mendez, C. delgado depaoli, d. Pierro, F. di Venere, L. di do Souto Espiñeira, E. Prester, d. dominis donini, A. dorner, d. doro, M. Elsaesser, d. Emery, G. Escudero, J. ramazani, V. Fallah Fariña, L. Fattorini, A. Font, L. Fruck, C. Fukami, S. Fukazawa, Y. López, r.J. García Garczarczyk, M. Gasparyan, S. Gaug, M. Paiva, J.G. Giesbrecht Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Grau, r. Green, d. Green, J.G. Hadasch, d. Hahn, A. Hassan, T. Heckmann, L. Herrera, J. Hrupec, d. Hütten, M. Imazawa, r. Inada, T. Iotov, r. Ishio, K. Martínez, I. Jiménez Jormanainen, J. Kerszberg, d. Kobayashi, Y. Kubo, H. Kushida, J. Lamastra, A. Lelas, d. Leone, F. Lindfors, E. Linhoff, L. Lombardi, S. Longo, F. López-Coto, r. López-Moya, M. López-Oramas, A. Loporchio, S. Lorini, A. Lyard, E. de Oliveira Fraga, B. Machado Majumdar, P. Makariev, M. Maneva, G. Mang, N. Manganaro, M. Mangano, S. Mannheim, K. Mariotti, M. Martínez, M. Aguilar, A. Mas Mazin, d. Menchiari, S. Mender, S. Mićanović, S. Miceli, d. Miener, T. Miranda, J.M. Mirzoyan, r. Molina, E. Mondal, H.A. Moralejo, A. Morcuende, d. Moreno, V. Nakamori, T. Nanci, C. Nava, L. Neustroev, V. rosillo, M. Nievas Nigro, C. Nilsson, K. Nishijima, K. Ekoume, T. Njoh Noda, K. Nozaki, S. Ohtani, Y. Oka, T. Okumura, A. The University of Tokyo Chiba Kashiwa277-8582 Japan Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna La Laguna TenerifeE-38200 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain RomeI-00136 Italy Università di Udine INFN Trieste UdineI-33100 Italy Max-Planck-Institut für Physik MünchenD-80805 Germany Università di Padova INFN PadovaI-35131 Italy Bellaterra BarcelonaE-08193 Spain Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland ZeuthenD-15738 Germany ETH Zürich ZürichCH-8093 Switzerland Università di Pisa INFN Pisa PisaI-56126 Italy Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Armenian MAGIC Group A. Alikhanyan National Science Laboratory Yerevan0036 Armenia Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain Department for Physics and Technology University of Bergen Norway INFN MAGIC Group INFN Sezione di Catania Dipartimento di Fisica e Astronomia University of Catania CataniaI-95123 Italy INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino TorinoI-10125 Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica dell’Università e del Politecnico di Bari BariI-70125 Italy Croatian MAGIC Group University of Rijeka Faculty of Physics Rijeka51000 Croatia Universität Würzburg WürzburgD-97074 Germany University of Geneva Chemin d’Ecogia 16 VersoixCH-1290 Switzerland Finnish MAGIC Group Finnish Centre for Astronomy with ESO University of Turku TurkuFI-20014 Finland Departament de Física CERES-IEEC Universitat Autònoma de Barcelona BellaterraE-08193 Spain Japanese MAG

Context. Certain types of Supernova remnants (SNrs) in our Galaxy are assumed to be PeVatrons, capable of accelerating cosmic rays (Crs) to ∼ PeV energies. However, conclusive observational evidence for this has not yet been found. The SNr G106.3+2.7, detected at 1–100 TeV energies by different γ-ray facilities, is one of the most promising PeVatron candidates. This SNr has a cometary shape which can be divided into a head and a tail region with different physical conditions. However, it is not identified in which region the 100 TeV emission is produced due to the limited position accuracy and/or angular resolution of existing observational data. Additionally, it remains unclear whether the origin of the γ-ray emission is leptonic or hadronic. Aims. With the better angular resolution provided by these new MAGIC data compared to earlier γ-ray datasets, we aim to reveal the acceleration site of PeV particles and the emission mechanism by resolving the SNr G106.3+2.7 with 0.1◦ resolution at TeV energies. Methods. We observed the SNr G106.3+2.7 using the MAGIC telescopes for 121.7 hours in total after quality cuts, between May 2017 and August 2019. The analysis energy threshold is ∼ 0.2 TeV, and the angular resolution is 0.07–0.1◦. The γ-ray spectra of different parts of the emission are examined, benefiting from the unprecedented statistics and angular resolution at these energies provided by our new data. The measurements at other wavelengths such as radio, X-rays, GeV γ-rays and 10 TeV γ-rays are also used to model the emission mechanism precisely. results. We detected extended γ-ray emission spatially coincident with the radio continuum emission at the head and tail of SNr G106.3+2.7. The fact that we detected a significant γ-ray emission with energies above 6.0 TeV from the tail region only suggests that the emissions above 10 TeV, detected with air shower experiments (Milagro, HAWC, Tibet ASγ and LHAASO), are emitted only from the SNr tail. Under this assumption,

关键词： Gamma rays

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Childhood Cardiovascular risk Factors and Adult Cardiovascular Events

引用

四川生理科学杂志 2022年第2期44卷 53-53页

作者： david r Jacobs Jr From the Division of Epidemiology and Community Health School of Public Health (D.R.J.) and the Department of Pediatrics University of Minnesota Medical School (A.R.S. J.S.) University of Minnesota Minneapolis the Division of Biostatistics and Epidemiology (J.G.W. N.Z.) and the Heart Institute (E.M.U.) Cincinnati Children’s Hospital Medical Center and the Department of Pediatrics University of Cincinnati College of Medicine (J.G.W. N.Z. E.M.U.) — both in Cincinnati the Department of Pediatrics University of Colorado School of Medicine and Anschutz Medical Campus Children’s Hospital Colorado — both in Aurora (S.R.D.) the Center for Population Health Research (J.I. N.K. C.G.M. O.T.R.) the Research Center of Applied and Preventive Cardiovascular Medicine (J.I. N.K. C.G.M. O.T.R.) and the Departments of Medicine (M.J. J.S.A.V.) and Mathematics and Statistics (N.K.) University of Turku and the Center for Population Health Research (J.I. N.K. C.G.M. O.T.R.) the Division of Medicine (M.J. J.S.A.V.) and the Department of Clinical Physiology and Nuclear Medicine (O.T.R.) Turku University Hospital Turku and the Department of Clinical Chemistry Fimlab Laboratories and the Finnish Cardiovascular Research Center and the Faculty of Medicine and Health Technology Tampere University Tampere (T.L.) — all in Finland Menzies Institute for Medical Research University of Tasmania Hobart TAS (C.G.M. A.J.V. T.D.) and the Heart Research Group Murdoch Children’s Research Institute Melbourne VIC (T.D.) — both in Australia the School of Public Health and Tropical Medicine Tulane University New Orleans (L.A.B.) the Department of Epidemiology College of Public Health University of Iowa Iowa City (T.L.B.) the Division of Public Health Sciences Wake Forest School of Medicine Winston-Salem NC (R.J.P.) and the Nuffield Department of Women’s and Reproductive Health University of Oxford Oxford United Kingdom (T.D.).

Background:Childhood cardiovascular risk factors predict subclinical adult cardiovascular disease,but links to clinical events are ***:In a prospective cohort study involving participants in the International Childhood Cardiovascular Cohorts(i3C)Consortium,we evaluated whether childhood risk factors(at the ages of 3 to 19 years)were associated with cardiovascular events in adulthood after a mean follow-up of 35 years.

关键词： Cardiovascular cardiovascular Childhood

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detector-Agnostic Phase-Space distributions

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Physical review Letters 2020年第1期124卷 013605-013605页

作者： J. Sperling d. S. Phillips J. F. F Bulmer G. S. Thekkadath A. Eckstein T. A. W. Wolterink J. Lugani S. W. Nam A. Lita T. Gerrits W. Vogel G. S. Agarwal C. Silberhorn I. A. Walmsley Integrated Quantum Optics Group Applied Physics University of Paderborn 33098 Paderborn Germany Clarendon Laboratory University of Oxford Parks Road Oxford OX1 3PU United Kingdom National Institute of Standards and Technology 325 Broadway Boulder Colorado 80305 USA Institut für Physik Universität Rostock Albert-Einstein-Straße 23 D-18059 Rostock Germany Texas A&M University College Station Texas 77845 USA

The representation of quantum states via phase-space functions constitutes an intuitive technique to characterize light. However, the reconstruction of such distributions is challenging as it demands specific types of detectors and detailed models thereof to account for their particular properties and imperfections. To overcome these obstacles, we derive and implement a measurement scheme that enables a reconstruction of phase-space distributions for arbitrary states whose functionality does not depend on the knowledge of the detectors, thus defining the notion of detector-agnostic phase-space distributions. Our theory presents a generalization of well-known phase-space quasiprobability distributions, such as the Wigner function. We implement our measurement protocol, using state-of-the-art transition-edge sensors without performing a detector characterization. Based on our approach, we reveal the characteristic features of heralded single- and two-photon states in phase space and certify their nonclassicality with high statistical significance.

关键词： Optical tests of quantum theory Quantum measurements Quantum optics Quantum states of light Phase space methods

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Search for Gamma-ray Spectral Lines from dark Matter Annihilation up to 100 TeV towards the Galactic Center with MAGIC

arXiv

引用

arXiv 2022年

作者： Abe, H. Abe, S. Acciari, V.A. Aniello, T. Ansoldi, S. Antonelli, L.A. Engels, A. Arbet Arcaro, C. Artero, M. Asano, K. Baack, d. Babić, A. Baquero, A. de Almeida, U. Barres Barrio, J.A. Batković, I. Baxter, J. González, J. Becerra Bednarek, W. Bernardini, E. Bernardos, M. Berti, A. Besenrieder, J. Bhattacharyya, W. Bigongiari, C. Biland, A. Blanch, O. Bonnoli, G. Bošnjak, Ž. Burelli, I. Busetto, G. Carosi, r. Carretero-Castrillo, M. Ceribella, G. Chai, Y. Chilingarian, A. Cikota, S. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. d’Amico, G. d’Elia, V. da Vela, P. dazzi, F. de Angelis, A. de Lotto, B. del Popolo, A. delfino, M. delgado, J. Mendez, C. delgado depaoli, d. di Pierro, F. di Venere, L. Espiñeira, E. do Souto Prester, d. dominis donini, A. dorner, d. doro, M. Elsaesser, d. Emery, G. ramazani, V. Fallah Fariña, L. Fattorini, A. Font, L. Fruck, C. Fukami, S. Fukazawa, Y. López, r.J. García Garczarczyk, M. Gasparyan, S. Gaug, M. Paiva, J.G. Giesbrecht Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Green, J.G. Green, d. Hadasch, d. Hahn, A. Hassan, T. Heckmann, L. Herrera, J. Hrupec, d. Hütten, M. Imazawa, r. Inada, T. Iotov, r. Ishio, K. Martínez, I. Jiménez Jormanainen, J. Kerszberg, d. Kobayashi, Y. Kubo, H. Kushida, J. Lamastra, A. Lelas, d. Leone, F. Lindfors, E. Linhoff, L. Lombardi, S. Longo, F. López-Coto, r. López-Moya, M. López-Oramas, A. Loporchio, S. Lorini, A. Lyard, E. de Oliveira Fraga, B. Machado Majumdar, P. Makariev, M. Maneva, G. Mang, N. Manganaro, M. Mangano, S. Mannheim, K. Mariotti, M. Martínez, M. Aguilar, A. Mas Mazin, d. Menchiari, S. Mender, S. Mićanović, S. Miceli, d. Miener, T. Miranda, J.M. Mirzoyan, r. Molina, E. Mondal, H.A. Moralejo, A. Morcuende, d. Moreno, V. Nakamori, T. Nanci, C. Nava, L. Neustroev, V. rosillo, M. Nievas Nigro, C. Nilsson, K. Nishijima, K. Ekoume, T. Njoh Noda, K. Nozaki, S. Ohtani, Y. Oka, T. Otero-Santos, J. Paiano, S. Palatiello, M. Paneque, d. Paoletti, r. Paredes, J.M. The University of Tokyo Chiba Kashiwa277-8582 Japan Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna La Laguna TenerifeE-38200 Spain RomeI-00136 Italy Università di Udine INFN Trieste UdineI-33100 Italy Rome Italy Max-Planck-Institut für Physik MünchenD-80805 Germany Università di Padova INFN PadovaI-35131 Italy Bellaterra BarcelonaE-08193 Spain Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain ZeuthenD-15738 Germany ETH Zürich ZürichCH-8093 Switzerland Università di Pisa INFN Pisa PisaI-56126 Italy Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Armenian MAGIC Group A. Alikhanyan National Science Laboratory Yerevan0036 Armenia Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain Department for Physics and Technology University of Bergen Norway University of Innsbruck Institute for Astro and Particle Physics Austria INFN MAGIC Group INFN Sezione di Catania Dipartimento di Fisica e Astronomia University of Catania CataniaI-95123 Italy Bellaterra BarcelonaE-08193 Spain INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino TorinoI-10125 Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica dell’Università e del Politecnico di Bari BariI-70125 Italy Croatian MAGIC Group University of Rijeka Department of Physics Rijeka51000 Croatia Universität Würzburg WürzburgD-97074 Germany University of Geneva Chemin d’Ecogia 16 VersoixCH-1290 Switzerland Finnish MAGIC Group Finnish Centre for Astronomy with ESO University of Turku T

Line-like features in TeV $\gamma$-rays constitute a ''smoking gun'' for TeV-scale particle dark matter and new physics. Probing the Galactic Center region with ground-based Cherenkov telescopes enables the search for TeV spectral features in immediate association with a dense dark matter reservoir at a sensitivity out of reach for satellite $\gamma$-ray detectors, and direct detection and collider experiments. We report on 223 hours of observations of the Galactic Center region with the MAGIC stereoscopic telescope system reaching $\gamma$-ray energies up to 100 TeV. We improved the sensitivity to spectral lines at high energies using large-zenith-angle observations and a novel background modeling method within a maximum-likelihood analysis in the energy domain. No line-like spectral feature is found in our analysis. Therefore, we constrain the cross section for dark matter annihilation into two photons to $\langle \sigma v \rangle \lesssim 5 \times 10^{-28}\,\mathrm{cm^3\,s^{-1}}$ at 1 TeV and $\langle \sigma v \rangle \lesssim 1 \times 10^{-25}\,\mathrm{cm^3\,s^{-1}}$ at 100 TeV, achieving the best limits to date for a dark matter mass above 20 TeV and a cuspy dark matter profile at the Galactic Center. Finally, we use the derived limits for both cuspy and cored dark matter profiles to constrain supersymmetric wino models. Copyright © 2022, The Authors. All rights reserved.

关键词： Galaxies

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