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1p3/2 Proton-Hole State in Sn132 and the Shell Structure Along N=82

Physical Review Letters 2014年第13期112卷 132501-132501页

作者： J. Taprogge A. Jungclaus H. Grawe S. Nishimura P. Doornenbal G. Lorusso G. S. Simpson P.-A. Söderström T. Sumikama Z. Y. Xu H. Baba F. Browne N. Fukuda R. Gernhäuser G. Gey N. Inabe T. Isobe H. S. Jung D. Kameda G. D. Kim Y.-K. Kim I. Kojouharov T. Kubo N. Kurz Y. K. Kwon Z. Li H. Sakurai H. Schaffner K. Steiger H. Suzuki H. Takeda Zs. Vajta H. Watanabe J. Wu A. Yagi K. Yoshinaga G. Benzoni S. Bönig K. Y. Chae L. Coraggio A. Covello J.-M. Daugas F. Drouet A. Gadea A. Gargano S. Ilieva F. G. Kondev T. Kröll G. J. Lane A. Montaner-Pizá K. Moschner D. Mücher F. Naqvi M. Niikura H. Nishibata A. Odahara R. Orlandi Z. Patel Zs. Podolyák A. Wendt Instituto de Estructura de la Materia CSIC E-28006 Madrid Spain Departamento de Física Teórica Universidad Autónoma de Madrid E-28049 Madrid Spain RIKEN Nishina Center RIKEN 2-1 Hirosawa Wako-shi Saitama 351-0198 Japan GSI Helmholtzzentrum für Schwerionenforschung GmbH 64291 Darmstadt Germany LPSC Université Joseph Fourier Grenoble 1 CNRS/IN2P3 Institut National Polytechnique de Grenoble F-38026 Grenoble Cedex France Department of Physics Tohoku University Aoba Sendai Miyagi 980-8578 Japan Department of Physics University of Tokyo Hongo 7-3-1 Bunkyo-ku 113-0033 Tokyo Japan School of Computing Engineering and Mathematics University of Brighton Brighton BN2 4JG United Kingdom Physik Department E12 Technische Universität München D-85748 Garching Germany Institut Laue-Langevin B.P. 156 F-38042 Grenoble Cedex 9 France Department of Physics Chung-Ang University Seoul 156-756 Republic of Korea Rare Isotope Science Project Institute for Basic Science Daejeon 305-811 Republic of Korea Department of Nuclear Engineering Hanyang University Seoul 133-791 Republic of Korea School of Physics and State key Laboratory of Nuclear Physics and Technology Peking University Beijing 100871 China MTA Atomki P.O. Box 51 Debrecen H-4001 Hungary Department of Physics Osaka University Machikaneyama-machi 1-1 Osaka 560-0043 Toyonaka Japan Department of Physics Faculty of Science and Technology Tokyo University of Science 2641 Yamazaki Noda Chiba Japan INFN Sezione di Milano via Celoria 16 I-20133 Milano Italy Institut für Kernphysik Technische Universität Darmstadt D-64289 Darmstadt Germany Department of Physics Sungkyunkwan University Suwon 440-746 Republic of Korea Istituto Nazionale di Fisica Nucleare Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy Dipartimento di Fisica Università di Napoli Federico II Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy CEA DAM DIF 91297 Arpajon cedex France Instituto de Fsica Corpuscular CSIC

A low-lying state in In82131, the one-proton hole nucleus with respect to double magic Sn132, was observed by its γ decay to the Iπ=1/2− β-emitting isomer. We identify the new state at an excitation energy of Ex=1353 keV, which was populated both in the β decay of Cd13183 and after β-delayed neutron emission from Cd13284, as the previously unknown πp3/2 single-hole state with respect to the Sn132 core. Exploiting this crucial new experimental information, shell-model calculations were performed to study the structure of experimentally inaccessible N=82 isotones below Sn132. The results evidence a surprising absence of proton subshell closures along the chain of N=82 isotones. The consequences of this finding for the evolution of the N=82 shell gap along the r-process path are discussed.

关键词： Excited states

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Excited-State Half-Lives in Cd130 and the Isospin Dependence of Effective Charges

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Physical Review Letters 2024年第22期132卷 222501-222501页

作者： A. Jungclaus M. Górska M. Mikołajczuk J. Acosta J. Taprogge S. Nishimura P. Doornenbal G. Lorusso G. S. Simpson P.-A. Söderström T. Sumikama Z. Xu P. Kumar G. Martínez-Pinedo F. Nowacki P. Van Isacker H. Baba F. Browne N. Fukuda R. Gernhäuser G. Gey N. Inabe T. Isobe H. S. Jung D. Kameda G. D. Kim Y.-K. Kim I. Kojouharov T. Kubo N. Kurz Y. K. Kwon Z. Li H. Sakurai H. Schaffner Y. Shimizu K. Steiger H. Suzuki H. Takeda Zs. Vajta H. Watanabe J. Wu A. Yagi K. Yoshinaga G. Benzoni S. Bönig K. Y. Chae J.-M. Daugas F. Drouet A. Gadea S. Ilieva F. G. Kondev T. Kröll G. J. Lane A. Montaner-Pizá K. Moschner F. Naqvi M. Niikura H. Nishibata A. Odahara R. Orlandi Z. Patel Zs. Podolyák A. Wendt Instituto de Estructura de la Materia CSIC E-28006 Madrid Spain GSI Helmholtzzentrum für Schwerionenforschung D-64291 Darmstadt Germany Faculty of Physics University of Warsaw Warsaw PL-02093 Poland Departamento de Física Teórica Universidad Autónoma de Madrid E-28049 Madrid Spain RIKEN Nishina Center RIKEN 2-1 Hirosawa Wako-shi Saitama 351-0198 Japan LPSC Université Joseph Fourier Grenoble 1 CNRS/IN2P3 Institut National Polytechnique de Grenoble F-38026 Grenoble Cedex France Department of Physics Tohoku University Aoba Sendai Miyagi 980-8578 Japan Department of Physics University of Tokyo Hongo 7-3-1 Bunkyo-ku 113-0033 Tokyo Japan Institut für Kernphysik (Theoriezentrum) Fachbereich Physik Technische Universität Darmstadt D-64289 Darmstadt Germany Université de Strasbourg CNRS IPHC UMR Strasbourg 7178 F-67000 France Grand Accélérateur National d’Ions Lourds CEA/DRF–CNRS/IN2P3 F-14076 Caen France School of Computing Engineering and Mathematics University of Brighton Brighton BN2 4GJ United Kingdom Physik Department E12 Technische Universität München D-85748 Garching Germany Institut Laue-Langevin B.P. 156 F-38042 Grenoble Cedex 9 France Department of Physics Chung-Ang University Seoul 156-756 Republic of Korea Rare Isotope Science Project Institute for Basic Science Daejeon 305-811 Republic of Korea Department of Nuclear Engineering Hanyang University Seoul 133-791 Republic of Korea School of Physics and State key Laboratory of Nuclear Physics and Technology Peking University Beijing 100871 China MTA Atomki P.O. Box 51 Debrecen H-4001 Hungary Department of Physics Osaka University Machikaneyama-machi 1-1 Osaka 560-0043 Toyonaka Japan Department of Physics Faculty of Science and Technology Tokyo University of Science 2641 Yamazaki Noda Chiba Japan INFN Sezione di Milano via Celoria 16 I-20133 Milano Italy Institut für Kernphysik Technische Universität Darmstadt D-64289 Darmstadt Germany Department of Physics Sungkyunkwan Univer

The known Iπ=81+, Ex=2129−keV isomer in the semimagic nucleus Cd13082 was populated in the projectile fission of a U238 beam at the Radioactive Isotope Beam Factory at RIKEN. The high counting statistics of the accumulated data allowed us to determine the excitation energy, Ex=2001.2(7) keV, and half-life, T1/2=57(3) ns, of the Iπ=61+ state based on γγ coincidence information. Furthermore, the half-life of the 81+ state, T1/2=224(4) ns, was remeasured with high precision. The new experimental information, combined with available data for Sn134 and large-scale shell model calculations, allowed us to extract proton and neutron effective charges for Sn132, a doubly magic nucleus far-off stability. A comparison to analogous information for Sn100 provides first reliable information regarding the isospin dependence of the isoscalar and isovector effective charges in heavy nuclei.

关键词： Electromagnetic transitions Nuclear structure & decays Shell model

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Euclid preparation. Simulations and nonlinearities beyond ΛCDM. 2. Results from non-standard simulations

arXiv

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arXiv 2024年

作者： Rácz, G. Breton, M.-A. Fiorini, B. Le Brun, A.M.C. Winther, H.-A. Sakr, Z. Pizzuti, L. Ragagnin, A. Gayoux, T. Altamura, E. Carella, E. Pardede, K. Verza, G. Koyama, K. Baldi, M. Pourtsidou, A. Vernizzi, F. Adame, A.G. Adamek, J. Avila, S. Carbone, C. Despali, G. Giocoli, C. Hernández-Aguayo, C. Hassani, F. Kunz, M. Li, B. Rasera, Y. Yepes, G. Gonzalez-Perez, V. Corasaniti, P.-S. García-Bellido, J. Hamaus, N. Kiessling, A. Marinucci, M. Moretti, C. Mota, D.F. Piga, L. Pisani, A. Szapudi, I. Tallada-Crespí, P. Aghanim, N. Andreon, S. Baccigalupi, C. Bardelli, S. Bonino, D. Branchini, E. Brescia, M. Brinchmann, J. Camera, S. Capobianco, V. Cardone, V.F. Carretero, J. Casas, S. Castellano, M. Castignani, G. Cavuoti, S. Cimatti, A. Colodro-Conde, C. Congedo, G. Conselice, C.J. Conversi, L. Copin, Y. Courbin, F. Courtois, H.M. Da Silva, A. Degaudenzi, H. De Lucia, G. Douspis, M. Dubath, F. Duncan, C.A.J. Dupac, X. Dusini, S. Ealet, A. Farina, M. Farrens, S. Ferriol, S. Fosalba, P. Frailis, M. Franceschi, E. Fumana, M. Galeotta, S. Gillis, B. Gómez-Alvarez, P. Grazian, A. Grupp, F. Haugan, S.V.H. Holmes, W. Hormuth, F. Hornstrup, A. Ilić, S. Jahnke, K. Jhabvala, M. Joachimi, B. Keihänen, E. Kermiche, S. Kilbinger, M. Kitching, T. Kubik, B. Kurki-Suonio, H. Lilje, P.B. Lindholm, V. Lloro, I. Mainetti, G. Maiorano, E. Mansutti, O. Marggraf, O. Markovic, K. Martinelli, M. Martinet, N. Marulli, F. Massey, R. Medinaceli, E. Mei, S. Mellier, Y. Meneghetti, M. Meylan, G. Moresco, M. Moscardini, L. Niemi, S.-M. Padilla, C. Paltani, S. Pasian, F. Pedersen, K. Percival, W.J. Pettorino, V. Pires, S. Polenta, G. Poncet, M. Popa, L.A. Raison, F. Rebolo, R. Renzi, A. Rhodes, J. Riccio, G. Romelli, E. Roncarelli, M. Saglia, R. Salvignol, J.-C. Sánchez, A.G. Sapone, D. Sartoris, B. Schirmer, M. Schrabback, T. Secroun, A. Seidel, G. Serrano, S. Sirignano, C. Sirri, G. Stanco, L. Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Department of Physics University of Helsinki P.O. Box 64 00014 Finland Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Campus UAB Carrer de Can Magrans s/n Cerdanyola del Vallés Barcelona08193 Spain Laboratoire Univers et Théorie Observatoire de Paris Université PSL Université Paris Cité CNRS Meudon92190 France Institute of Cosmology and Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom School of Physics and Astronomy Queen Mary University of London Mile End Road LondonE1 4NS United Kingdom Institut d’Astrophysique de Paris UMR 7095 CNRS Sorbonne Université 98 bis boulevard Arago Paris75014 France Institute of Theoretical Astrophysics University of Oslo P.O. Box 1029 Blindern Oslo0315 Norway Institut für Theoretische Physik University of Heidelberg Philosophenweg 16 Heidelberg69120 Germany Université de Toulouse CNRS UPS CNES 14 Av. Edouard Belin Toulouse31400 France Université St Joseph Faculty of Sciences Beirut Lebanon Dipartimento di Fisica "G. Occhialini" Università degli Studi di Milano Bicocca Piazza della Scienza 3 Milano20126 Italy INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Piero Gobetti 93/3 Bologna40129 Italy IFPU Institute for Fundamental Physics of the Universe via Beirut 2 Trieste34151 Italy Dipartimento di Fisica e Astronomia "Augusto Righi" Alma Mater Studiorum Università di Bologna via Piero Gobetti 93/2 Bologna40129 Italy ICSC - Centro Nazionale di Ricerca in High Performance Computing Big Data e Quantum Computing Via Magnanelli 2 Bologna Italy Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy University of Manchester Oxford Road ManchesterM13 9PL United Kingdom INAF-IASF Milano Via Alfonso Corti 12 Milano20133 Italy Dipartimento di Fisica "Aldo Pontremoli" Università degli Studi di Milano Via Celoria 16

The Euclid mission will measure cosmological parameters with unprecedented precision. To distinguish between cosmological models, it is essential to generate realistic mock observables from cosmological simulations that were run in both the standard Λ-cold-dark-matter (ΛCDM) paradigm and in many non-standard models beyond ΛCDM. We present the scientific results from a suite of cosmological N-body simulations using non-standard models including dynamical dark energy, k-essence, interacting dark energy, modified gravity, massive neutrinos, and primordial non-Gaussianities. We investigate how these models affect the large-scale-structure formation and evolution in addition to providing synthetic observables that can be used to test and constrain these models with Euclid data. We developed a custom pipeline based on the Rockstar halo finder and the nbodykit large-scale structure toolkit to analyse the particle output of non-standard simulations and generate mock observables such as halo and void catalogues, mass density fields, and power spectra in a consistent way. We compare these observables with those from the standard ΛCDM model and quantify the deviations. We find that non-standard cosmological models can leave significant imprints on the synthetic observables that we have generated. Our results demonstrate that non-standard cosmological N-body simulations provide valuable insights into the physics of dark energy and dark matter, which is essential to maximising the scientific return of Euclid. © 2024, CC BY.

关键词： Dark energy

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DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements

arXiv

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arXiv 2024年

作者： Adame, A.G. Aguilar, J. Ahlen, S. Alam, S. Alexander, D.M. Prieto, C. Allende Alvarez, M. Alves, O. Anand, A. Andrade, U. Armengaud, E. Avila, S. Aviles, A. Awan, H. Bahr-Kalus, B. Bailey, S. Baltay, C. Bault, A. Behera, J. BenZvi, S. Beutler, F. Bianchi, D. Blake, C. Blum, R. Bonici, M. Brieden, S. Brodzeller, A. Brooks, D. Buckley-Geer, E. Burtin, E. Calderon, R. Canning, R. Rosell, A. Carnero Cereskaite, R. Cervantes-Cota, J.L. Chabanier, S. Chaussidon, E. Chaves-Montero, J. Chebat, D. Chen, S. Chen, X. Claybaugh, T. Cole, S. Cuceu, A. Davis, T.M. Dawson, K. de la Macorra, A. de Mattia, A. Deiosso, N. Dey, A. Dey, B. Ding, Z. Doel, P. Edelstein, J. Eftekharzadeh, S. Eisenstein, D.J. Elbers, W. Elliott, A. Fagrelius, P. Fanning, K. Ferraro, S. Ereza, J. Findlay, N. Flaugher, B. Font-Ribera, A. Forero-Sánchez, D. Forero-Romero, J.E. Frenk, C.S. Garcia-Quintero, C. Garrison, L.H. Gaztañaga, E. Gil-Marín, H. Gontcho, S.A. Gontcho Gonzalez-Morales, A.X. Gonzalez-Perez, V. Gordon, C. Green, D. Gruen, D. Gsponer, R. Gutierrez, G. Guy, J. Hadzhiyska, B. Hahn, C. Hanif, M.M.S. Herrera-Alcantar, H.K. Honscheid, K. Howlett, C. Huterer, D. Iršič, V. Ishak, M. Joyce, R. Juneau, S. Karaçaylı, N.G. Kehoe, R. Kent, S. Kirkby, D. Kong, H. Koposov, S.E. Kremin, A. Krolewski, A. Lahav, O. Lai, Y. Lan, T.-W. Landriau, M. Lang, D. Lasker, J. Le Goff, J.M. Le Guillou, L. Leauthaud, A. Levi, M.E. Li, T.S. Lodha, K. Magneville, C. Manera, M. Margala, D. Martini, P. Matthewson, W. Maus, M. McDonald, P. Medina-Varela, L. Meisner, A. Mena-Fernández, J. Miquel, R. Moon, J. Moore, S. Moustakas, J. Mudur, N. Mueller, E. Muñoz-Gutiérrez, A. Myers, A.D. Nadathur, S. Napolitano, L. Neveux, R. Newman, J.A. Nguyen, N.M. Nie, J. Niz, G. Noriega, H.E. Padmanabhan, N. Paillas, E. Palanque-Delabrouille, N. Pan, J. Penmetsa, S. Percival, W.J. Pieri, M.M. Pinon, M. Poppett, C. Porredon, A. Prada, F. Pérez-Fernández, A. UAM CSIC Universidad Autónoma de Madrid Cantoblanco MadridE-28049 Spain Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Physics Dept. Boston University 590 Commonwealth Avenue BostonMA02215 United States Tata Institute of Fundamental Research Homi Bhabha Road Mumbai400005 India Centre for Extragalactic Astronomy Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Institute for Computational Cosmology Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Tenerife La LagunaE-38206 Spain Instituto de Astrofísica de Canarias C/ Vía Láctea s/n Tenerife La LagunaE-38205 Spain Department of Physics University of Michigan Ann ArborMI48109 United States Leinweber Center for Theoretical Physics University of Michigan 450 Church Street Ann ArborMI48109-1040 United States IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France The Barcelona Institute of Science and Technology Campus UAB Bellaterra Barcelona08193 Spain Instituto de Ciencias Físicas Universidad Autónoma de México Morelos Cuernavaca62210 Mexico Instituto Avanzado de Cosmología A. C. San Marcos 11 - Atenas 202. Magdalena Contreras Ciudad de México10720 Mexico Université Claude Bernard Lyon 1 CNRS IN2P3 IP2I Lyon France Physics Department Yale University P.O. Box 208120 New HavenCT06511 United States Department of Physics and Astronomy University of California Irvine92697 United States Department of Physics Kansas State University 116 Cardwell Hall ManhattanKS66506 United States Department of Physics & Astronomy University of Rochester 206 Bausch and Lomb Hall P.O. Box 270171 RochesterNY14627-0171 United States Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Dipartimento di Fisica "Aldo Pontremoli" Università degli Studi di Milano Via Celoria 16 MilanoI-20133 Italy Centre for Astrophysics &

We present cosmological results from the measurement of clustering of galaxy, quasar and Lyman-α forest tracers from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). We adopt the full-shape (FS) modeling of the power spectrum, including the effects of redshift-space distortions, in an analysis which has been thoroughly validated in a series of supporting papers as summarised in [1]. We combine the full-shape information with DESI’s DR1 constraints from the baryon acoustic oscillations (BAO) of these tracers. In the flat ΛCDM cosmological model, DESI (FS+BAO), combined with a baryon density prior from Big Bang Nucleosynthesis and a weak prior on the scalar spectral index, determines matter density to Ωm = 0.2962 ±0.0095, and the amplitude of mass fluctuations to σ8 = 0.842±0.034. The addition of the cosmic microwave background (CMB) data tightens these constraints to Ωm = 0.3056 ± 0.0049 and σ8 = 0.8121 ± 0.0053, while further addition of the the joint clustering and lensing analysis from the Dark Energy Survey Year-3 (DESY3) data further improves these measurements, and leads to a 0.4% determination of the Hubble constant, H0 = (68.40 ± 0.27) km s−1 Mpc−1. In models with a time-varying dark energy equation of state parametrised by w0 and wa, combinations of DESI (FS+BAO) with CMB and type Ia supernovae continue to show the preference, previously found in the DESI DR1 BAO analysis, for w0 > −1 and wa ν 0 = 0.04 ± 0.22 and Σ0 = 0.044 ± 0.047, again in agreement with general relativity. © 2024, CC BY.

关键词： Dark energy

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DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars

arXiv

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arXiv 2024年

作者： Adame, A.G. Aguilar, J. Ahlen, S. Alam, S. Alexander, D.M. Alvarez, M. Alves, O. Anand, A. Andrade, U. Armengaud, E. Avila, S. Aviles, A. Awan, H. Bailey, S. Baltay, C. Bault, A. Behera, J. BenZvi, S. Beutler, F. Bianchi, D. Blake, C. Blum, R. Brieden, S. Brodzeller, A. Brooks, D. Buckley-Geer, E. Burtin, E. Calderon, R. Canning, R. Rosell, A. Carnero Cereskaite, R. Cervantes-Cota, J.L. Chabanier, S. Chaussidon, E. Chaves-Montero, J. Chen, S. Chen, X. Claybaugh, T. Cole, S. Cuceu, A. Davis, T.M. Dawson, K. de laMacorra, A. de Mattia, A. Deiosso, N. Dey, A. Dey, B. Ding, Z. Doel, P. Edelstein, J. Eftekharzadeh, S. Ferraro, S. Ereza, J. Findlay, N. Flaugher, B. Font-Ribera, A. Forero-Sánchez, D. Forero-Romero, J.E. Garcia-Quintero, C. Garrison, L.H. Gaztañaga, E. Gil-Marín, H. Eisenstein, D.J. Elliott, A. Fagrelius, P. Fanning, K. Gontcho, A. Gonzalez-Morales, A.X. Gonzalez-Perez, V. Gordon, C. Green, D. Gruen, D. Gsponer, R. Gutierrez, G. Guy, J. Hadzhiyska, B. Hahn, C. Hanif, M.M.S. Herrera-Alcantar, H.K. Honscheid, K. Howlett, C. Huterer, D. Iršič, V. Ishak, M. Juneau, S. Karaçaylı, N.G. Kehoe, R. Kent, S. Kirkby, D. Kong, H. Koposov, S.E. Kremin, A. Krolewski, A. Lai, Y. Lan, T.-W. Landriau, M. Lang, D. Lasker, J. Le Goff, J.M. Le Guillou, L. Leauthaud, A. Levi, M.E. Li, T.S. Lodha, K. Magneville, C. Manera, M. Margala, D. Martini, P. Maus, M. McDonald, P. Medina-Varela, L. Meisner, A. Mena-Fernández, J. Miquel, R. Moon, J. Moore, S. Moustakas, J. Mueller, E. Muñoz-Gutiérrez, A. Myers, A.D. Nadathur, S. Napolitano, L. Neveux, R. Newman, J.A. Nguyen, N.M. Nie, J. Niz, G. Noriega, H.E. Padmanabhan, N. Paillas, E. Palanque-Delabrouille, N. Pan, J. Penmetsa, S. Percival, W.J. Pieri, M.M. Pinon, M. Poppett, C. Porredon, A. Prada, F. Pérez-Fernández, A. Pérez-Ràfols, I. Rabinowitz, D. Raichoor, A. Ramírez-Pérez, C. Ramirez-Solano, S. Rashkovetskyi, M. Ravoux, C. Rezaie, M. Rich, J. UAM CSIC Universidad Autónoma de Madrid Cantoblanco MadridE-28049 Spain Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Physics Dept. Boston University 590 Commonwealth Avenue BostonMA02215 United States Tata Institute of Fundamental Research Homi Bhabha Road Mumbai400005 India Centre for Extragalactic Astronomy Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Institute for Computational Cosmology Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Department of Physics University of Michigan Ann ArborMI48109 United States Leinweber Center for Theoretical Physics University of Michigan 450 Church Street Ann ArborMI48109-1040 United States IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France The Barcelona Institute of Science and Technology Campus UAB Bellaterra Barcelona08193 Spain Instituto de Ciencias Físicas Universidad Autónoma de México Morelos Cuernavaca62210 Mexico Instituto Avanzado de Cosmología A. C. San Marcos 11 - Atenas 202. Magdalena Contreras Ciudad de México10720 Mexico Physics Department Yale University P.O. Box 208120 New HavenCT06511 United States Department of Physics and Astronomy University of California Irvine92697 United States Department of Physics Kansas State University 116 Cardwell Hall ManhattanKS66506 United States Department of Physics & Astronomy University of Rochester 206 Bausch and Lomb Hall P.O. Box 270171 RochesterNY14627-0171 United States Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Dipartimento di Fisica "Aldo Pontremoli" Università degli Studi di Milano Via Celoria 16 MilanoI-20133 Italy Centre for Astrophysics & Supercomputing Swinburne University of Technology P.O. Box 218 HawthornVIC3122 Australia NSF NOIRLab 950 N. Cherry Ave. TucsonAZ85719 United States Department of Physics & Astronomy Un

We present the measurements and cosmological implications of the galaxy two-point clustering using over 4.7 million unique galaxy and quasar redshifts in the range 0.1 b, and a weak Gaussian prior on the spectral index, ns, we constrain the matter density is Ωm = 0.296±0.010 and the Hubble constant H0 = (68.63±0.79)[km s−1Mpc−1]. Additionally, we measure the amplitude of clustering σ8 = 0.841 ± 0.034. The DESI DR1 galaxy clustering results are in agreement with the ΛCDM model based on general relativity with parameters consistent with those from Planck. The cosmological interpretation of these results in combination with DESI DR1 Ly-α forest data and external datasets are presented in the companion paper [1]. © 2024, CC BY.

关键词： Systematic errors

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Snowmass2021 Cosmic Frontier CF6 White Paper: Multi-Experiment Probes for Dark Energy - Transients

arXiv

引用

arXiv 2022年

作者： Kim, Alex G. Palmese, Antonella Pereira, Maria E.S. Aldering, Greg Andrade-Oliveira, Felipe Annis, James Bailey, Stephen BenZvi, Segev Braga-Neto, Ulysses Courbin, Frédéric Garcia, Alyssa Jeffery, David Narayan, Gautham Perlmutter, Saul Soares-Santos, Marcelle Treu, Tommaso Wang, Lifan Aguiar, Odylio D. Akrami, Yashar Birrer, Simon Bom, Clécio R. Buckley-Geer, Elizabeth Cabuk, Nazim Cabuk, Senem Cadonati, Laura Caliskan, Mesut Chen, Thomas Y. Davis, Tamara M. Eskilt, Johannes R. Esteves, Johnny Ferraro, Simone Fisher, Robert Gamezo, Vadim N. García-Bellido, Juan Gill, Mandeep S.S. Herner, Kenneth Huterer, Dragan Ishak, Mustapha Iyer, Bala Jin, Shang-Jie Kilpatrick, Charles D. Koopmans, Léon V.E. Lagos, Macarena Lahav, Ofer Makler, Martín Nugent, Peter Nunes, Rafael C. Poludnenko, Alexei Y. Radice, David Rao, Suvrat Santana-Silva, Luidhy Sasaki, Misao Sathyaprakash, Bangalore Shafieloo, Arman Shao, Lijing Sherman, Nora Singh, Rajeev Smith, Joshua Tohuvavohu, Aaron Physics Division Lawrence Berkeley National Laboratory Berkeley94720 CA United States Department of Physics University of California Berkeley 366 LeConte Hall MC 7300 BerkeleyCA94720 United States NASA Einstein Germany Hamburger Sternwarte Universität Hamburg Gojenbergsweg 112 Hamburg21029 Germany Department of Physics University of Michigan Ann ArborMI48109 United States Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Department of Physics and Astronomy University of Rochester RochesterNY14627 United States Department of Physics and Astronomy Texas A&M University College StationTX77845 United States Observatoire de Sauverny Versoix1290 Switzerland Department of Physics and Astronomy University of Nevada United States University of Illinois at Urbana-Champaign UrbanaIL61801 United States Department of Physics and Astronomy University of California Los AngelesCA90095-1547 United States Instituto Nacional de Pesquisas Espaciais São José dos Campos São Paulo12227-010 Brazil CERCA ISO Department of Physics Case Western Reserve University 10900 Euclid Avenue ClevelandOH44106 United States Department of Physics Imperial College London Blackett Laboratory Prince Consort Road LondonSW7 2AZ United Kingdom Laboratoire de Physique de l'École Normale Supérieure ENS Université PSL CNRS Sorbonne Université Université de Paris ParisF-75005 France Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States Centro Brasileiro de Pesquisas Físicas Rua Dr. Xavier Sigaud 150 RJ Rio de JaneiroCEP 22290-180 Brazil Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Faculty of Engineering Department of Physics Engineering Ankara University Turkey Faculty of Science Department of Astronomy and Space Sciences Ankara University Turkey Center for Relativistic Astrophysics School of Physics Georgia Inst

This invited Snowmass 2021 White Paper highlights the power of joint-analysis of astronomical transients in advancing HEP Science and presents research activities that can realize the opportunities that come with current and upcoming projects. Transients of interest include gravitational wave events, neutrino events, strongly-lensed quasars and supernovae, and Type Ia supernovae specifically. These transients can serve as probes of cosmological distances in the Universe and as cosmic laboratories of extreme strong-gravity, high-energy physics. Joint analysis refers to work that requires significant coordination from multiple experiments or facilities so encompasses Multi-Messenger Astronomy and optical transient discovery and distributed follow-up programs. Copyright © 2022, The Authors. All rights reserved.

关键词： Probes

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Application of pattern spectra and convolutional neural networks to the analysis of simulated Cherenkov Telescope Array data

arXiv

引用

arXiv 2021年

作者： Aschersleben, Jann Peletier, R.F. Vecchi, M. Wilkinson, M.H.F. Abdalla, H. Abe, H. Abe, S. Abusleme, A. Acero, F. Acharyya, A. Portella, V. Acín Ackley, K. Adam, R. Adams, C. Adhikari, S.S. Aguado-Ruesga, I. Agudo, I. Aguilera, R. Aguirre-Santaella, A. Aharonian, F. Alberdi, A. Alfaro, R. Alfaro, J. Alispach, C. Aloisio, R. Batista, R. Alves Amans, J.-P. Amati, L. Amato, E. Ambrogi, L. Ambrosi, G. Ambrosio, M. Ammendola, R. Anderson, J. Anduze, M. Angüner, E.O. Antonelli, L.A. Antonuccio, V. Antoranz, P. Anutarawiramkul, R. Gutierrez, J. Aragunde Aramo, C. Araudo, A. Araya, M. Arbet-Engels, A. Arcaro, C. Arendt, V. Armand, C. Armstrong, T. Arqueros, F. Arrabito, L. Arsioli, B. Artero, M. Asano, K. Ascasíbar, Y. Ashley, M. Attinà, P. Aubert, P. Singh, C.B. Baack, D. Babic, A. Backes, M. Baena, V. Bajtlik, S. Baktash, A. Balazs, C. Balbo, M. Ballester, O. Ballet, J. Balmaverde, B. Bamba, A. Bandiera, R. Larriva, A. Baquero Barai, P. Barbier, C. Martins, V. Barbosa Barcelo, M. Barkov, M. Barnard, M. Baroncelli, L. de Almeida, U. Barres Barrio, J.A. Bastieri, D. Batista, P.I. Batkovic, I. Bauer, C. Bautista-González, R. Baxter, J. Becciani, U. González, J. Becerra Becherini, Y. Beck, G. Tjus, J. Becker Bednarek, W. Belfiore, A. Bellizzi, L. Belmont, R. Benbow, W. Berge, D. Bernardini, E. Bernardos, M.I. Bernlöhr, K. Berti, A. Berton, M. Bertucci, B. Beshley, V. Bhatt, N. Bhattacharyya, S. Bhattacharyya, W. Bhattacharyya, S. Bi, B. Bicknell, G. Biederbeck, N. Bigongiari, C. Biland, A. Bird, R. Bissaldi, E. Biteau, J. Bitossi, M. Blanch, O. Blank, M. Blazek, J. Bobin, J. Boccato, C. Bocchino, F. Boehm, C. Bohacova, M. Boisson, C. Boix, J. Bolle, J.-P. Bolmont, J. Bonanno, G. Bonavolontà, C. Arbeletche, L. Bonneau Bonnoli, G. Bordas, P. Borkowski, J. Bórquez, S. Bose, R. Bose, D. Bosnjak, Z. Bottacini, E. Böttcher, M. Botticella, M.T. Boutonnet, C. Bouyjou, F. Bozhilov, V. Bozzo, E. Brahimi, L. Braiding, C. Brau-Nogué, S. Breen, S. Kapteyn Astronomical Institute University of Groningen PO Box 800 Groningen9700 AV Netherlands Bernoulli Institute for Mathematics Computer Science and Artificial Intelligence University of Groningen PO Box 407 AK GroningenNL-9700 Netherlands Centre for Space Research North-West University Potchefstroom2520 South Africa Institute for Cosmic Ray Research University of Tokyo 5-1-5 Kashiwa-no-ha Chiba Kashiwa277-8582 Japan Pontificia Universidad Católica de Chile Av. Libertador Bernardo O'Higgins 340 Santiago Chile AIM CEA CNRS Université Paris-Saclay Université Paris Diderot Sorbonne Paris Cité CEA Paris-Saclay IRFU/DAp Bat 709 Orme des Merisiers Gif-sur-Yvette91191 France Centre for Advanced Instrumentation Dept. of Physics Durham University South Road DurhamDH1 3LE United Kingdom Port d'Informació Científica Edifici D Carrer de l'Albareda Cerdanyola del Vallès Bellaterrra08193 Spain School of Physics and Astronomy Monash University MelbourneVIC3800 Australia Palaiseau91128 France Department of Physics Columbia University 538 West 120th Street New YorkNY10027 United States University of Oslo Department of Physics Sem Saelandsvei 24 - PO Box 1048 Blindern OsloN-0316 Norway EMFTEL Department IPARCOS Universidad Complutense de Madrid Madrid28040 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain Campus UAB Carrer de Can Magrans s/n Cerdanyola del Vallés08193 Spain Instituto de Física Teórica UAM/CSIC Departamento de Física Teórica Universidad Autónoma de Madrid Campus de Cantoblanco UAM c/ Nicolás Cabrera 13-15 Madrid28049 Spain Dublin Institute for Advanced Studies 31 Fitzwilliam Place Dublin 2 Ireland Universidad Nacional Autónoma de México Delegación Coyoacán Ciudad de México04510 Mexico University of Geneva Département de Physique Nucléaire et Corpusculaire 24 rue du Général-Dufour Genève 41211 Switzerland INFN Dipartimento di Scienze Fisiche e Chimiche Università

The Cherenkov Telescope Array (CTA) will be the next generation gamma-ray observatory and will be the major global instrument for very-high-energy astronomy over the next decade, offering 5 - 10 × better flux sensitivity than current generation gamma-ray telescopes. Each telescope will provide a snapshot of gamma-ray induced particle showers by capturing the induced Cherenkov emission at ground level. The simulation of such events provides images that can be used as training data for convolutional neural networks (CNNs) to determine the energy of the initial gamma rays. Compared to other state-of-the-art algorithms, analyses based on CNNs promise to further enhance the performance to be achieved by CTA. Pattern spectra are commonly used tools for image classification and provide the distributions of the shapes and sizes of various objects comprising an image. The use of relatively shallow CNNs on pattern spectra would automatically select relevant combinations of features within an image, taking advantage of the 2D nature of pattern spectra. In this work, we generate pattern spectra from simulated gamma-ray events instead of using the raw images themselves in order to train our CNN for energy reconstruction. This is different from other relevant learning and feature selection methods that have been tried in the past. Thereby, we aim to obtain a significantly faster and less computationally intensive algorithm, with minimal loss of performance. © 2021, CC BY.

关键词： Gamma rays

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HAWC J2227+610: A potential PeVatron candidate for the CTA in the northern hemisphere

arXiv

引用

arXiv 2021年

作者： Abdalla, H. Abe, H. Abe, S. Abusleme, A. Acero, F. Acharyya, A. Acín Portella, V. Ackley, K. Adam, R. Adams, C. Adhikari, S.S. Aguado-Ruesga, I. Agudo, I. Aguilera, R. Aguirre-Santaella, A. Aharonian, F. Alberdi, A. Alfaro, R. Alfaro, J. Alispach, C. Aloisio, R. Alves Batista, R. Amans, J.-P. Amati, L. Amato, E. Ambrogi, L. Ambrosi, G. Ambrosio, M. Ammendola, R. Anderson, J. Anduze, M. Angüner, E.O. Antonelli, L.A. Antonuccio, V. Antoranz, P. Anutarawiramkul, R. Aragunde Gutierrez, J. Aramo, C. Araudo, A. Araya, M. Arbet-Engels, A. Arcaro, C. Arendt, V. Armand, C. Armstrong, T. Arqueros, F. Arrabito, L. Arsioli, B. Artero, M. Asano, K. Ascasíbar, Y. Aschersleben, J. Ashley, M. Attinà, P. Aubert, P. Singh, C.B. Baack, D. Babic, A. Backes, M. Baena, V. Bajtlik, S. Baktash, A. Balazs, C. Balbo, M. Ballester, O. Ballet, J. Balmaverde, B. Bamba, A. Bandiera, R. Baquero Larriva, A. Barai, P. Barbier, C. Barbosa Martins, V. Barcelo, M. Barkov, M. Barnard, M. Baroncelli, L. Barres de Almeida, U. Barrio, J.A. Bastieri, D. Batista, P.I. Batkovic, I. Bauer, C. Bautista-González, R. Baxter, J. Becciani, U. Becerra González, J. Becherini, Y. Beck, G. Becker Tjus, J. Bednarek, W. Belfiore, A. Bellizzi, L. Belmont, R. Benbow, W. Berge, D. Bernardini, E. Bernardos, M.I. Bernlöhr, K. Berti, A. Berton, M. Bertucci, B. Beshley, V. Bhatt, N. Bhattacharyya, S. Bhattacharyya, W. Bhattacharyya, S. Bi, B. Bicknell, G. Biederbeck, N. Bigongiari, C. Biland, A. Bird, R. Bissaldi, E. Biteau, J. Bitossi, M. Blanch, O. Blank, M. Blazek, J. Bobin, J. Boccato, C. Bocchino, F. Boehm, C. Bohacova, M. Boisson, C. Boix, J. Bolle, J.-P. Bolmont, J. Bonanno, G. Bonavolontà, C. Bonneau Arbeletche, L. Bonnoli, G. Bordas, P. Borkowski, J. Bórquez, S. Bose, R. Bose, D. Bosnjak, Z. Bottacini, E. Böttcher, M. Botticella, M.T. Boutonnet, C. Bouyjou, F. Bozhilov, V. Bozzo, E. Brahimi, L. Braiding, C. Brau-Nogué, S. Breen, S. Bregeon, J. Breuhaus, M. Brill, A. Brisken, W. Brocato, E. Aix Marseille Univ CNRS IN2P3 CPPM Marseille France Centre for Space Research North-West University Potchefstroom2520 South Africa Institute for Cosmic Ray Research University of Tokyo 5-1-5 Kashiwa-no-ha Chiba Kashiwa277-8582 Japan Pontificia Universidad Católica de Chile Av. Libertador Bernardo O'Higgins 340 Santiago Chile AIM CEA CNRS Université Paris-Saclay Université Paris Diderot Sorbonne Paris Cité CEA Paris-Saclay IRFU DAp Bat 709 Orme des Merisiers Gif-sur-Yvette 91191 France Centre for Advanced Instrumentation Dept. of Physics Durham University South Road DurhamDH1 3LE United Kingdom 08193 Spain School of Physics and Astronomy Monash University MelbourneVIC3800 Australia Laboratoire Leprince-Ringuet École Polytechnique UMR 7638 CNRS IN2P3 Institut Polytechnique de Paris Palaiseau91128 France Department of Physics Columbia University 538 West 120th Street New YorkNY10027 United States University of Oslo Department of Physics Sem Saelandsvei 24 - PO Box 1048 Blindern OsloN-0316 Norway EMFTEL Department IPARCOS Universidad Complutense de Madrid Madrid28040 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain Campus UAB Carrer de Can Magrans s/n Cerdanyola del Vallés 08193 Spain Instituto de Física Teórica UAM/CSIC Departamento de Física Teórica Universidad Autónoma de Madrid Campus de Cantoblanco UAM c/Nicolás Cabrera 13-15 Madrid28049 Spain Dublin Institute for Advanced Studies 31 Fitzwilliam Place Dublin 2 Ireland Universidad Nacional Autónoma de México Delegación Coyoacán Ciudad de México04510 Mexico University of Geneva Département de Physique Nucléaire et Corpusculaire 24 rue du Général-Dufour Genève 41211 Switzerland INFN Dipartimento di Scienze Fisiche e Chimiche Università degli Studi dell'Aquila Gran Sasso Science Institute Via Vetoio 1 Viale Crispi 7 L'Aquila67100 Italy Instituto de Astronomia Geofísico e Ciências Atmosféricas Universidade de S

Recent observations of the gamma-ray source HAWC J2227+610 by Tibet AS+MD and LHAASO confirm the special interest of this source as a galactic PeVatron candidate in the northern hemisphere. HAWC J2227+610 emits Very High Energy (VHE) gamma-rays up to 500 TeV, from a region coincident with molecular clouds and significantly displaced from the nearby pulsar J2229+6114. Even if this morphology favours an hadronic origin, both leptonic or hadronic models can describe the current VHE gamma-ray emission. The morphology of the source is not well constrained by the present measurements and a better characterisation would greatly help the understanding of the underlying particle acceleration mechanisms. The Cherenkov Telescope Array (CTA) will be the future most sensitive Imaging Atmospheric Cherenkov Telescope and, thanks to its unprecedented angular resolution, could contribute to better constrain the nature of this source. The present work investigates the potentiality of CTA to study the morphology and the spectrum of HAWC J2227+610. For this aim, the source is simulated assuming the hadronic model proposed by the Tibet AS+MD collaboration, recently fitted on multi-wavelength data, and two spatial templates associated to the source nearby molecular clouds. Different CTA layouts and observation times are considered. A 3D map based analysis shows that CTA is able to significantly detect the extension of the source and to attribute higher detection significance to the simulated molecular cloud template compared to the alternative one. CTA data does not allow to disentangle the hadronic and the leptonic emission models. However, it permits to correctly reproduce the simulated parent proton spectrum characterized by a ∼ 500 TeV cutoff. © 2021, CC BY-NC-SA.

关键词： Morphology

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Searching for continuous Gravitational Waves in the second data release of the International Pulsar Timing Array

arXiv

引用

arXiv 2023年

作者： Falxa, M. Babak, S. Baker, P.T. Bécsy, B. Chalumeau, A. Chen, S. Chen, Z. Cornish, N.J. Guillemot, L. Hazboun, J.S. Mingarelli, C.M.F. Parthasarathy, A. Petiteau, A. Pol, N.S. Sesana, A. Spolaor, S.B. Taylor, S.R. Theureau, G. Vallisneri, M. Vigeland, S.J. Witt, C.A. Zhu, X. Antoniadis, J. Arzoumanian, Z. Bailes, M. Bhat, N.D.R. Blecha, L. Brazier, A. Brook, P.R. Caballero, N. Cameron, A.D. Casey-Clyde, J.A. Champion, D. Charisi, M. Chatterjee, S. Cognard, I. Cordes, J.M. Crawford, F. Cromartie, H.T. Crowter, K. Dai, S. DeCesar, M.E. Demorest, P.B. Desvignes, G. Dolch, T. Drachler, B. Feng, Y. Ferrara, E.C. Fiore, W. Fonseca, E. Garver-Daniels, N. Glaser, J. Goncharov, B. Good, D.C. Griessmeier, J. Guo, Y.J. Gültekin, K. Hobbs, G. Hu, H. Islo, K. Jang, J. Jennings, R.J. Johnson, A.D. Jones, M.L. Kaczmarek, J. Kaiser, A.R. Kaplan, D.L. Keith, M. Kelley, L.Z. Kerr, M. Key, J.S. Laal, N. Lam, M.T. Lamb, W.G. Lazio, T.J.W. Liu, K. Liu, T. Luo, J. Lynch, R.S. Madison, D.R. Main, R. Manchester, R. McEwen, A. McKee, J. McLaughlin, M.A. Ng, C. Nice, D.J. Ocker, S. Olum, K.D. Oslowski, S. Pennucci, T.T. Perera, B.B.P. Perrodin, D. Porayko, N. Possenti, A. Quelquejay-Leclere, H. Ransom, S.M. Ray, P.S. Reardon, D.J. Russell, C.J. Samajdar, A. Sarkissian, J. Schult, L. Shaifullah, G. Shannon, R.M. Shapiro-Albert, B.J. Siemens, X. Simon, J.J. Siwek, M. Smith, T.L. Speri, L. Spiewak, R. Stairs, I.H. Stappers, B. Stinebring, D.R. Swiggum, J.K. Tiburzi, C. Turner, J. Vecchio, A. Verbiest, J.P.W. Wahl, H. Wang, S.Q. Wang, J. Wang, J. Wu, Z. Zhang, L. Zhang, S. Université de Paris CNRS Astroparticule et Cosmologie Paris75013 France Department of Physics and Astronomy Widener University One University Place ChesterPA19013 United States Department of Physics Montana State University BozemanMT59717 United States Dipartimento di Fisica "G. Occhialini" Universitá degli Studi di Milano-Bicocca Piazza della Scienza 3 Milano20126 Italy Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy Beijing Normal University Beijing100875 China Station de Radioastronomie de Nançay Observatoire de Paris PSL University CNRS Université d’Orléans Nançay18330 France Laboratoire de Physique et Chimie de l’Environnement et de l’Espace LPC2E UMR7328 Université d’Orléans CNRS Orléans45071 France Department of Physics Oregon State University CorvallisOR97331 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Department of Physics University of Connecticut 196 Auditorium Road U-3046 StorrsCT06269-3046 United States Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France Department of Physics and Astronomy Vanderbilt University 2301 Vanderbilt Place NashvilleTN37235 United States INFN Sezione di Milano-Bicocca Piazza della Scienza 3 Milano20126 Italy Department of Physics and Astronomy West Virginia University P.O. Box 6315 MorgantownWV26506 United States Laboratoire Univers et Théories LUTh Observatoire de Paris Université PSL CNRS Université de Paris Meudon92190 France Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Center for Gravitation Cosmology and Astrophysics Department of Physics University of Wisconsin-Milwaukee P.O. Box 413 MilwaukeeWI53201 United States Northwestern University EvanstonIL60208 United States Adler Planet

The International Pulsar Timing Array 2nd data release is the combination of datasets from worldwide collaborations. In this study, we search for continuous waves: gravitational wave signals produced by individual supermassive black hole binaries in the local universe. We consider binaries on circular orbits and neglect the evolution of orbital frequency over the observational span. We find no evidence for such signals and set sky averaged 95% upper limits on their amplitude h95. The most sensitive frequency is 10nHz with ℎ95 = 9.1 × 10−15. We achieved the best upper limit to date at low and high frequencies of the PTA band thanks to improved effective cadence of observations. In our analysis, we have taken into account the recently discovered common red noise process, which has an impact at low frequencies. We also find that the peculiar noise features present in some pulsars data must be taken into account to reduce the false alarm. We show that using custom noise models is essential in searching for continuous gravitational wave signals and setting the upper limit. Copyright © 2023, The Authors. All rights reserved.

关键词： Pulsars

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Reconstruction of stereoscopic CTA events using deep learning with CTLearn

arXiv

引用

arXiv 2021年

作者： Miener, Tjark Nieto, Daniel Brill, Aryeh Spencer, Samuel Contreras, Jose Luis Abdalla, H. Abe, H. Abe, S. Abusleme, A. Acero, F. Acharyya, A. Portella, V. Acín Ackley, K. Adam, R. Adams, C. Adhikari, S.S. Aguado-Ruesga, I. Agudo, I. Aguilera, R. Aguirre-Santaella, A. Aharonian, F. Alberdi, A. Alfaro, R. Alfaro, J. Alispach, C. Aloisio, R. Batista, R. Alves Amans, J.-P. Amati, L. Amato, E. Ambrogi, L. Ambrosi, G. Ambrosio, M. Ammendola, R. Anderson, J. Anduze, M. Angüner, E.O. Antonelli, L.A. Antonuccio, V. Antoranz, P. Anutarawiramkul, R. Gutierrez, J. Aragunde Aramo, C. Araudo, A. Araya, M. Arbet-Engels, A. Arcaro, C. Arendt, V. Armand, C. Armstrong, T. Arqueros, F. Arrabito, L. Arsioli, B. Artero, M. Asano, K. Ascasíbar, Y. Aschersleben, J. Ashley, M. Attinà, P. Aubert, P. Singh, C.B. Baack, D. Babic, A. Backes, M. Baena, V. Bajtlik, S. Baktash, A. Balazs, C. Balbo, M. Ballester, O. Ballet, J. Balmaverde, B. Bamba, A. Bandiera, R. Larriva, A. Baquero Barai, P. Barbier, C. Martins, V. Barbosa Barcelo, M. Barkov, M. Barnard, M. Baroncelli, L. Barres de Almeida, U. Barrio, J.A. Bastieri, D. Batista, P.I. Batkovic, I. Bauer, C. Bautista-González, R. Baxter, J. Becciani, U. González, J. Becerra Becherini, Y. Beck, G. Tjus, J. Becker Bednarek, W. Belfiore, A. Bellizzi, L. Belmont, R. Benbow, W. Berge, D. Bernardini, E. Bernardos, M.I. Bernlöhr, K. Berti, A. Berton, M. Bertucci, B. Beshley, V. Bhatt, N. Bhattacharyya, S. Bhattacharyya, W. Bhattacharyya, S. Bi, B. Bicknell, G. Biederbeck, N. Bigongiari, C. Biland, A. Bird, R. Bissaldi, E. Biteau, J. Bitossi, M. Blanch, O. Blank, M. Blazek, J. Bobin, J. Boccato, C. Bocchino, F. Boehm, C. Bohacova, M. Boisson, C. Boix, J. Bolle, J.-P. Bolmont, J. Bonanno, G. Bonavolontà, C. Arbeletche, L. Bonneau Bonnoli, G. Bordas, P. Borkowski, J. Bórquez, S. Bose, R. Bose, D. Bosnjak, Z. Bottacini, E. Böttcher, M. Botticella, M.T. Boutonnet, C. Bouyjou, F. Bozhilov, V. Bozzo, E. Brahimi, L. Braiding, C. Centre for Space Research North-West University Potchefstroom2520 South Africa Institute for Cosmic Ray Research University of Tokyo 5-1-5 Kashiwa-no-ha Chiba Kashiwa277-8582 Japan Pontificia Universidad Católica de Chile Av. Libertador Bernardo O'Higgins 340 Santiago Chile AIM CEA CNRS Université Paris-Saclay Université Paris Diderot Sorbonne Paris Cité CEA Paris-Saclay IRFU DAp Bat 709 Orme des Merisiers Gif-sur-Yvette91191 France Centre for Advanced Instrumentation Dept. of Physics Durham University South Road DurhamDH1 3LE United Kingdom Port d'Informació Científica Edifici D Carrer de l'Albareda Cerdanyola del Vallès Bellaterrra08193 Spain School of Physics and Astronomy Monash University MelbourneVIC3800 Australia Laboratoire Leprince-Ringuet École Polytechnique UMR 7638 CNRS IN2P3 Institut Polytechnique de Paris Palaiseau91128 France Department of Physics Columbia University 538 West 120th Street New YorkNY10027 United States University of Oslo Department of Physics Sem Saelandsvei 24 - PO Box 1048 Blindern OsloN-0316 Norway EMFTEL Department IPARCOS Universidad Complutense de Madrid Madrid28040 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain Campus UAB Carrer de Can Magrans s/n Cerdanyola del Vallés08193 Spain Instituto de Física Teórica UAM/CSIC Departamento de Física Teórica Universidad Autónoma de Madrid Campus de Cantoblanco UAM c/Nicolás Cabrera 13-15 Madrid28049 Spain Dublin Institute for Advanced Studies 31 Fitzwilliam Place Dublin 2 Ireland Universidad Nacional Autónoma de México Delegación Coyoacán Ciudad de México04510 Mexico University of Geneva Département de physique nucléaire et corpusculaire 24 rue du Général-Dufour Genève 41211 Switzerland INFN Dipartimento di Scienze Fisiche e Chimiche Università degli Studi dell'Aquila Gran Sasso Science Institute Via Vetoio 1 Viale Crispi 7 L'Aquila67100 Italy Instituto de Astronomia Geofísico e Ci

The Cherenkov Telescope Array (CTA), conceived as an array of tens of imaging atmospheric Cherenkov telescopes (IACTs), is an international project for a next-generation ground-based gamma-ray observatory, aiming to improve on the sensitivity of current-generation instruments a factor of five to ten and provide energy coverage from 20 GeV to more than 300 TeV. Arrays of IACTs probe the very-high-energy gamma-ray sky. Their working principle consists of the simultaneous observation of air showers initiated by the interaction of very-high-energy gamma rays and cosmic rays with the atmosphere. Cherenkov photons induced by a given shower are focused onto the camera plane of the telescopes in the array, producing a multi-stereoscopic record of the event. This image contains the longitudinal development of the air shower, together with its spatial, temporal, and calorimetric information. The properties of the originating very-high-energy particle (type, energy, and incoming direction) can be inferred from those images by reconstructing the full event using machine learning techniques. In this contribution, we present a purely deep-learning driven, full-event reconstruction of simulated, stereoscopic IACT events using CTLearn. CTLearn is a package that includes modules for loading and manipulating IACT data and for running deep learning models, using pixel-wise camera data as input. © 2021, CC BY-NC-SA.

关键词： Cameras

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