检索结果-内蒙古大学图书馆

Extending the π-Conjugated System in Spiro-Type Hole Transport Material Enhances the Efficiency and Stability of Perovskite Solar Modules

引用

Angewandte Chemie 2023年第29期135卷

作者： Xuepeng Liu Bin Ding Mingyuan Han Zhenhai Yang Jianlin Chen Pengju Shi Xiangying Xue Rahim Ghadari Xianfu Zhang Rui Wang Keith Brooks Li Tao Sachin Kinge Songyuan Dai Jiang Sheng Paul J. Dyson Mohammad Khaja Nazeeruddin Yong Ding Beijing Key Laboratory of Novel Thin-Film Solar Cells School of New Energy North China Electric Power University Beijing 102206 P. R. China Contribution: Investigation (lead) Institute of Chemical Sciences and Engineering École Polytechnique Fédérale de Lausanne (EPFL) 1015 Lausanne Switzerland Contribution: Methodology (lead) Contribution: Methodology (equal) Ningbo Institute of Materials Technology and Engineering Chinese Academy of Sciences (CAS) Ningbo 315201 China Contribution: Data curation (equal) Contribution: Validation (equal) School of Engineering Westlake University Hangzhou 310024 China Contribution: Formal analysis (equal) Contribution: Investigation (equal) Computational Chemistry Laboratory Department of Organic and Biochemistry Faculty of Chemistry University of Tabriz Tabriz *** Iran Contribution: Software (lead) Contribution: Visualization (equal) School of Microelectronic & Faculty of Physics and Electronic Science Hubei University Wuhan 430062 China Toyota Motor Europe Toyota Motor Technical Centre Advanced Technology Div. Hoge Wei 33 1930 Zaventum Belgium Contribution: Resources (equal) Contribution: Supervision (equal) Contribution: Writing - original draft (equal) Writing - review & editing (equal) Contribution: Conceptualization (equal) Writing - original draft (equal) Writing - review & editing (equal) Contribution: Supervision (equal) Writing - original draft (lead)

Hole transport materials (HTMs) are a key component of perovskite solar cells (PSCs). The small molecular 2,2′,7,7′-tetrakis(N,N-di-p-methoxyphenyl)-amine-9,9′-spirobifluorene (spiro-OMeTAD, termed “Spiro”) is the most successful HTM used in PSCs, but its versatility is imperfect. To improve its performance, we developed a novel spiro-type HTM (termed “DP”) by substituting four anisole units on Spiro with 4-methoxybiphenyl moieties. By extending the π-conjugation of Spiro in this way, the HOMO level of the HTM matches well with the perovskite valence band, enhancing hole mobility and increasing the glass transition temperature. DP-based PSC achieves high power conversion efficiencies (PCEs) of 25.24 % for small-area (0.06 cm 2 ) devices and 21.86 % for modules (designated area of 27.56 cm 2 ), along with the certified efficiency of 21.78 % on a designated area of 27.86 cm 2 . The encapsulated DP-based devices maintain 95.1 % of the initial performance under ISOS-L-1 conditions after 2560 hours and 87 % at the ISOS-L-3 conditions over 600 hours.

关键词： Hole Transport Materials Modules Perovskite Solar Cells π-Conjugated System Stability

来源：评论

学校读者我要写书评

暂无评论

SEARCH FOR NEW COSMIC-RAY ACCELERATION SITES WITHIN THE 4FGL CATALOG GALACTIC PLANE SOURCES

arXiv

引用

arXiv 2022年

作者： Abdollahi, S. Acero, F. Ackermann, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Berenji, B. Berretta, A. Bissaldi, E. Blandford, R.D. Bonino, R. Bruel, P. Buson, S. Cameron, R.A. Caputo, R. Caraveo, P.A. castro, D. Chiaro, G. Cibrario, N. Ciprini, S. Coronado-Blázquez, J. Crnogorcevic, M. Cutini, S. D'Ammando, F. De Gaetano, S. Di Lalla, N. Dirirsa, F. Di Venere, L. Domínguez, A. Fegan, S.J. Fiori, A. Fleischhack, H. Franckowiak, A. Fukazawa, Y. Fusco, P. Gammaldi, V. Gargano, F. Gasparrini, D. Giacchino, F. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Green, D. Grenier, I.A. Grondin, M.-H. Guiriec, S. Gustafsson, M. Harding, A.K. Hays, E. Hewitt, J.W. Horan, D. Hou, X. Jóhannesson, G. Kayanoki, T. Kerr, M. Kuss, M. Larsson, S. Latronico, L. Lemoine-Goumard, M. Li, J. Longo, F. Loparco, F. Lubrano, P. Maldera, S. Malyshev, D. Manfreda, A. Martí-Devesa, G. Mazziotta, M.N. Mereu, I. Michelson, P.F. Mirabal, N. Mitthumsiri, W. Mizuno, T. Monzani, M.E. Morselli, A. Moskalenko, I.V. Nuss, E. Omodei, N. Orienti, M. Orlando, E. Ormes, J.F. Paneque, D. Pei, Z. Persic, M. Pesce-Rollins, M. Pillera, R. Poon, H. Porter, T.A. Principe, G. Rainò, S. Rando, R. Rani, B. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Reposeur, T. Sánchez-Conde, M. Parkinson, P.M. Saz Scotton, L. Serini, D. Sgrò, C. Siskind, E.J. Spandre, G. Spinelli, P. Sueoka, K. Suson, D.J. Tajima, H. Tak, D. Thayer, J.B. Torres, D.F. Troja, E. Valverde, J. Wadiasingh, Z. Wood, K. Zaharijas, G. IRAP Université de Toulouse CNRS UPS CNES ToulouseF-31028 France Université Paris Saclay Université Paris Cité CEA CNRS AIM Gif-sur-Yvette F-91191 France Deutsches Elektronen Synchrotron DESY ZeuthenD-15738 Germany Università di Pisa Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Trieste TriesteI-34127 Italy Dipartimento di Fisica Università di Trieste TriesteI-34127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Padova PadovaI-35131 Italy Dipartimento di Fisica e Astronomia "G. Galilei" Università di Padova PadovaI-35131 Italy Center for Space Studies and Activities "G. Colombo" University of Padova Via Venezia 15 PadovaI-35131 Italy Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy California State University Los Angeles Department of Physics and Astronomy Los AngelesCA90032 United States Dipartimento di Fisica Università degli Studi di Perugia PerugiaI-06123 Italy Dipartimento di Fisica "M. Merlin" Università e del Politecnico di Bari via Amendola 173 BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States Istituto Nazionale di Fisica Nucleare Sezione di Torino TorinoI-10125 Italy Dipartimento di Fisica Università degli Studi di Torino TorinoI-10125 Italy Laboratoire Leprince-Ringuet École Polytechnique CNRS IN2P3 PalaiseauF-91128 France Institut für Theoretische Physik and Astrophysik Universität Würzburg WürzburgD-97074 Germany NASA Goddard Space Flight Center GreenbeltMD20771 United States INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Milano via E. Bassini 15 MilanoI-20133 Italy Harvard-Smithsonian Center for Astrophysics CambridgeMA02138 United States Is

Cosmic rays are mostly composed of protons accelerated to relativistic speeds. When those protons encounter interstellar material, they produce neutral pions which in turn decay into gamma rays. This offers a compelling way to identify the acceleration sites of protons. A characteristic hadronic spectrum, with a low-energy break around 200 MeV, was detected in the gamma-ray spectra of four Supernova Remnants (SNRs), IC 443, W44, W49B and W51C, with the Fermi Large Area Telescope. This detection provided direct evidence that cosmic-ray protons are (re-)accelerated in SNRs. Here, we present a comprehensive search for low-energy spectral breaks among 311 4FGL catalog sources located within 5◦ from the Galactic plane. Using 8 years of data from the Fermi Large Area Telescope between 50 MeV and 1 GeV, we find and present the spectral characteristics of 56 sources with a spectral break confirmed by a thorough study of systematic uncertainty. Our population of sources includes 13 SNRs for which the proton-proton interaction is enhanced by the dense target material;the high-mass γ-ray binary LS I +61 303;the colliding wind binary η Carinae;and the Cygnus star-forming region. This analysis better constrains the origin of the γ-ray emission and enlarges our view to potential new cosmic-ray acceleration sites. Copyright © 2022, The Authors. All rights reserved.

关键词： Cosmic rays

来源：评论

学校读者我要写书评

暂无评论

THE PROPERTIES OF GRB 120923A AT A SPECTROSCOPIC REDSHIFT OF z ≈ 7.8

arXiv

引用

arXiv 2017年

作者： Tanvir, N.R. Laskar, T. Levan, A.J. Perley, D.A. Zabl, J. Fynbo, J.P.U. Rhoads, J. Cenko, S.B. Greiner, J. Wiersema, K. Hjorth, J. Cucchiara, A. Berger, E. Bremer, M.N. Cano, Z. Cobb, B.E. Covino, S. D’Elia, V. Fong, W. Fruchter, A.S. Goldoni, P. Hammer, F. Heintz, K.E. Jakobsson, P. Kann, D.A. Kaper, L. Klose, S. Knust, F. Krühler, T. Malesani, D. Misra, K. Nicuesa Guelbenzu, A. Pugliese, G. Sánchez-Ramírez, R. Schulze, S. Stanway, E.R. de Ugarte Postigo, A. Watson, D. Wijers, R.A.M.J. Xu, D. Department of Physics and Astronomy University of Leicester University Road LeicesterLE1 7RH United Kingdom National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States Department of Astronomy University of California 501 Campbell Hall BerkeleyCA94720-3411 United States Department of Physics University of Warwick CoventryCV4 7AL United Kingdom Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Dark Cosmology Centre Niels Bohr Institute Copenhagen University Juliane Maries Vej 30 Copenhagen Ø2100 Denmark School of Earth and Space Exploration Arizona State University TempeAZ85287 United States Astrophysics Science Division NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States Joint Space-Science Institute University of Maryland College ParkMD20742 United States Max-Planck-Institut für Extraterrestrische Physik Giessenbachstrasse GarchingD-85748 Germany Excellence Cluster Universe Technische Universität München Boltzmannstrasse 2 GarchingD-85748 Germany University of the Virgin Islands #2 John Brewers Bay St ThomasVI00802 United States Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States H.H. Wills Physics Laboratory University of Bristol Tyndall Avenue BristolBS8 1TL United Kingdom Glorieta de la Astronomía s/n GranadaE-18008 Spain Department of Physics The George Washington University WashingtonDC20052 United States I-23807 Italy INAF-Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio CatoneI-00040 Italy ASI-Science Data Centre Via del Politecnico snc RomeI-00133 Italy Steward Observatory University of Arizona 933 N. Cherry Avenue TucsonAZ85721 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States APC Astroparticule et Cosmologie Universite Paris Diderot CNRS/IN2P3

Gamma-ray bursts (GRBs) are powerful probes of early stars and galaxies, during and potentially even before the era of reionization. Although the number of GRBs identified at z & 6 remains small, they provide a unique window on typical star-forming galaxies at that time, and thus are complementary to deep field observations. We report the identification of the optical drop-out afterglow of Swift GRB 120923A in near-infrared Gemini-North imaging, and derive a redshift of z = 7.84+0−0..0612 from VLT/X-shooter spectroscopy. At this redshift the peak 15-150 keV luminosity of the burst was 3.2 × 1052 erg s−1, and in fact the burst was close to the Swift/BAT detection threshold. The X-ray and near-infrared afterglow were also faint, and in this sense it was a rather typical long-duration GRB in terms of rest-frame luminosity. We present ground- and space-based follow-up observations spanning from X-ray to radio, and find that a standard external shock model with a constant-density circumburst environment with density, n ≈ 4×10−2 cm−3 gives a good fit to the data. The near-infrared light curve exhibits a sharp break at t ≈ 3.4 days in the observer frame, which if interpreted as being due to a jet corresponds to an opening angle of θjet ≈ 5 degrees. The beaming corrected γ-ray energy is then Eγ ≈ 2 × 1050 erg, while the beaming-corrected kinetic energy is lower, EK ≈ 1049 erg, suggesting that GRB 120923A was a comparatively low kinetic energy event. We discuss the implications of this event for our understanding of the high-redshift population of GRBs and their identification. Copyright © 2017, The Authors. All rights reserved.

关键词： Stars

来源：评论

学校读者我要写书评

暂无评论

Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b

arXiv

引用

arXiv 2024年

作者： Carleo, Ilaria Barragan, Oscar Persson, Carina M. Fridlund, Malcolm Lam, Kristine W.F. Messina, Sergio Gandolfi, Davide Smith, Alexis M.S. Johnson, Marshall C. Cochran, William Osborne, Hannah L.M. Brahm, Rafael Ciardi, David R. Collins, Karen A. Everett, Mark E. Giacalone, Steven Guenther, Eike W. Hatzes, Artie Hellier, Coel Horner, Jonathan Kabath, Petr Korth, Judith MacQueen, Phillip Masseron, Thomas Murgas, Felipe Nowak, Grzegorz Rodriguez, Joseph E. Watkins, Cristilyn N. Wittenmyer, Rob Zhou, George Ziegler, Carl Bieryla, Allyson Boyd, Patricia T. Clark, Catherine A. Dressing, Courtney D. Eastman, Jason D. Eberhardt, Jan Endl, Michael Espinoza, Nestor Fausnaugh, Michael Guerrero, Natalia M. Henning, Thomas Hesse, Katharine Hobson, Melissa J. Howell, Steve B. Jordan, Andres Latham, David W. Lund, Michael B. Mireles, Ismael Narita, Norio Pinto, Marcelo Tala Pugh, Teznie Quinn, Samuel N. Ricker, George Rodriguez, David R. Rojas, Felipe I. Rose, Mark E. Rudat, Alexander Sarkis, Paula Savel, Arjun B. Schlecker, Martin Schwarz, Richard P. Seager, Sara Shporer, Avi Smith, Jeffrey C. Stassun, Keivan G. Stockdale, Chris Trifonov, Trifon Vanderspek, Roland Winn, Joshua N. Wright, Duncan INAF-Osservatorio Astrofisico di Torino Via Osservatorio 20 Pino TorineseI-10025 Italy Tenerife La Laguna38205 Spain Tenerife La LagunaE-38206 Spain Sub-department of Astrophysics Department of Physics University of Oxford OxfordOX1 3RH United Kingdom Chalmers University of Technology Department of Space Earth and Environment Onsala Space Observatory OnsalaSE-439 92 Sweden Leiden Observatory University of Leiden PO Box 9513 Leiden2300 RA Netherlands Rutherfordstrasse 2 Berlin12489 Germany INAF - Osservatorio Astrofisico di Catania Via S. Sofia 78 CataniaI-95123 Italy Dipartimento di Fisica Universita degli Studi di Torino via Pietro Giuria 1 TorinoI-10125 Italy Department of Astronomy The Ohio State University 4055 McPherson Laboratory 140 West 18th Avenue ColumbusOH43210 United States Mullard Space Science Laboratory University College London Holmbury St Mary Dorking SurreyRH5 6NT United Kingdom European Southern Observatory Karl-Schwarzschild-Strase 2 Garching bei MunchenD-85748 Germany Facultad de Ingeniera y Ciencias Universidad Adolfo Ibanez Av. Diagonallas Torres 2640 Penalolen Santiago Chile Millennium Institute for Astrophysics Chile NASA Exoplanet Science Institute-Caltech IPAC PasadenaCA91125 United States Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Department of Astronomy and McDonald Observatory University of Texas at Austin 2515 Speedway Stop C1400 AustinTX78712 United States NSF National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. TucsonAZ85719 United States Department of Astronomy California Institute of Technology PasadenaCA91125 United States Thuringer Landessternwarte Tautenburg Sternwarte 5 TautenburgD-07778 Germany Astrophysics Group Keele University StaffordshireST5 5BG United Kingdom Astronomical Institute Czech Academy of Sciences Fričova 298 Ondřejov25165 Czech Republic Lund Observatory Division of Astrophysics

Context. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters, challenging our understanding on their actual origin. Aims. The present work, which is the results of our warm Jupiters survey carried out with the CHIRON spectrograph within the KESPRINT collaboration, aims to address this challenge by studying two planets that could help bridge the gap between the two populations. *** report the confirmation and mass determination of a hot Jupiter (orbital period shorter than 10 days), TOI-2420 b, and a warm Jupiter, TOI-2485 b. We performed a joint analysis using a wide variety of spectral and photometric data in order to characterize these planetary systems. Results. We found that TOI-2420 b has an orbital period of Pb=5.8 days, a mass of Mb=0.9 MJ and a radius of Rb=1.3 RJ, with a planetary density of 0.477 g cm-3;while TOI-2485 b has an orbital period of Pb=11.2 days, a mass of Mb=2.4 MJ and a radius of Rb=1.1 RJ with density 2.36 g cm-3. Conclusions. With current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: the high-eccentricity migration scenarios cannot be ruled out, and TOI-2485 b's characteristics may rather support this scenario. Copyright © 2024, The Authors. All rights reserved.

关键词： Planets

来源：评论

学校读者我要写书评

暂无评论

Fostering innovation and advancement in evidence-based practice and guidelines within the field of pediatrics: The 2024 BRIGHT declaration

Pediatric Discovery

引用

Pediatric Discovery 2024年第4期2卷

作者： Xu Wang Hui Liu Janne Estill Fujian Song Akihiko Ozaki Juan V. A. Franco Ivan D. Florez Etienne Ngeh Nav Persaud Liliya Eugenevna Ziganshina Myeong Soo Lee Lu Zhang Yuan Chi Yuting Duan Enmei Liu Yaolong Chen Xiaodong Zhao National Clinical Research Center for Child Health and Disorders Ministry of Education Key Laboratory of Child Development and Disorders Chongqing Key Laboratory of Child Infection and Immunity China International Science and Technology Cooperation base of Child Development and Critical Disorders Chongqing China Chevidence Lab Child & Adolescent Health Department of Pediatric Research Institute Children's Hospital of Chongqing Medical University Chongqing China Evidence-based Medicine Center School of Basic Medical Sciences Lanzhou University Lanzhou Gansu China Institute of Global Health University of Geneva Geneva Switzerland Norwich Medical School University of East Anglia Norwich UK Breast and Thyroid Center Jyoban Hospital of Tokiwa Foundation Fukushima Japan Institute of General Practice Medical Faculty Heinrich-Heine-Universitat Dusseldorf Dusseldorf Nordrhein-Westfalen Germany Department of Pediatrics University of Antioquia Medellin Colombia School of Rehabilitation Science McMaster University Hamilton Ontario Canada Pediatric Intensive Care Unit Clinica Las Americas-AUNA Medellin Colombia School of Health and Well Being Sheffield Hallam University Sheffield UK Research Organisation for Health Education and Rehabilitation-Cameroon (ROHER-CAM) Bamenda Cameroon Department of Family Medicine University of Toronto Faculty of Medicine Toronto Ontario Canada Russian Medical Academy for Continuing Professional Education (RMANPO) Moscow Russian Federation The Peoples' Friendship University of Russia named after Patrice Lumumba (RUDN University) Moscow Russian Federation The Kazan State Medical University Kazan Russian Federation KM Science Research Division Korea Institute of Oriental Medicine Daejeon Republic of Korea Department of Computer Science Hong Kong Baptist University Hong Kong China Institute of Systems Medicine and Health Sciences Hong Kong Baptist University Hong Kong China Yealth Network Beijing Health Technology Co. Ltd Beijing Chin

The first Better evidence and RecommendatIons for the next Generation HealTh—BRIGHT symposium was held in Chongqing, China between June 21 and 23, 2024. The symposium did not only showcase the recent progress made by multidisciplinary teams in generating and translating evidence for children's healthcare, guideline development and evaluation, and the utilization of AI applications in pediatrics but also fostered transnational and transregional cooperation to promote the advancement of high-quality evidence and guidelines in this field. The symposium contributed significantly to the future development and transformation of research endeavors in pediatrics.

关键词： declaration evidence-based medicine guidelines pediartic

来源：评论

学校读者我要写书评

暂无评论

The Fermi-LAT Light Curve Repository

arXiv

引用

arXiv 2023年

作者： Abdollahi, S. Ajello, M. Baldini, L. Ballet, J. Bastieri, D. Gonzalez, J. Becerra Bellazzini, R. Berretta, A. Bissaldi, E. Bonino, R. Brill, A. Bruel, P. Burns, E. Buson, S. Cameron, R.A. Caputo, R. Caraveo, P.A. Cibrario, N. Ciprini, S. Orestano, P. Cristarella Crnogorcevic, M. Cutini, S. D’Ammando, F. De Gaetano, S. Digel, S.W. Di Lalla, N. Di Venere, L. Domínguez, A. Ramazani, V. Fallah Fegan, S.J. Ferrara, E.C. Fiori, A. Fleischhack, H. Franckowiak, A. Fukazawa, Y. Fusco, P. Gammaldi, V. Gargano, F. Garrappa, S. Gasbarra, C. Gasparrini, D. Giglietto, N. Giordano, F. Giroletti, M. Green, D. Grenier, I.A. Guiriec, S. Gustafsson, M. Hays, E. Horan, D. Hou, X. Jóhannesson, G. Kerr, M. Kocevski, D. Kuss, M. Latronico, L. Li, J. Liodakis, I. Longo, F. Loparco, F. Lorusso, L. Lott, B. Lovellette, M.N. Lubrano, P. Maldera, S. Manfreda, A. Martí-Devesa, G. Mazziotta, M.N. Mereu, I. Meyer, M. Michelson, P.F. Mizuno, T. Monzani, M.E. Morselli, A. Moskalenko, I.V. Negro, M. Omodei, N. Orlando, E. Ormes, J.F. Paneque, D. Panzarini, G. Perkins, J.S. Persic, M. Pesce-Rollins, M. Pillera, R. Porter, T.A. Principe, G. Racusin, J.L. Rainò, S. Rando, R. Rani, B. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Sánchez-Conde, M. Parkinson, P.M. Saz Scargle, Jeff Scotton, L. Serini, D. Sgrò, C. Siskind, E.J. Spandre, G. Spinelli, P. Suson, D.J. Tajima, H. Thompson, D.J. Torres, D.F. Valverde, J. Venters, T. Wadiasingh, Z. Wagner, S. Wood, K. IRAP Université de Toulouse CNRS UPS CNES ToulouseF-31028 France Department of Physics and Astronomy Clemson University Kinard Lab of Physics ClemsonSC29634-0978 United States Università di Pisa Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Université Paris-Saclay Université Paris Cité CEA CNRS AIM Gif-sur-YvetteF-91191 Cedex France Istituto Nazionale di Fisica Nucleare Sezione di Padova PadovaI-35131 Italy Dipartimento di Fisica e Astronomia "G. Galilei" Università di Padova Via F. Marzolo 8 PadovaI-35131 Italy Center for Space Studies and Activities "G. Colombo" University of Padova Via Venezia 15 PadovaI-35131 Italy Instituto de Astrofísica de Canarias Observatorio del Teide C/Via Lactea s/n Tenerife La LagunaE-38205 Spain Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Dipartimento di Fisica Università degli Studi di Perugia PerugiaI-06123 Italy Dipartimento di Fisica "M. Merlin" dell’Università e del Politecnico di Bari via Amendola 173 BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Torino TorinoI-10125 Italy Dipartimento di Fisica Università degli Studi di Torino TorinoI-10125 Italy NASA Postdoctoral Program Fellow United States NASA Goddard Space Flight Center GreenbeltMD20771 United States Laboratoire Leprince-Ringuet CNRS IN2P3 École polytechnique Institut Polytechnique de Paris Palaiseau91120 France Department of physics and Astronomy Louisiana State University Baton RougeLA70803 United States Institut für Theoretische Physik and Astrophysik Universität Würzburg WürzburgD-97074 Germany W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Milano via E. Bassi

The Fermi Large Area Telescope (LAT) light curve repository (LCR) is a publicly available, continually updated library of gamma-ray light curves of variable Fermi-LAT sources generated over multiple timescales. The Fermi-LAT LCR aims to provide publication-quality light curves binned on timescales of 3 days, 7 days, and 30 days for 1525 sources deemed variable in the source catalog of the first 10 years of Fermi-LAT observations. The repository consists of light curves generated through full likelihood analyses that model the sources and the surrounding region, providing fluxes and photon indices for each time bin. The LCR is intended as a resource for the time-domain and multi-messenger communities by allowing users to quickly search LAT data to identify correlated variability and flaring emission episodes from gamma-ray sources. We describe the sample selection and analysis employed by the LCR and provide an overview of the associated data access portal. Copyright © 2023, The Authors. All rights reserved.

关键词： Gamma rays

来源：评论

学校读者我要写书评

暂无评论

The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope - data Release 3

arXiv

引用

arXiv 2022年

作者： Ajello, Marco Baldini, Luca Ballet, Jean Bastieri, Denis Gonzalez, Joseff Becerra Bellazzini, Ronaldo Berretta, Alessandra Bissaldi, Elisabetta Bonino, Raffaella Brill, Ari Bruel, Philippe Buson, Sara Caputo, Regina Caraveo, Patrizia A. Cheung, C.C. Chiaro, Graziano Cibrario, Nicolo Ciprini, Stefano Crnogorcevic, Milena Cutini, Sara D’Ammando, Filippo De Gaetano, Salvatore Di Lalla, Niccolo Di Venere, Leonardo Domínguez, Alberto Ramazani, Vandad Fallah Ferrara, Elizabeth C. Fiori, Alessio Fukazawa, Yasushi Funk, Stefan Fusco, Piergiorgio Gammaldi, Viviana Gargano, Fabio Garrappa, Simone Gasparrini, Dario Giglietto, Nico Giordano, Francesco Giroletti, Marcello Green, David Grenier, Isabelle A. Guiriec, Sylvain Horan, Deirdre Hou, Xian Kayanoki, Taishu Kuss, Michael Larsson, Stefan Latronico, Luca Lewis, Tiffany Li, Jian Liodakis, Ioannis Longo, Francesco Loparco, Francesco Lott, Benoit Lovellette, Michael N. Lubrano, Pasquale Madejski, Grzegorz M. Maldera, Simone Manfreda, Alberto Martí-Devesa, Guillem Mazziotta, Mario Nicola Mereu, Isabella Michelson, Peter F. Mirabal, Nestor Mitthumsiri, Warit Mizuno, Tsunefumi Monzani, Maria Elena Morselli, Aldo Moskalenko, Igor V. Negro, Michela Ojha, Roopesh Orienti, Monica Orlando, Elena Ormes, Jonathan F. Pei, Zhiyuan Peña-Herazo, Harold A. Persic, Massimo Pesce-Rollins, Melissa Petrosian, Vahe Pillera, Roberta Poon, Helen Porter, Troy A. Principe, Giacomo Rainò, Silvia Rando, Riccardo Rani, Bindu Razzano, Massimiliano Razzaque, Soebur Reimer, Anita Reimer, Olaf Scotton, Lorenzo Serini, Davide Sgrò, Carmelo Siskind, Eric J. Spandre, Gloria Spinelli, Paolo Suson, Dan J. Tajima, Hiro Torres, Diego F. Valverde, Janeth Yassin, Hend Zaharijas, Gabrijela Department of Physics and Astronomy Clemson University Kinard Lab of Physics ClemsonSC29634-0978 United States Università di Pisa Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy AIM CEA CNRS Université Paris-Saclay Université de Paris Gif-sur-YvetteF-91191 France Istituto Nazionale di Fisica Nucleare Sezione di Padova PadovaI-35131 Italy Dipartimento di Fisica e Astronomia "G. Galilei" Università di Padova Via F. Marzolo 8 PadovaI-35131 Italy Center for Space Studies and Activities "G. Colombo" University of Padova Via Venezia 15 PadovaI-35131 Italy Instituto de Astrofísica de Canarias Observatorio del Teide C/Via Lactea s/n La Laguna TenerifeE-38205 Spain Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Dipartimento di Fisica Università degli Studi di Perugia PerugiaI-06123 Italy Dipartimento di Fisica "M. Merlin" Università e del Politecnico di Bari via Amendola 173 BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Torino TorinoI-10125 Italy Dipartimento di Fisica Università degli Studi di Torino TorinoI-10125 Italy NASA Postdoctoral Program United States NASA Goddard Space Flight Center GreenbeltMD20771 United States Laboratoire Leprince-Ringuet École polytechnique CNRS IN2P3 PalaiseauF-91128 France Institut für Theoretische Physik and Astrophysik Universität Würzburg WürzburgD-97074 Germany INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Milano via E. Bassini 15 MilanoI-20133 Italy Space Science Division Naval Research Laboratory WashingtonDC20375-5352 United States Istituto Nazionale di Fisica Nucleare Sezione di Roma "Tor Vergata" RomaI-00133 Italy Space Science Data Center - Agenzia Spaziale Italiana Via del Politecnico snc RomaI-00133 Italy Department of Astronomy University of Maryland College ParkMD20742 United States Istituto Nazionale di Fisica Nucleare Sezio

An incremental version of the fourth catalog of active galactic nuclei (AGNs) detected by the Fermi-Large Area Telescope is presented. This version (4LAC-DR3) derives from the third data release of the 4FGL catalog based on 12 years of E>50 MeV gamma-ray data, where the spectral parameters, spectral energy distributions (SEDs), yearly light curves, and associations have been updated for all sources. The new reported AGNs include 587 blazar candidates and four radio galaxies. We describe the properties of the new sample and outline changes affecting the previously published one. We also introduce two new parameters in this release, namely the peak energy of the SED high-energy component and the corresponding flux. These parameters allow an assessment of the Compton dominance, the ratio of the Inverse-Compton to the synchrotron peak luminosities, without relying on X-ray data. © 2022, CC BY.

关键词： Active Galactic Nuclei

来源：评论

学校读者我要写书评

暂无评论

Publisher Correction: A global overview of marine heatwaves in a changing climate

Communications Earth & Environment

引用

Communications Earth & Environment 2024年第1期5卷 1页

作者： Antonietta Capotondi Tongtong Xu Dillon J. Amaya Regina R. Rodrigues Alex Sen Gupta Jessica A. Benthuysen Clara Deser Thomas L. Frölicher Natacha Le Grix Nicole S. Lovenduski Juliet Hermes Neil J. Holbrook Cristian Martinez-Villalobos Simona Masina Mathew Koll Roxy Amandine Schaeffer Robert W. Schlegel Kathryn E. Smith Chunzai Wang Cooperative Institute for Research in Environmental Sciences University of Colorado Boulder Boulder CO USA NOAA/Physical Sciences Laboratory Boulder CO USA Federal University of Santa Catarina Florianópolis Brazil Climate ChangeResearch Centre and CentreforMarine Science and Innovation University of New South Wales Sydney NSW Australia Australian Research Council Centre of Excellence for Climate Extremes University of New South Wales Sydney NSW Australia Australian Institute of Marine Science Crawley WA Australia Climate and Global Dynamics Laboratory National Center for Atmospheric Research Boulder CO USA Climate and Environmental Physics Physics Institute University of Bern Bern Switzerland Oeschger Centre for Climate Change Research University of Bern Bern Switzerland Department of Atmospheric and Oceanic Sciences and Institute of Arctic and Alpine Research University of Colorado Boulder Boulder CO USA South African Environmental Observation Network Cape Town South Africa Institute for Marine and Antarctic Studies University of Tasmania Hobart TAS Australia ARC Centre of Excellence for Climate Extremes University of Tasmania Hobart TAS Australia Faculty of Engineering and Science Universidad Adolfo Ibáñez Santiago Chile Data Observatory Foundation ANID Technology Center No. DO210001 Santiago Chile CMCC Foundation—Euro-Mediterranean Center on Climate Change Bologna Italy Centre for Climate Change Research Indian Institute of Tropical Meteorology Ministry of Earth Sciences Pune India School of Mathematics and Statistics UNSW Sydney NSW Australia Center for Marine Science and Innovation UNSW Sydney NSW Australia Laboratoire d’Océanographie de Villefranche Sorbonne University CNRS Villefranche-sur-mer France Marine Biological Association of the United Kingdom Plymouth UK State Key Laboratory of Tropical Oceanography South China Sea Institute of Oceanology Chinese Academy of Sciences Guangzhou China Global Ocean and Climate Research Center

来源：评论

学校读者我要写书评

暂无评论

SEARCH FOR EXTENDED GEV SOURCES IN THE INNER GALACTIC PLANE

arXiv

引用

arXiv 2024年

作者： Abdollahi, S. Acero, F. Acharyya, A. Adelfio, A. Ajello, M. Baldini, L. Ballet, J. Bartolini, C. Gonzalez, J. Becerra Bellazzini, R. Bissaldi, E. Bonino, R. Bruel, P. Cameron, R.A. Caraveo, P.A. castro, D. Cavazzuti, E. Cheung, C.C. Cibrario, N. Ciprini, S. Cozzolongo, G. Orestano, P. Cristarella Cuoco, A. Cutini, S. D’Ammando, F. Di Lalla, N. Dinesh, A. Di Venere, L. Domínguez, A. Fiori, A. Funk, S. Fusco, P. Gargano, F. Gasbarra, C. Gasparrini, D. Germani, S. Giacchino, F. Giglietto, N. Giliberti, M. Giordano, F. Giroletti, M. Green, D. Grenier, I.A. Guillemot, L. Guiriec, S. Gupta, R. Hashizume, M. Hays, E. Hewitt, J.W. Horan, D. Hou, X. Kayanoki, T. Kuss, M. Laviron, A. Lemoine-Goumard, M. Liguori, A. Li, J. Liodakis, I. Loizzo, P. Longo, F. Loparco, F. Lorusso, L. Lovellette, M.N. Lubrano, P. Maldera, S. Malyshev, D. Martí-Devesa, G. Martin, P. Mazziotta, M.N. Mereu, I. Michelson, P.F. Mirabal, N. Mitthumsiri, W. Mizuno, T. Monti-Guarnieri, P. Monzani, M.E. Morselli, A. Moskalenko, I.V. Negro, M. Omodei, N. Orienti, M. Orlando, E. Paneque, D. Panzarini, G. Persic, M. Pesce-Rollins, M. Pillera, R. Porter, T.A. Rainò, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Bernal, M. Rocamora Sánchez-Conde, M. Parkinson, P.M. Saz Serini, D. Sgrò, C. Siskind, E.J. Smith, D.A. Spandre, G. Spinelli, P. Strong, A.W. Suson, D.J. Tajima, H. Thayer, J.B. Torres, D.F. Valverde, J. Wadiasingh, Z. Wood, K. Zaharijas, G. IRAP Université de Toulouse CNRS UPS CNES ToulouseF-31028 France AIM CEA CNRS Université Paris-Saclay Université de Paris Gif-sur-YvetteF-91191 France Center for Cosmology and Particle Physics Phenomenology University of Southern Denmark Campusvej 55 Odense MDK-5230 Denmark Istituto Nazionale di Fisica Nucleare Sezione di Perugia PerugiaI-06123 Italy Department of Physics and Astronomy Clemson University Kinard Lab of Physics ClemsonSC29634-0978 United States Università di Pisa Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Université Paris-Saclay Université Paris Cité CEA CNRS AIM Gif-sur-YvetteF-91191 Cedex France Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy Università degli studi di Trento via Calepina 14 Trento38122 Italy Instituto de Astrofísica de Canarias Universidad de La Laguna Dpto. Astrofísica Tenerife La Laguna38200 Spain Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Dipartimento di Fisica "M. Merlin" dell’Università e del Politecnico di Bari via Amendola 173 BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Torino TorinoI-10125 Italy Dipartimento di Fisica Università degli Studi di Torino TorinoI-10125 Italy Laboratoire Leprince-Ringuet CNRS IN2P3 École polytechnique Institut Polytechnique de Paris Palaiseau91120 France W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Milano via E. Bassini 15 MilanoI-20133 Italy Harvard-Smithsonian Center for Astrophysics CambridgeMA02138 United States Astrophysics Science Division NASA Goddard Space Flight Center GreenbeltMD20771 United States Italian Space Agency Via del Politecnico snc Roma00133 Italy Space Science Division Naval Research Laboratory Washin

The recent detection of extended γ-ray emission around middle-aged pulsars is interpreted as inverse-Compton scattering of ambient photons by electron-positron pairs escaping the pulsar wind nebula, which are confined near the system by unclear mechanisms. This emerging population of γ-ray sources was first discovered at TeV energies and remains underexplored in the GeV range. To address this, we conducted a systematic search for extended sources along the Galactic plane using 14 years of Fermi-LAT data above 10 GeV, aiming to identify a number of pulsar halo candidates and extend our view to lower energies. The search covered the inner Galactic plane (|l| ≤ 100◦, |b| ≤ 1◦) and the positions of known TeV sources and bright pulsars, yielding broader astrophysical interest. We found 40 such sources, forming the Second Fermi Galactic Extended Sources Catalog (2FGES), most with 68% containment radii smaller than 1.0◦ and relatively hard spectra with photon indices below 2.5. We assessed detection robustness using field-specific alternative interstellar emission models and by inspecting significance maps. Noting 13 sources previously known as extended in the 4FGL-DR3 catalog and five dubious sources from complex regions, we report 22 newly detected extended sources above 10 GeV. Of these, 13 coincide with H.E.S.S., HAWC, or LHAASO sources;six coincide with bright pulsars (including four also coincident with TeV sources);six are associated with 4FGL point sources only;and one has no association in the scanned catalogs. Notably, six to eight sources may be related to pulsars as classical pulsar wind nebulae or pulsar halos. © 2024, CC BY.

关键词： Gamma rays

来源：评论

学校读者我要写书评

暂无评论

The X-shooter GRB afterglow legacy sample (XS-GRB)?

arXiv

引用

arXiv 2018年

作者： Selsing, J. Malesani, D. Goldoni, P. Fynbo, J.P.U. Krühler, T. Antonelli, L.A. Arabsalmani, M. Bolmer, J. Cano, Z. Christensen, L. Covino, S. D’Avanzo, P. D’Elia, V. de Cia, A. de Ugarte, A. Postigo Flores, H. Friis, M. Gomboc, A. Greiner, J. Groot, P. Hammer, F. Hartoog, O.E. Heintz, K.E. Hjorth, J. Jakobsson, P. Japelj, J. Kann, D.A. Kaper, L. Ledoux, C. Leloudas, G. Levan, A.J. Maiorano, E. Melandri, A. Milvang-Jensen, B. Palazzi, E. Palmerio, J.T. Perley, D.A. Pian, E. Piranomonte, S. Pugliese, G. Sánchez-Ramírez, R. Savaglio, S. Schady, P. Schulze, S. Sollerman, J. Sparre, M. Tagliaferri, G. Tanvir, N.R. Thöne, C.C. Vergani, S.D. Vreeswijk, P. Watson, D. Wiersema, K. Wijers, R. Xu, D. Zafar, T. Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Juliane Maries Vej 30 København Ø2100 Denmark Cosmic Dawn Center Niels Bohr Institute University of Copenhagen Juliane Maries Vej 30 København Ø2100 Denmark DTU Space National Space Institute Technical University of Denmark Elektrovej 327 Lyngby2800 Denmark APC Astroparticule et Cosmologie Université Paris Diderot CNRS/IN2P3 CEA/Irfu Observatoire de Paris Sorbonne Paris Cité 10 Rue Alice Domon et Léonie Duquet Paris Cedex 1375205 France Max-Planck-Institut für extraterrestrische Physik Giessenbachstraße Garching85748 Germany 00078 Italy IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France Université Paris Diderot AIM Sorbonne Paris Cité CEA CNRS Gif-sur-YvetteF-91191 France European Southern Observatory Alonso de Córdova 3107 Vitacura Casilla Santiago 1919001 Chile Glorieta de la Astronomía s/n GranadaE-18008 Spain 23807 Italy Space Science Data Center - Agenzia Spaziale Italiana via del Politecnico s.n.c. RomaI-00133 Italy European Southern Observatory Karl-Schwarzschild Str. 2 Garching bei München85748 Germany GEPI Observatoire de Paris PSL University CNRS 5 place Jules Janssen 92195 Meudon France KTH Royal Institute of Technology Department of Physics Stockholm106 91 Sweden The Oskar Klein Centre for Cosmoparticle Physics AlbaNova University Centre Stockholm106 91 Sweden Center for Astrophysics and Cosmology University of Nova Gorica Vipavska 11c Ajdovščina5270 Slovenia Department of Astrophysics IMAPP Radboud University Nijmegen PO Box 9010 Nijmegen6500 GL Netherlands Anton Pannekoek Institute for Astronomy University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands Centre for Astrophysics and Cosmology Science Institute University of Iceland Dunhagi 5 Reykjavik107 Iceland Department of Physics University of Warwick CoventryCV4 7AL United Kingdom IASF/INAF Bologna via Piero Gobetti 101 Bologna40129 Italy Sorbonne

In this work we present spectra of all γ-ray burst (GRB) afterglows that have been promptly observed with the X-shooter spectrograph until 31/03/2017. In total, we obtained spectroscopic observations of 103 individual GRBs observed within 48 hours of the GRB trigger. Redshifts have been measured for 97 per cent of these, covering a redshift range from 0.059 to 7.84. Based on a set of observational selection criteria that minimize biases with regards to intrinsic properties of the GRBs, the follow-up effort has been focused on producing a homogeneous sample of 93 afterglow spectra for GRBs discovered by the Swift satellite. We here provide a public release of all the reduced spectra, including continuum estimates and telluric absorption corrections. For completeness, we also provide reductions for the 18 late-time observations of the underlying host galaxies. We provide an assessment of the degree of completeness with respect to the parent GRB population, in terms of the X-ray properties of the bursts in the sample and find that the sample presented here is representative of the full Swift sample. We constrain the fraction of dark bursts to be Copyright © 2018, The Authors. All rights reserved.

关键词： X ray absorption

来源：评论

学校读者我要写书评

暂无评论

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案：

请选择收藏分类：

通借通还

建议与咨询 留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案： 新增检索档案 确定 取消

请选择收藏分类： 新增自定义分类 确定 取消

通借通还

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

请选择保存的检索档案：

请选择收藏分类：