检索结果-内蒙古大学图书馆

measurement of the Lifetime and Λ separation Energy of HΛ3

Physical Review Letters 2023年第10期131卷 102302-102302页

作者： s. Acharya D. Adamová A. Adler G. Aglieri Rinella m. Agnello N. Agrawal Z. Ahammed s. Ahmad s. U. Ahn I. Ahuja A. Akindinov m. Al-Turany D. Aleksandrov B. Alessandro H. m. Alfanda R. Alfaro molina B. Ali Y. Ali A. Alici N. Alizadehvandchali A. Alkin J. Alme G. Alocco T. Alt I. Altsybeev m. N. Anaam C. Andrei A. Andronic V. Anguelov F. Antinori P. Antonioli C. Anuj N. Apadula L. Aphecetche H. Appelshäuser C. Arata s. Arcelli m. Aresti R. Arnaldi I. C. Arsene m. Arslandok A. Augustinus R. Averbeck m. D. Azmi A. Badalà Y. W. Baek X. Bai R. Bailhache Y. Bailung R. Bala A. Balbino A. Baldisseri B. Balis D. Banerjee Z. Banoo R. Barbera F. Barile L. Barioglio m. Barlou G. G. Barnaföldi L. s. Barnby V. Barret L. Barreto C. Bartels K. Barth E. Bartsch F. Baruffaldi N. Bastid s. Basu G. Batigne D. Battistini B. Batyunya D. Bauri J. L. Bazo Alba I. G. Bearden C. Beattie P. Becht D. Behera I. Belikov A. D. C. Bell Hechavarria F. Bellini R. Bellwied s. Belokurova V. Belyaev G. Bencedi s. Beole A. Bercuci Y. Berdnikov A. Berdnikova L. Bergmann m. G. Besoiu L. Betev P. P. Bhaduri A. Bhasin m. A. Bhat B. Bhattacharjee L. Bianchi N. Bianchi J. Bielčík J. Bielčíková J. Biernat A. P. Bigot A. Bilandzic G. Biro s. Biswas N. Bize J. T. Blair D. Blau m. B. Blidaru N. Bluhme C. Blume G. Boca F. Bock T. Bodova A. Bogdanov s. Boi J. Bok L. Boldizsár A. Bolozdynya m. Bombara P. m. Bond G. Bonomi H. Borel A. Borissov A. G. Borquez Carcamo H. Bossi E. Botta Y. E. m. Bouziani L. Bratrud P. Braun-munzinger m. Bregant m. Broz G. E. Bruno m. D. Buckland D. Budnikov H. Buesching s. Bufalino O. Bugnon P. Buhler Z. Buthelezi J. B. Butt s. A. Bysiak m. Cai H. Caines A. Caliva E. Calvo Villar J. m. m. Camacho P. Camerini F. D. m. Canedo m. Carabas A. A. Carballo F. Carnesecchi R. Caron J. Castillo Castellanos F. Catalano C. Ceballos sanchez I. Chakaberia P. Chakraborty s. Chandra s. Chapeland m. Chartier s. Chattopadhyay T. G. Chavez T. Cheng C. Cheshkov B. Cheynis V. Chibante Barroso D. D. Chinellato E. s. Chizzali J. Cho s. Cho P. Chochula P. Chri Université Clermont Auvergne CNRS/IN2P3 LPC Clermont-Ferrand France Nuclear Physics Institute of the Czech Academy of Sciences Husinec-Řež Czech Republic Johann-Wolfgang-Goethe Universität Frankfurt Institut für Informatik Fachbereich Informatik und Mathematik Frankfurt Germany European Organization for Nuclear Research (CERN) Geneva Switzerland Dipartimento DISAT del Politecnico and Sezione INFN Turin Italy INFN Sezione di Bologna Bologna Italy Variable Energy Cyclotron Centre Homi Bhabha National Institute Kolkata India Department of Physics Aligarh Muslim University Aligarh India Korea Institute of Science and Technology Information Daejeon Republic of Korea Faculty of Science P.J. Šafárik University Košice Slovak Republic Affiliated with an institute covered by a cooperation agreement with CERN Research Division and ExtreMe Matter Institute EMMI GSI Helmholtzzentrum für Schwerionenforschung GmbH Darmstadt Germany INFN Sezione di Torino Turin Italy Central China Normal University Wuhan China Instituto de Física Universidad Nacional Autónoma de México Mexico City Mexico COMSATS University Islamabad Islamabad Pakistan Dipartimento di Fisica e Astronomia dell’Università and Sezione INFN Bologna Italy University of Houston Houston Texas United States Department of Physics and Technology University of Bergen Bergen Norway INFN Sezione di Cagliari Cagliari Italy Institut für Kernphysik Johann Wolfgang Goethe-Universität Frankfurt Frankfurt Germany Horia Hulubei National Institute of Physics and Nuclear Engineering Bucharest Romania Westfälische Wilhelms-Universität Münster Institut für Kernphysik Munster Germany Physikalisches Institut Ruprecht-Karls-Universität Heidelberg Heidelberg Germany INFN Sezione di Padova Padova Italy Lawrence Berkeley National Laboratory California United States SUBATECH IMT Atlantique Nantes Université CNRS-IN2P3 Nantes France Laboratoire de Physique Subatomique et de Cosmologie Université Grenoble-Alpes CNRS-IN2P3

The m.s. precise measurements to date of the HΛ3 lifetime τ and Λ separation energy BΛ are obtained using the data sample of Pb-Pb collisions at sNN=5.02 TeV collected by ALICE at the LHC. The HΛ3 is reconstructed via its charged two-body m.s.nic decay channel (HΛ3→He3+π− and the charge-conjugate process). The measured values τ=[253±11(stat)±6(syst)] ps and BΛ=[102±63(stat)±67(syst)] keV are compatible with predictions from effective field theories and confirm that the HΛ3 structure is consistent with a weakly bound system.

关键词： m.s.n & hyperon induced nuclear reactions Relativistic heavy-ion collisions Hyperons

来源：评论

学校读者我要写书评

暂无评论

studying the interaction between charm and light-flavor m.s.ns

引用

Physical Review D 2024年第3期110卷 032004-032004页

作者： s. Acharya D. Adamová G. Aglieri Rinella L. Aglietta m. Agnello N. Agrawal Z. Ahammed s. Ahmad s. U. Ahn I. Ahuja A. Akindinov V. Akishina m. Al-Turany D. Aleksandrov B. Alessandro H. m. Alfanda R. Alfaro molina B. Ali A. Alici N. Alizadehvandchali A. Alkin J. Alme G. Alocco T. Alt A. R. Altamura I. Altsybeev J. R. Alvarado m. N. Anaam C. Andrei N. Andreou A. Andronic E. Andronov V. Anguelov F. Antinori P. Antonioli N. Apadula L. Aphecetche H. Appelshäuser C. Arata s. Arcelli m. Aresti R. Arnaldi J. G. m. C. A. Arneiro I. C. Arsene m. Arslandok A. Augustinus R. Averbeck m. D. Azmi H. Baba A. Badalà J. Bae Y. W. Baek X. Bai R. Bailhache Y. Bailung R. Bala A. Balbino A. Baldisseri B. Balis D. Banerjee Z. Banoo F. Barile L. Barioglio m. Barlou B. Barman G. G. Barnaföldi L. s. Barnby E. Barreau V. Barret L. Barreto C. Bartels K. Barth E. Bartsch N. Bastid s. Basu G. Batigne D. Battistini B. Batyunya D. Bauri J. L. Bazo Alba I. G. Bearden C. Beattie P. Becht D. Behera I. Belikov A. D. C. Bell Hechavarria F. Bellini R. Bellwied s. Belokurova L. G. E. Beltran Y. A. V. Beltran G. Bencedi A. Bensaoula s. Beole Y. Berdnikov A. Berdnikova L. Bergmann m. G. Besoiu L. Betev P. P. Bhaduri A. Bhasin m. A. Bhat B. Bhattacharjee L. Bianchi N. Bianchi J. Bielčík J. Bielčíková A. P. Bigot A. Bilandzic G. Biro s. Biswas N. Bize J. T. Blair D. Blau m. B. Blidaru N. Bluhme C. Blume G. Boca F. Bock T. Bodova J. Bok L. Boldizsár m. Bombara P. m. Bond G. Bonomi H. Borel A. Borissov A. G. Borquez Carcamo H. Bossi E. Botta Y. E. m. Bouziani L. Bratrud P. Braun-munzinger m. Bregant m. Broz G. E. Bruno m. D. Buckland D. Budnikov H. Buesching s. Bufalino P. Buhler N. Burm.s.v Z. Buthelezi A. Bylinkin s. A. Bysiak J. C. Cabanillas Noris m. F. T. Cabrera m. Cai H. Caines A. Caliva E. Calvo Villar J. m. m. Camacho P. Camerini F. D. m. Canedo s. L. Cantway m. Carabas A. A. Carballo F. Carnesecchi R. Caron L. A. D. Carvalho J. Castillo Castellanos m. Castoldi F. Catalano s. Cattaruzzi C. Ceballos sanchez R. Cerri I. Chakaberia P. Chakraborty s. Ch Université Clermont Auvergne CNRS/IN2P3 LPC Clermont-Ferrand France Nuclear Physics Institute of the Czech Academy of Sciences Husinec-Řež Czech Republic Geneva Switzerland Dipartimento di Fisica dell’Università and Sezione INFN Turin Italy Dipartimento DISAT del Politecnico and Sezione INFN Turin Italy Dipartimento di Fisica e Astronomia dell’Università and Sezione INFN Bologna Italy Variable Energy Cyclotron Centre Homi Bhabha National Institute Kolkata India Department of Physics Aligarh Muslim University Aligarh India Korea Institute of Science and Technology Information Daejeon Republic of Korea Faculty of Science P.J. Šafárik University Košice Slovak Republic Affiliated with an institute covered by a cooperation agreement with CERN Frankfurt Institute for Advanced Studies Johann Wolfgang Goethe-Universität Frankfurt Frankfurt Germany Research Division and ExtreMe Matter Institute EMMI GSI Helmholtzzentrum für Schwerionenforschung GmbH Darmstadt Germany INFN Sezione di Torino Turin Italy Central China Normal University Wuhan China Instituto de Física Universidad Nacional Autónoma de México Mexico City Mexico University of Houston Houston Texas USA Sungkyunkwan University Suwon City Republic of Korea Department of Physics and Technology University of Bergen Bergen Norway INFN Sezione di Cagliari Cagliari Italy Institut für Kernphysik Johann Wolfgang Goethe-Universität Frankfurt Frankfurt Germany INFN Sezione di Bari Bari Italy Physik Department Technische Universität München Munich Germany High Energy Physics Group Universidad Autónoma de Puebla Puebla Mexico Horia Hulubei National Institute of Physics and Nuclear Engineering Bucharest Romania University of Derby Derby United Kingdom Universität Münster Institut für Kernphysik Münster Germany Physikalisches Institut Ruprecht-Karls-Universität Heidelberg Heidelberg Germany INFN Sezione di Padova Padova Italy INFN Sezione di Bologna Bologna Italy Lawrence Berkeley National Laboratory

The two-particle momentum correlation functions between charm m.s.ns (D*± and D±) and charged light-flavor m.s.ns (π± and K±) in all charge combinations are measured for the first time by the ALICE Collaboration in high-multiplicity proton–proton collisions at a center-of-m.s. energy of s=13 TeV. For DK and D*K pairs, the experimental results are in agreement with theoretical predictions of the residual strong interaction based on quantum chromodynamics calculations on the lattice and chiral effective field theory. In the case of Dπ and D*π pairs, tension between the calculations including strong interactions and the measurement is observed. For all particle pairs, the data can be adequately described by Coulomb interaction only, indicating a shallow interaction between charm and light-flavor m.s.ns. Finally, the scattering lengths governing the residual strong interaction of the Dπ and D*π systems are determined by fitting the experimental correlation functions with a model that employs a Gaussian potential. The extracted values are small and compatible with zero.

关键词： Hadron-hadron interactions strong interaction Charmed m.s.ns

来源：评论

学校读者我要写书评

暂无评论

Joint analysis of Dark Energy survey Year 3 data and CmB lensing from.s.T and Planck. I. Construction of CmB lensing maps and modeling choices

引用

Physical Review D 2023年第2期107卷 023529-023529页

作者： Y. Omori E. J. Baxter C. Chang O. Friedrich A. Alarcon O. Alves A. Amon F. Andrade-Oliveira K. Bechtol m. R. Becker G. m. Bernstein J. Blazek L. E. Bleem H. Camacho A. Campos A. Carnero Rosell m. Carrasco Kind R. Cawthon R. Chen A. Choi J. Cordero T. m. Crawford m. Crocce C. Davis J. DeRose s. Dodelson C. Doux A. Drlica-Wagner K. Eckert T. F. Eifler F. Elsner J. Elvin-Poole s. Everett X. Fang A. Ferté P. Fosalba m. Gatti G. Giannini D. Gruen R. A. Gruendl I. Harrison K. Herner H. Huang E. m. Huff D. Huterer m. Jarvis E. Krause N. Kuropatkin P.-F. Leget P. Lem.s.A. R. Liddle N. macCrann J. mcCullough J. muir J. myles A. Navarro-Alsina s. Pandey Y. Park A. Porredon J. Prat m. Raveri R. P. Rollins A. Roodman R. Rosenfeld A. J. Ross E. s. Rykoff C. sánchez J. sanchez L. F. secco I. sevilla-Noarbe E. sheldon T. shin m. A. Troxel I. Tutusaus T. N. Varga N. Weaverdyck R. H. Wechsler W. L. K. Wu B. Yanny B. Yin Y. Zhang J. Zuntz T. m. C. Abbott m. Aguena s. Allam J. Annis D. Bacon B. A. Benson E. Bertin s. Bocquet D. Brooks D. L. Burke J. E. Carlstrom J. Carretero C. L. Chang R. Chown m. Costanzi L. N. da Costa A. T. Crites m. E. s. Pereira T. de Haan J. De Vicente s. Desai H. T. Diehl m. A. Dobbs P. Doel W. Everett I. Ferrero B. Flaugher D. Friedel J. Frieman J. García-Bellido E. Gaztanaga E. m. George T. Giannantonio N. W. Halverson s. R. Hinton G. P. Holder D. L. Hollowood W. L. Holzapfel K. Honscheid J. D. Hrubes D. J. Jam.s.L. Knox K. Kuehn O. Lahav A. T. Lee m. Lima D. Luong-Van m. march J. J. mcmahon P. melchior F. menanteau s. s. meyer R. miquel L. mocanu J. J. mohr R. morgan T. Natoli s. Padin A. Palm.s. F. Paz-Chinchón A. Pieres A. A. Plazas malagón C. Pryke C. L. Reichardt A. K. Romer J. E. Ruhl E. sanchez K. K. schaffer m. schubnell s. serrano E. shirokoff m. smith Z. staniszewski A. A. stark E. suchyta G. Tarle D. Thom.s.C. To J. D. Vieira J. Weller R. Williamson Department of Astronomy and Astrophysics University of Chicago Chicago Illinois 60637 USA Kavli Institute for Cosmological Physics University of Chicago Chicago Illinois 60637 USA Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA Kavli Institute for Particle Astrophysics and Cosmology P. O. Box 2450 Stanford University Stanford California 94305 USA Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive Honolulu Hawaii 96822 USA Kavli Institute for Cosmology University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ 20921-400 Brazil Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue Madison Wisconsin 53706-1390 USA Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA Department of Physics Northeastern University Boston Massachusetts 02115 USA Laboratory of Astrophysics École Polytechnique Fédérale de Lausanne (EPFL) Observatoire de Sauverny 1290 Versoix Switzerland High-Energy Physics Division Argonne National Laboratory 9700 South Cass Avenue. Argonne Illinois 60439 USA Instituto de Física Teórica Universidade Estadual Paulista São Paulo 01140-070 Brazil Department of Physics Carnegie Mellon University Pittsburgh Pennsylvania 15312 USA Instituto de Astrofisica de Canarias E-38205 La Laguna Tenerife Spain Universidad de La Laguna Departamento Astrofísica E-38206 La Laguna Tenerife Spain Center for Astrophysical Surveys National Center for Supercomputing Applications 1205 West Clark Street Urbana Illinois 61801 USA Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green Street Urbana Illinois 61801 USA Physic

Joint analyses of cross-correlations between measurements of galaxy positions, galaxy lensing, and lensing of the cosmic microwave background (CmB) offer powerful constraints on the large-scale structure of the Universe. In a forthcoming analysis, we will present cosmological constraints from the analysis of such cross-correlations measured using Year 3 data from the Dark Energy survey (DEs), and CmB data from the south Pole Telescope (sPT) and Planck. Here we present two key ingredients of this analysis: (1) an improved CmB lensing map in the sPT-sZ survey footprint and (2) the analysis methodology that will be used to extract cosmological information from the cross-correlation measurements. Relative to previous lensing maps made from the same CmB observations, we have implemented techniques to remove contamination from the thermal sunyaev Zel’dovich effect, enabling the extraction of cosmological information from.s.aller angular scales of the cross-correlation measurements than in previous analyses with DEs Year 1 data. We describe our model for the cross-correlations between these maps and DEs data, and validate our modeling choices to demonstrate the robustness of our analysis. We then forecast the expected cosmological constraints from the galaxy survey-CmB lensing auto and cross-correlations. We find that the galaxy-CmB lensing and galaxy shear-CmB lensing correlations will on their own provide a constraint on s8=σ8Ωm/0.3 at the few percent level, providing a powerful consistency check for the DEs-only constraints. We explore scenarios where external priors on shear calibration are removed, finding that the joint analysis of CmB lensing cross-correlations can provide constraints on the shear calibration amplitude at the 5% to 10% level.

关键词： Cosmic microwave background Cosmological parameters Dark matter Evolution of the Universe Gravitational lenses Large scale structure of the Universe

来源：评论

学校读者我要写书评

暂无评论

sPT clusters with DEs and HsT weak lensing. II. Cosmological constraints from the abundance of m.s.ive halos

引用

Physical Review D 2024年第8期110卷 083510页

作者： s. Bocquet s. Grandis L. E. Bleem m. Klein J. J. mohr T. schrabback T. m. C. Abbott P. A. R. Ade m. Aguena A. Alarcon s. Allam.s. W. Allen O. Alves A. Amon A. J. Anderson J. Annis B. Ansarinejad J. E. Austermann s. Avila D. Bacon m. Bayliss J. A. Beall K. Bechtol m. R. Becker A. N. Bender B. A. Benson G. m. Bernstein s. Bhargava F. Bianchini m. Brodwin D. Brooks L. Bryant A. Campos R. E. A. Canning J. E. Carlstrom A. Carnero Rosell m. Carrasco Kind J. Carretero F. J. Castander R. Cawthon C. L. Chang C. Chang P. Chaubal R. Chen H. C. Chiang A. Choi T-L. Chou R. Citron C. Corbett moran J. Cordero m. Costanzi T. m. Crawford A. T. Crites L. N. da Costa m. E. s. Pereira C. Davis T. m. Davis J. DeRose s. Desai T. de Haan H. T. Diehl m. A. Dobbs s. Dodelson C. Doux A. Drlica-Wagner K. Eckert J. Elvin-Poole s. Everett W. Everett I. Ferrero A. Ferté A. m. Flores J. Frieman J. Gallicchio J. García-Bellido m. Gatti E. m. George G. Giannini m. D. Gladders D. Gruen R. A. Gruendl N. Gupta G. Gutierrez N. W. Halverson I. Harrison W. G. Hartley K. Herner s. R. Hinton G. P. Holder D. L. Hollowood W. L. Holzapfel K. Honscheid J. D. Hrubes N. Huang J. Hubmayr E. m. Huff D. Huterer K. D. Irwin D. J. Jam.s.m. Jarvis G. Khullar K. Kim L. Knox R. Kraft E. Krause K. Kuehn N. Kuropatkin F. Kéruzoré O. Lahav A. T. Lee P.-F. Leget D. Li H. Lin A. Lowitz N. macCrann G. mahler A. mantz J. L. marshall J. mcCullough m. mcDonald J. J. mcmahon J. mena-Fernández F. menanteau s. s. meyer R. miquel J. montgomery J. myles T. Natoli A. Navarro-Alsina J. P. Nibarger G. I. Noble V. Novosad R. L. C. Ogando Y. Omori s. Padin s. Pandey P. Paschos s. Patil A. Pieres A. A. Plazas malagón A. Porredon J. Prat C. Pryke m. Raveri C. L. Reichardt J. Roberson R. P. Rollins C. Romero A. Roodman J. E. Ruhl E. s. Rykoff B. R. saliwanchik L. salvati C. sánchez E. sanchez D. sanchez Cid A. saro K. K. schaffer L. F. secco I. sevilla-Noarbe K. sharon E. sheldon T. shin C. sievers G. smecher m. smith T. somboonpanyakul m. sommer B. stalder A. A. stark J. stephen V. straz University Observatory Faculty of Physics Universität Innsbruck Institut für Astro- und Teilchenphysik Technikerstraße 25/8 6020 Innsbruck Austria High-Energy Physics Division Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Max Planck Institute for Extraterrestrial Physics Gießenbachstraße 1 85748 Garching Germany Argelander-Institut für Astronomie Auf dem Hügel 71 53121 Bonn Germany Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile School of Physics and Astronomy Cardiff University Cardiff CF24 3YB United Kingdom Laboratório Interinstitucional de e-Astronomia—LIneA Rua Gal. José Cristino 77 Rio de Janeiro Rio de Janeiro—20921-400 Brazil Fermi National Accelerator Laboratory P. O. Box 500 Batavia Illinois 60510 USA Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall Stanford California 94305 USA Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo Park California 94025 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Institute of Astronomy University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom School of Physics University of Melbourne Parkville Victoria 3010 Australia NIST Quantum Devices Group 325 Broadway Mailcode 817.03 Boulder Colorado 80305 USA Department of Physics University of Colorado Boulder Colorado 80309 USA Institut de Física d’Altes Energies (IFAE) The Barcelona Institute of Science and Technology Campus UAB 08193 Bellaterra (Barcelona) Spain Institute of Cosmology and Gravitation University of Portsmouth Portsmouth

We present cosmological constraints from the abundance of galaxy clusters selected via the thermal sunyaev-Zel’dovich (sZ) effect in south Pole Telescope (sPT) data with a simultaneous m.s. calibration using weak gravitational lensing data from the Dark Energy survey (DEs) and the Hubble space Telescope (HsT). The cluster sample is constructed from the combined sPT-sZ, sPTpol ECs, and sPTpol 500d surveys, and comprises 1,005 confirmed clusters in the redshift range 0.25–1.78 over a total sky area of 5200 deg2. We use DEs Year 3 weak-lensing data for 688 clusters with redshifts z<0.95 and HsT weak-lensing data for 39 clusters with 0.6sing measurements enable robust m.s. measurements of sample clusters and allow us to empirically constrain the sZ observable-m.s. relation without having to make strong assumptions about, e.g., the hydrodynamical state of the clusters. For a flat ΛCDm cosmology, and marginalizing over the sum of m.s.ive neutrinos, we measure Ωm=0.286±0.032, σ8=0.817±0.026, and the parameter combination σ8(Ωm/0.3)0.25=0.805±0.016. Our measurement of s8≡σ8Ωm/0.3=0.795±0.029 and the constraint from Planck CmB anisotropies (2018 TT, TE, EE+lowE) differ by 1.1σ. In combination with that Planck dataset, we place a 95% upper limit on the sum of neutrino m.s.es ∑mν<0.18 eV. When additionally allowing the dark energy equation of state parameter w to vary, we obtain w=−1.45±0.31 from our cluster-based analysis. In combination with Planck data, we measure w=−1.34−0.15+0.22, or a 2.2σ difference with a cosmological constant. We use the cluster abundance to measure σ8 in five redshift bins between 0.25 and 1.8, and we find the results to be consistent with structure growth as predicted by the ΛCDm model fit to Planck primary CmB data.

关键词： Cosmological parameters Dark energy Large scale structure of the Universe Galaxy clusters

来源：评论

学校读者我要写书评

暂无评论

The protostars in Orion: Characterizing the properties of their magnetized envelopes

arXiv

引用

arXiv 2024年

作者： Huang, Bo Girart, Josep m. stephens, Ian W. López, manuel Fernández myers, Philip C. Zhang, Qizhou Tobin, John J. Cortes, Paulo murillo, Nadia m. sadavoy, sarah Arce, Hector G. Carpenter, John m. Kwon, Woojin Le Gouellec, Valentin J.m. Li, Zhi-Yun Looney, Leslie W. megeath, Tom Cox, Erin G. Karnath, Nicole segura-Cox, Dominique Campus UAB Can Magrans S/N Cerdanyola del Vallès CataloniaE-08193 Spain c/Gran Capita 2-4 Barcelona CataloniaE-08034 Spain Department of Earth Environment and Physics Worcester State University WorcesterMA01602 United States C.C. No. 5 Villa Elisa Buenos Aires1894 Argentina Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States National Radio Astronomy Observatory 520 Edgemont Rd. CharlottesvilleVA22093 United States Joint ALMA Observatory Alonso de Córdova 3107 Vitacura Santiago Chile Instituto de Astronomía Universidad Nacional Autónoma de México AP106 B. C. EnsenadaCP 22830 Mexico Star and Planet Formation Laboratory RIKEN Cluster for Pioneering Research Saitama Wako351-0198 Japan Department of Physics Engineering and Astronomy Queen’s University 64 Bader Lane KingstonONK7L 3N6 Canada Department of Astronomy Yale University New HavenCT06511 United States Joint ALMA Observatory Av. Alonso de Córdova 3107 Vitacura Santiago Chile Department of Earth Science Education Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of SNU Astronomy Research Center Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of The Center for Educational Research Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of NASA Ames Research Center Space Science and Astrobiology Division M.S. 245-6 Moffett FieldCA94035 United States NASA Postdoctoral Program Fellow Astronomy Department University of Virginia CharlottesvilleVA22904 United States Department of Astronomy University of Illinois 1002 West Green Street UrbanaIL61801 United States Department of Astronomy University of Toledo ToledoOH43606 United States 1800 Sherman Avenue EvanstonIL60201 United States SOFIA Science Center Universities Space Research Association NASA Ames Research Center Moffett FieldCA94035 United States Space Science Institute 4765 Walnut

We present a study connecting the physical properties of protostellar envelopes to the morphology of the envelope-scale magnetic field. We used the ALmA polarization observations of 61 young prtostars at 0.87 mm on ∼ 400−3000 au scales from the B-field Orion Protostellar survey to infer the envelope-scale magnetic field, and used the dust em.s.ion to measure the envelope properties on comparable scales. We find that protostars showing standard-hourglass-field morphology tend to have larger m.s.es and lower velocity dispersions in their envelopes, whereas systems with spiral-field morphologies have higher velocity dispersion. Combining with the disk properties taken from the Orion VLA/ALmA Nascent Disk and multiplicity survey, we connect envelope properties to fragmentation. Our results show that the fragmentation level is positively correlated with the angle dispersion of the magnetic field, suggesting that the envelope fragmentation tends to be suppressed by the magnetic field. We also find that protostars exhibiting standard hourglass magnetic field structure tend to have a smaller disk and smaller angle dispersion of the magnetic field than other field configurations, specially the rotated hourglass, but also the spiral and others, suggesting a more effective magnetic braking in the standard hourglass morphology of magnetic fields. Nevertheless, significant m.s.lignment between the magnetic field and outflow axes tends to reduce magnetic braking, leading to the formation of larger disks. Copyright © 2024, 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

Very-high-energy gamma-ray em.s.ion from GRB 201216C detected by mAGIC 37

Very-high-energy gamma-ray emission from GRB 201216C detecte...

引用

37th International Cosmic Ray Conference, ICRC 2021

作者： Fukami, satoshi Berti, Alessio Loporchio, serena suda, Yusuke Nava, Lara Noda, Koji Bošnjak, Željka Asano, Katsuaki Longo, Francesco Acciari, V.A. Ansoldi, s. Antonelli, L.A. Arbet Engels, A. Artero, m. Baack, D. Babić, A. Baquero, A. Barres de Almeida, U. Barrio, J.A. Batković, I. Becerra González, J. Bednarek, W. Bellizzi, L. Bernardini, E. Bernardos, m. Besenrieder, J. Bhattacharyya, W. Bigongiari, C. Biland, A. Blanch, O. Bökenkamp, H. Bonnoli, G. Busetto, G. Carosi, R. Ceribella, G. Cerruti, m. Chai, Y. Chilingarian, A. Cikota, s. Colak, s.m. 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. Delfino, m. Delgado, J. Delgado mendez, C. Depaoli, D. Di Pierro, F. Di Venere, L. Do souto Espiñeira, E. Dominis Prester, D. Donini, A. Dorner, D. Doro, m. Elsaesser, D. Fallah Ramazani, V. Fattorini, A. Fonseca, m.V. Font, L. Fruck, C. Fukazawa, Y. García López, R.J. Garczarczyk, m. Gasparyan, s. Gaug, m. Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Green, J.G. Green, D. Hadasch, D. Hahn, A. Heckmann, L. Herrera, J. Hoang, J. Hrupec, D. Hütten, m. Inada, T. Ishio, K. Iwamura, Y. Jiménez martínez, I. Jormanainen, J. Jouvin, L. Karjalainen, m. Kerszberg, D. Kobayashi, Y. Kubo, H. Kushida, J. Lam.s.ra, A. Lelas, D. Leone, F. Lindfors, E. Linhoff, L. Lombardi, s. López-Coto, R. López-moya, m. López-Oram.s. A. machado de Oliveira Fraga, B. maggio, C. majumdar, P. makariev, m. mallamaci, m. maneva, G. manganaro, m. mannheim, K. maraschi, L. mariotti, m. martínez, m. mazin, D. menchiari, s. mender, s. mićanović, s. miceli, D. miener, T. miranda, J.m. mirzoyan, R. molina, E. moralejo, A. morcuende, D. moreno, V. moretti, E. Nakamori, T. Neustroev, V. Nigro, C. Nilsson, K. Nishijima, K. Nozaki, s. Ohtani, Y. Oka, T. Otero-santos, J. Paiano, s. Palatiello, m. Paneque, D. Paoletti, R. Paredes, J.m. Pavletić, L. Peñil, P. Persic, m. Pihet, m. Prada moroni, P.G. Prandini, E. Institute for Cosmic Ray Research The University of Tokyo Kashiwanoha 5-1-5 Kashiwa Japan Max Planck Institut for Physics Föhringer Ring 6 Munich Germany INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica Università e del Politecnico di Bari BariI-70125 Italy Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Hiroshima739-8526 Japan Street number Merate Italy Faculty of Electrical Engineering and Computing University of Zagreb Zagreb Croatia University of Trieste Department of Physics via Valerio 2 Trieste Italy INFN Sezione di Trieste via Valerio 2 Trieste Italy Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna Tenerife La LagunaE-38200 Spain Università di Udine INFN Trieste UdineI-33100 Italy RomeI-00136 Italy ETH Zürich ZürichCH-8093 Switzerland Bellaterra BarcelonaE-08193 Spain The University of Tokyo Chiba Kashiwa277-8582 Japan 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 Università di Padova INFN PadovaI-35131 Italy University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Università di Siena INFN Pisa SienaI-53100 Italy ZeuthenD-15738 Germany Max-Planck-Institut für Physik MünchenD-80805 Germany Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain 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 INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino TorinoI-10125 Italy Croatian MAGIC Group University o

Gamma-ray bursts (GRBs) are the m.s. energetic phenomena in the Universe. many aspects of GRB physics are still under debate, such as the origin of their gamma-ray em.s.ion above the GeV energy range. In 2019, mAGIC detected TeV gamma rays from the long GRB 190114C, whose em.s.ion can be well explained by synchrotron-self Compton em.s.ion by relativistic electrons. However, it is still unclear whether such a process is common in GRBs, given the reduced number of GRBs detected until now at the very high energies (VHE). GRB 201216C is a long GRB and is the second one detected by mAGIC in this energy range. After receiving the alert provided by swift-BAT, mAGIC automatically slewed to the GRB position, starting observations 56 seconds after the GRB onset. In the offline analyses of the collected data, we confirmed the detection of gamma-ray em.s.ion with a significance above 5 sigma. Following measurements from optical facilities, the redshift of this GRB was estimated to be z = 1.1. This makes GRB 201216C the m.s. distant object ever detected by ground-based gamma-ray telescopes. In this contribution we will show the analysis results of the mAGIC data, also in comparison with past detected GRBs in the same energy range. Finally, accounting for available multi-wavelength observations, we will comment on the possible origin of the VHE em.s.ion detected by mAGIC. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0)

关键词： Germanium compounds

来源：评论

学校读者我要写书评

暂无评论

Joint analysis of Dark Energy survey Year 3 data and CmB lensing from.s.T and Planck. III. Combined cosmological constraints

引用

Physical Review D 2023年第2期107卷 023531-023531页

作者： T. m. C. Abbott m. Aguena A. Alarcon O. Alves A. Amon F. Andrade-Oliveira J. Annis B. Ansarinejad s. Avila D. Bacon E. J. Baxter K. Bechtol m. R. Becker B. A. Benson G. m. Bernstein E. Bertin J. Blazek L. E. Bleem.s. Bocquet D. Brooks E. Buckley-Geer D. L. Burke H. Camacho A. Campos J. E. Carlstrom A. Carnero Rosell m. Carrasco Kind J. Carretero R. Cawthon C. Chang C. L. Chang R. Chen A. Choi R. Chown C. Conselice J. Cordero m. Costanzi T. Crawford A. T. Crites m. Crocce L. N. da Costa C. Davis T. m. Davis T. de Haan J. De Vicente J. DeRose s. Desai H. T. Diehl m. A. Dobbs s. Dodelson P. Doel C. Doux A. Drlica-Wagner K. Eckert T. F. Eifler F. Elsner J. Elvin-Poole s. Everett W. Everett X. Fang I. Ferrero A. Ferté B. Flaugher P. Fosalba O. Friedrich J. Frieman J. García-Bellido m. Gatti E. m. George T. Giannantonio G. Giannini D. Gruen R. A. Gruendl J. Gschwend G. Gutierrez N. W. Halverson I. Harrison K. Herner s. R. Hinton G. P. Holder D. L. Hollowood W. L. Holzapfel K. Honscheid J. D. Hrubes H. Huang E. m. Huff D. Huterer B. Jain D. J. Jam.s.m. Jarvis T. Jeltema s. Kent L. Knox A. Kovacs E. Krause K. Kuehn N. Kuropatkin O. Lahav A. T. Lee P.-F. Leget P. Lem.s.A. R. Liddle C. Lidman D. Luong-Van J. J. mcmahon N. macCrann m. march J. L. marshall P. martini J. mcCullough P. melchior F. menanteau s. s. meyer R. miquel L. mocanu J. J. mohr R. morgan J. muir J. myles T. Natoli A. Navarro-Alsina R. C. Nichol Y. Omori s. Padin s. Pandey Y. Park F. Paz-Chinchón m. E. s. Pereira A. Pieres A. A. Plazas malagón A. Porredon J. Prat C. Pryke m. Raveri C. L. Reichardt R. P. Rollins A. K. Romer A. Roodman R. Rosenfeld A. J. Ross J. E. Ruhl E. s. Rykoff C. sánchez E. sanchez J. sanchez K. K. schaffer L. F. secco I. sevilla-Noarbe E. sheldon T. shin E. shirokoff m. smith Z. staniszewski A. A. stark E. suchyta m. E. C. swanson G. Tarle C. To m. A. Troxel I. Tutusaus T. N. Varga J. D. Vieira N. Weaverdyck R. H. Wechsler J. Weller R. Williamson W. L. K. Wu B. Yanny B. Yin Y. Zhang J. Zuntz Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Laboratório Interinstitucional de e-Astronomia–LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ–20921-400 Brazil Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Institute of Astronomy University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Fermi National Accelerator Laboratory P. O. Box 500 Batavia Illinois 60510 USA School of Physics University of Melbourne Parkville VIC 3010 Australia Instituto de Fisica Teorica UAM/CSIC Universidad Autonoma de Madrid 28049 Madrid Spain Institute of Cosmology and Gravitation University of Portsmouth Portsmouth PO1 3FX United Kingdom Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive Honolulu Hawaii 96822 USA Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue Madison Wisconsin 53706-1390 USA Department of Astronomy and Astrophysics University of Chicago Chicago Illinois 60637 USA Kavli Institute for Cosmological Physics University of Chicago Chicago Illinois 60637 USA Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA CNRS UMR 7095 Institut d’Astrophysique de Paris F-75014 Paris France Sorbonne Universités UPMC Univ Paris 06 UMR 7095 Institut d’Astrophysique de Paris F-75014 Paris France Department of Physics Northeastern University Boston Massachusetts 02115 USA High-Energy Physics Division Argonne National Laboratory 9700 South Cass Avenue Argonne Illinois 60439 USA University Observatory Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 81679 Munich Germany Department of Physics and Astronomy University College London Gower Stre

We present cosmological constraints from the analysis of two-point correlation functions between galaxy positions and galaxy lensing measured in Dark Energy survey (DEs) Year 3 data and measurements of cosmic microwave background (CmB) lensing from the south Pole Telescope (sPT) and Planck. When jointly analyzing the DEs-only two-point functions and the DEs cross-correlations with sPT+Planck CmB lensing, we find Ωm=0.344±0.030 and s8≡σ8(Ωm/0.3)0.5=0.773±0.016, assuming ΛCDm. When additionally combining with measurements of the CmB lensing autospectrum, we find Ωm=0.306−0.021+0.018 and s8=0.792±0.012. The high signal-to-noise of the CmB lensing cross-correlations enables several powerful consistency tests of these results, including comparisons with constraints derived from cross-correlations only, and comparisons designed to test the robustness of the galaxy lensing and clustering measurements from DEs. Applying these tests to our measurements, we find no evidence of significant biases in the baseline cosmological constraints from the DEs-only analyses or from the joint analyses with CmB lensing cross-correlations. However, the CmB lensing cross-correlations suggest possible problems with the correlation function measurements using alternative lens galaxy samples, in particular the redmagic galaxies and high-redshift maglim galaxies, consistent with the findings of previous studies. We use the CmB lensing cross-correlations to identify directions for further investigating these problems.

关键词： Cosmic microwave background Cosmological constant Cosmological parameters Dark energy Dark matter Evolution of the Universe Large scale structure of the Universe Optical, UV, & IR astronomy Normal galaxies

来源：评论

学校读者我要写书评

暂无评论

Excited state m.s. spectra, decay properties and Regge trajectories of charm and charm.s.range m.s.ns

引用

Chinese physics C 2017年第7期41卷 14-24页

作者： Virendrasinh Kher Nayneshkumar Devlani Ajay Kumar Rai Applied Physics Department Polytechnic The M.S. University of Baroda Vadodara 390002 Gujarat India Department of Applied Physics Sardar Vallabhbhai National Institute of Technology Surat 395007 Gujarat India

The framework of a phenomenological quark-antiquark potential（Coulomb plus linear confinement）model with a Gaussian wave function is used for detailed study of m.s.es of the ground, orbitally and radially excited states of heavy-light Qq^-,（Q=c,q=u/d,s） m.s.ns. We incorporate a O（1/m） correction to the potential energy term and relativistic corrections to the kinetic energy term of the Hamiltonian. The spin-hyperfine, spin-orbit and tensor interactions incorporating the effect of mixing are employed to obtain the pseudoscalar, vector, radially and orbitally excited state m.s.n m.s.es. The Regge trajectories in the（J,m^2） and（nr,m^2） planes for heavy-light m.s.ns are investigated with their corresponding parameters. Leptonic and radiative leptonic decay widths and corresponding branching ratios are computed. The mixing parameters are also estimated. Our predictions are in good agreement with experimental results as well as lattice and other theoretical models.

关键词： charm m.s.n strange m.s.n potential model

来源：评论

学校读者我要写书评

暂无评论

Joint analysis of Dark Energy survey Year 3 data and CmB lensing from.s.T and Planck. II. Cross-correlation measurements and cosmological constraints

引用

Physical Review D 2023年第2期107卷 023530-023530页

作者： C. Chang Y. Omori E. J. Baxter C. Doux A. Choi s. Pandey A. Alarcon O. Alves A. Amon F. Andrade-Oliveira K. Bechtol m. R. Becker G. m. Bernstein F. Bianchini J. Blazek L. E. Bleem H. Camacho A. Campos A. Carnero Rosell m. Carrasco Kind R. Cawthon R. Chen J. Cordero T. m. Crawford m. Crocce C. Davis J. DeRose s. Dodelson A. Drlica-Wagner K. Eckert T. F. Eifler F. Elsner J. Elvin-Poole s. Everett X. Fang A. Ferté P. Fosalba O. Friedrich m. Gatti G. Giannini D. Gruen R. A. Gruendl I. Harrison K. Herner H. Huang E. m. Huff D. Huterer m. Jarvis A. Kovacs E. Krause N. Kuropatkin P.-F. Leget P. Lem.s.A. R. Liddle N. macCrann J. mcCullough J. muir J. myles A. Navarro-Alsina Y. Park A. Porredon J. Prat m. Raveri R. P. Rollins A. Roodman R. Rosenfeld A. J. Ross E. s. Rykoff C. sánchez J. sanchez L. F. secco I. sevilla-Noarbe E. sheldon T. shin m. A. Troxel I. Tutusaus T. N. Varga N. Weaverdyck R. H. Wechsler W. L. K. Wu B. Yanny B. Yin Y. Zhang J. Zuntz T. m. C. Abbott m. Aguena s. Allam J. Annis D. Bacon B. A. Benson E. Bertin s. Bocquet D. Brooks D. L. Burke J. E. Carlstrom J. Carretero C. L. Chang R. Chown m. Costanzi L. N. da Costa A. T. Crites m. E. s. Pereira T. de Haan J. De Vicente s. Desai H. T. Diehl m. A. Dobbs P. Doel W. Everett I. Ferrero B. Flaugher D. Friedel J. Frieman J. García-Bellido E. Gaztanaga E. m. George T. Giannantonio N. W. Halverson s. R. Hinton G. P. Holder D. L. Hollowood W. L. Holzapfel K. Honscheid J. D. Hrubes D. J. Jam.s.L. Knox K. Kuehn O. Lahav A. T. Lee m. Lima D. Luong-Van m. march J. J. mcmahon P. melchior F. menanteau s. s. meyer R. miquel L. mocanu J. J. mohr R. morgan T. Natoli s. Padin A. Palm.s. F. Paz-Chinchón A. Pieres A. A. Plazas malagón C. Pryke C. L. Reichardt m. Rodríguez-monroy A. K. Romer J. E. Ruhl E. sanchez K. K. schaffer m. schubnell s. serrano E. shirokoff m. smith Z. staniszewski A. A. stark E. suchyta G. Tarle D. Thom.s.C. To J. D. Vieira J. Weller R. Williamson Department of Astronomy and Astrophysics University of Chicago Chicago Illinois 60637 USA Kavli Institute for Cosmological Physics University of Chicago Chicago Illinois 60637 USA Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA Kavli Institute for Particle Astrophysics & Cosmology P. O. Box 2450 Stanford University Stanford California 94305 USA Institute for Astronomy University of Hawai‘i 2680 Woodlawn Drive Honolulu Hawaii 96822 USA Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA California Institute of Technology 1200 East California Blvd MC 249-17 Pasadena California 91125 USA Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ - 20921-400 Brazil Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue Madison Wisconsin 53706-1390 School of Physics University of Melbourne Parkville Victoria 3010 Australia Department of Physics Northeastern University Boston Massachusetts 02115 USA Laboratory of Astrophysics École Polytechnique Fédérale de Lausanne (EPFL) Observatoire de Sauverny 1290 Versoix Switzerland Instituto de Física Teórica Universidade Estadual Paulista São Paulo Brazil Department of Physics Carnegie Mellon University Pittsburgh Pennsylvania 15312 USA Instituto de Astrofisica de Canarias E-38205 La Laguna Tenerife Spain Universidad de La Laguna Dpto. Astrofísica E-38206 La Laguna Tenerife Spain Center for Astrophysical Surveys National Center for Supercomputing Applications 1205 West Clark St. Urbana Illinois 61801 USA Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green Street Urbana Illinois 61801 USA Physics Department William Jewell College Liberty Missouri 6

Cross-correlations of galaxy positions and galaxy shears with maps of gravitational lensing of the cosmic microwave background (CmB) are sensitive to the distribution of large-scale structure in the Universe. such cross-correlations are also expected to be immune to some of the systematic effects that complicate correlation measurements internal to galaxy surveys. We present measurements and modeling of the cross-correlations between galaxy positions and galaxy lensing measured in the first three years of data from the Dark Energy survey with CmB lensing maps derived from a combination of data from the 2500 deg2 sPT-sZ survey conducted with the south Pole Telescope and full-sky data from the Planck satellite. The CmB lensing maps used in this analysis have been constructed in a way that minimizes biases from the thermal sunyaev Zel’dovich effect, making them well suited for cross-correlation studies. The total signal-to-noise of the cross-correlation measurements is 23.9 (25.7) when using a choice of angular scales optimized for a linear (nonlinear) galaxy bias model. We use the cross-correlation measurements to obtain constraints on cosmological parameters. For our fiducial galaxy sample, which consist of four bins of magnitude-selected galaxies, we find constraints of Ωm=0.272−0.052+0.032 and s8≡σ8Ωm/0.3=0.736−0.028+0.032 (Ωm=0.245−0.044+0.026 and s8=0.734−0.028+0.035) when assuming linear (nonlinear) galaxy bias in our modeling. Considering only the cross-correlation of galaxy shear with CmB lensing, we find Ωm=0.270−0.061+0.043 and s8=0.740−0.029+0.034. Our constraints on s8 are consistent with recent cosmic shear measurements, but lower than the values preferred by primary CmB measurements from Planck.

关键词： Cosmic microwave background Cosmological parameters Large scale structure of the Universe

来源：评论

学校读者我要写书评

暂无评论

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

引用

Astronomy and Astrophysics 2025年 694卷

作者： mAGIC Collaboration 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. Lam.s.ra, A. Leone, F. Lindfors, E. Lombardi, s. Longo, F. López-Coto, R. López-moya, m. López-Oram.s. A. Loporchio, s. Lorini, A. Lyard, E. machado De Oliveira Fraga, B. majumdar, P. makariev, m. maneva, G. manganaro, m. ETH Zürich ZürichCH-8093 Switzerland Università di Siena and INFN Pisa SienaI-53100 Italy 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 and INFN Trieste UdineI-33100 Italy Max-Planck-Institut für Physik GarchingD-85748 Germany Università di Padova and INFN PadovaI-35131 Italy Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia Rio de Janeiro22290-180 URCA Brazil IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna 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 and INFN Pisa PisaI-56126 Italy INFN MAGIC Group: INFN Sezione di Bari Dipartimento Interateneo di Fisica dell'Università e del Politecnico di Bari BariI-70125 Italy Department for Physics and Technology University of Bergen 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 Centre for Astronomy with ESO Department of Physics and Astronomy U

self-repairing graphite protective layer has been discovered as a suitable protective layer in blast furnace (BF) hearth in recent years. In the current study, actual samples of self-repairing graphite protective layer taken from a commercial BF were analyzed in detail. The results revealed that the hot face of graphite protective layer exhibits a distinct white graphite luster, with large areas of graphite adhering to the surface. Along the direction of its formation, the sample displays a striped pattern with alternating layers. The graphite is strip-shaped, it is relatively coarse and unevenly distributed. The coarse graphite runs in the same direction, unlike graphite in molten iron which has no fixed direction in a chaotic state. The formation process of selfrepairing graphite protective layer can be concluded, graphite precipitates at the interface through heterogeneous nucleation. Crystal nuclei often preferentially adhere to the surface of these impurities to form, owing to the fact that the nucleation energy of heterogeneous nucleation is lower than that of homogeneous nucleation. Titanium is discovered during the observation of microscopic morphology of graphite protective layer, graphite protective layer is more robust due to the strengthening effect of titanium. Titanium.s.rengthening mechanism of self-repairing graphite protective layer is summarized, the strengthening mechanism can be divided into four steps. TiC particles are dispersed around graphite, which reduces the difficulty of the orientation of flake graphite growth. The presence of TiC increases the growth rate of crystals. The four steps are cyclically performed, so the self-repairing graphite protective layer can precipitate layer by layer through titanium.s.rengthening mechanism, which serves to protect the carbon brick in BF hearth. © EDP sciences, 2025.

关键词： Blast furnaces

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：