Broadband γ-Ray Spectrum of Supernova Remnant Cassiopeia A
dc.contributor.author | Cao Z. | |
dc.contributor.author | Aharonian F. | |
dc.contributor.author | Bai Y.X. | |
dc.contributor.author | Bao Y.W. | |
dc.contributor.author | Bastieri D. | |
dc.contributor.author | Bi X.J. | |
dc.contributor.author | Bi Y.J. | |
dc.contributor.author | Bian W. | |
dc.contributor.author | Bukevich A.V. | |
dc.contributor.author | Cai C.M. | |
dc.contributor.author | Cao W.Y. | |
dc.contributor.author | Cao Z. | |
dc.contributor.author | Chang J. | |
dc.contributor.author | Chang J.F. | |
dc.contributor.author | Chen A.M. | |
dc.contributor.author | Chen E.S. | |
dc.contributor.author | Chen H.X. | |
dc.contributor.author | Chen L. | |
dc.contributor.author | Chen L. | |
dc.contributor.author | Chen M.J. | |
dc.contributor.author | Chen M.L. | |
dc.contributor.author | Chen Q.H. | |
dc.contributor.author | Chen S. | |
dc.contributor.author | Chen S.H. | |
dc.contributor.author | Chen S.Z. | |
dc.contributor.author | Chen T.L. | |
dc.contributor.author | Chen X.B. | |
dc.contributor.author | Chen X.J. | |
dc.contributor.author | Chen Y. | |
dc.contributor.author | Cheng N. | |
dc.contributor.author | Cheng Y.D. | |
dc.contributor.author | Chu M.C. | |
dc.contributor.author | Cui M.Y. | |
dc.contributor.author | Cui S.W. | |
dc.contributor.author | Cui X.H. | |
dc.contributor.author | Cui Y.D. | |
dc.contributor.author | Dai B.Z. | |
dc.contributor.author | Dai H.L. | |
dc.contributor.author | Dai Z.G. | |
dc.contributor.author | Danzengluobu | |
dc.contributor.author | Diao Y.X. | |
dc.contributor.author | Dong X.Q. | |
dc.contributor.author | Duan K.K. | |
dc.contributor.author | Fan J.H. | |
dc.contributor.author | Fan Y.Z. | |
dc.contributor.author | Fang J. | |
dc.contributor.author | Fang J.H. | |
dc.contributor.author | Fang K. | |
dc.contributor.author | Feng C.F. | |
dc.contributor.author | Feng H. | |
dc.contributor.author | Feng L. | |
dc.contributor.author | Feng S.H. | |
dc.contributor.author | Feng X.T. | |
dc.contributor.author | Feng Y. | |
dc.contributor.author | Feng Y.L. | |
dc.contributor.author | Gabici S. | |
dc.contributor.author | Gao B. | |
dc.contributor.author | Gao C.D. | |
dc.contributor.author | Gao Q. | |
dc.contributor.author | Gao W. | |
dc.contributor.author | Gao W.K. | |
dc.contributor.author | Ge M.M. | |
dc.contributor.author | Ge T.T. | |
dc.contributor.author | Geng L.S. | |
dc.contributor.author | Giacinti G. | |
dc.contributor.author | Gong G.H. | |
dc.contributor.author | Gou Q.B. | |
dc.contributor.author | Gu M.H. | |
dc.contributor.author | Guo F.L. | |
dc.contributor.author | Guo J. | |
dc.contributor.author | Guo X.L. | |
dc.contributor.author | Guo Y.Q. | |
dc.contributor.author | Guo Y.Y. | |
dc.contributor.author | Han Y.A. | |
dc.contributor.author | Hannuksela O.A. | |
dc.contributor.author | Hasan M. | |
dc.contributor.author | He H.H. | |
dc.contributor.author | He H.N. | |
dc.contributor.author | He J.Y. | |
dc.contributor.author | He X.Y. | |
dc.contributor.author | He Y. | |
dc.contributor.author | ndez-Cadena S.H. | |
dc.contributor.author | Hor Y.K. | |
dc.contributor.author | Hou B.W. | |
dc.contributor.author | Hou C. | |
dc.contributor.author | Hou X. | |
dc.contributor.author | Hu H.B. | |
dc.contributor.author | Hu S.C. | |
dc.contributor.author | Huang C. | |
dc.contributor.author | Huang D.H. | |
dc.contributor.author | Huang J.J. | |
dc.contributor.author | Huang T.Q. | |
dc.contributor.author | Huang W.J. | |
dc.contributor.author | Huang X.T. | |
dc.contributor.author | Huang X.Y. | |
dc.contributor.author | Huang Y. | |
dc.contributor.author | Huang Y.Y. | |
dc.contributor.author | Ji X.L. | |
dc.contributor.author | Jia H.Y. | |
dc.contributor.author | Jia K. | |
dc.contributor.correspondence | Cao Z. | |
dc.contributor.other | Mahidol University | |
dc.date.accessioned | 2025-04-02T18:09:33Z | |
dc.date.available | 2025-04-02T18:09:33Z | |
dc.date.issued | 2025-03-20 | |
dc.description.abstract | The core-collapse supernova remnant (SNR) Cassiopeia A (Cas A) is one of the brightest galactic radio sources with an angular radius of ~2.5 ¢ . Although no extension of this source has been detected in the γ-ray band, using more than 1000 days of LHAASO data above ∼0.8 TeV, we find that its spectrum is significantly softer than those obtained with Imaging Air Cherenkov Telescopes (IACTs), and its flux near ∼1 TeV is about 2 times higher. In combination with analyses of more than 16 yr of Fermi-LAT data covering 0.1 GeV–1 TeV, we find that the spectrum above 30 GeV deviates significantly from a single power law and is best described by a smoothly broken power law with a spectral index of 1.90 ± 0.15stat (3.41 ± 0.19stat) below (above) a break energy of 0.63 ± 0.21stat TeV. Given differences in the angular resolution of LHAASO-WCDA and IACTs, TeV γ-ray emission detected with LHAASO may have a significant contribution from regions surrounding the SNR illuminated by particles accelerated earlier, which, however, are treated as background by IACTs. Detailed modeling can be used to constrain the acceleration processes of TeV particles in the early stage of SNR evolution. | |
dc.identifier.citation | Astrophysical Journal Letters Vol.982 No.1 (2025) | |
dc.identifier.doi | 10.3847/2041-8213/adb97c | |
dc.identifier.eissn | 20418213 | |
dc.identifier.issn | 20418205 | |
dc.identifier.scopus | 2-s2.0-105000826702 | |
dc.identifier.uri | https://repository.li.mahidol.ac.th/handle/20.500.14594/108596 | |
dc.rights.holder | SCOPUS | |
dc.subject | Earth and Planetary Sciences | |
dc.subject | Physics and Astronomy | |
dc.title | Broadband γ-Ray Spectrum of Supernova Remnant Cassiopeia A | |
dc.type | Article | |
mu.datasource.scopus | https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=105000826702&origin=inward | |
oaire.citation.issue | 1 | |
oaire.citation.title | Astrophysical Journal Letters | |
oaire.citation.volume | 982 | |
oairecerif.author.affiliation | Zhejiang Lab | |
oairecerif.author.affiliation | State Key Laboratory of Particle Detection & Electronics | |
oairecerif.author.affiliation | Université Paris Cité | |
oairecerif.author.affiliation | Yunnan Observatories | |
oairecerif.author.affiliation | Yerevan State University | |
oairecerif.author.affiliation | Nanjing University | |
oairecerif.author.affiliation | Shanghai Astronomical Observatory Chinese Academy of Sciences | |
oairecerif.author.affiliation | Institute for Nuclear Research of the Russian Academy of Sciences | |
oairecerif.author.affiliation | Shandong University | |
oairecerif.author.affiliation | Yunnan University | |
oairecerif.author.affiliation | Institute of High Energy Physics, Chinese Academy of Sciences | |
oairecerif.author.affiliation | University of Chinese Academy of Sciences | |
oairecerif.author.affiliation | Guangzhou University | |
oairecerif.author.affiliation | Tsinghua University | |
oairecerif.author.affiliation | Shanghai Jiao Tong University | |
oairecerif.author.affiliation | Sun Yat-Sen University | |
oairecerif.author.affiliation | University of Science and Technology of China | |
oairecerif.author.affiliation | Zhengzhou University | |
oairecerif.author.affiliation | National Astronomical Observatories Chinese Academy of Sciences | |
oairecerif.author.affiliation | Max-Planck-Institut für Kernphysik | |
oairecerif.author.affiliation | Southwest Jiaotong University | |
oairecerif.author.affiliation | China Center of Advanced Science and Technology World Laboratory | |
oairecerif.author.affiliation | Purple Mountain Observatory Chinese Academy of Sciences | |
oairecerif.author.affiliation | Chinese University of Hong Kong | |
oairecerif.author.affiliation | Hebei Normal University | |
oairecerif.author.affiliation | Tibet University | |
oairecerif.author.affiliation | TIANFU Cosmic Ray Research Center |