Publication: Discovery of a New Gamma-Ray Source, LHAASO J0341+5258, with Emission up to 200 TeV
Issued Date
2021-08-10
Resource Type
ISSN
20418213
20418205
20418205
Other identifier(s)
2-s2.0-85113363927
Rights
Mahidol University
Rights Holder(s)
SCOPUS
Bibliographic Citation
Astrophysical Journal Letters. Vol.917, No.1 (2021)
Suggested Citation
Zhen Cao, F. Aharonian, Q. An, Axikegu, L. X. Bai, Y. X. Bai, Y. W. Bao, D. Bastieri, X. J. Bi, Y. J. Bi, H. Cai, J. T. Cai, Zhe Cao, J. Chang, J. F. Chang, B. M. Chen, E. S. Chen, J. Chen, Liang Chen, Liang Chen, Long Chen, M. J. Chen, M. L. Chen, Q. H. Chen, S. H. Chen, S. Z. Chen, T. L. Chen, X. L. Chen, Y. Chen, N. Cheng, Y. D. Cheng, S. W. Cui, X. H. Cui, Y. D. Cui, B. D'Ettorre Piazzoli, B. Z. Dai, H. L. Dai, Z. G. Dai, Danzengluobu, D. Della Volpe, X. J. Dong, K. K. Duan, J. H. Fan, Y. Z. Fan, Z. X. Fan, J. Fang, K. Fang, C. F. Feng, L. Feng, S. H. Feng, Y. L. Feng, B. Gao, C. D. Gao, L. Q. Gao, Q. Gao, W. Gao, M. M. Ge, L. S. Geng, G. H. Gong, Q. B. Gou, M. H. Gu, F. L. Guo, J. G. Guo, X. L. Guo, Y. Q. Guo, Y. Y. Guo, Y. A. Han, H. H. He, H. N. He, J. C. He, S. L. He, X. B. He, Y. He, M. Heller, Y. K. Hor, C. Hou, H. B. Hu, S. Hu, S. C. Hu, X. J. Hu, D. H. Huang, Q. L. Huang, W. H. Huang, X. T. Huang, X. Y. Huang, Z. C. Huang, F. Ji, X. L. Ji, H. Y. Jia, K. Jiang, Z. J. Jiang, C. Jin, T. Ke, D. Kuleshov, K. Levochkin, B. B. Li, Cheng Li, Cong Li, F. Li, H. B. Li Discovery of a New Gamma-Ray Source, LHAASO J0341+5258, with Emission up to 200 TeV. Astrophysical Journal Letters. Vol.917, No.1 (2021). doi:10.3847/2041-8213/ac0fd5 Retrieved from: https://repository.li.mahidol.ac.th/handle/20.500.14594/76856
Research Projects
Organizational Units
Authors
Journal Issue
Thesis
Title
Discovery of a New Gamma-Ray Source, LHAASO J0341+5258, with Emission up to 200 TeV
Author(s)
Zhen Cao
F. Aharonian
Q. An
Axikegu
L. X. Bai
Y. X. Bai
Y. W. Bao
D. Bastieri
X. J. Bi
Y. J. Bi
H. Cai
J. T. Cai
Zhe Cao
J. Chang
J. F. Chang
B. M. Chen
E. S. Chen
J. Chen
Liang Chen
Liang Chen
Long Chen
M. J. Chen
M. L. Chen
Q. H. Chen
S. H. Chen
S. Z. Chen
T. L. Chen
X. L. Chen
Y. Chen
N. Cheng
Y. D. Cheng
S. W. Cui
X. H. Cui
Y. D. Cui
B. D'Ettorre Piazzoli
B. Z. Dai
H. L. Dai
Z. G. Dai
Danzengluobu
D. Della Volpe
X. J. Dong
K. K. Duan
J. H. Fan
Y. Z. Fan
Z. X. Fan
J. Fang
K. Fang
C. F. Feng
L. Feng
S. H. Feng
Y. L. Feng
B. Gao
C. D. Gao
L. Q. Gao
Q. Gao
W. Gao
M. M. Ge
L. S. Geng
G. H. Gong
Q. B. Gou
M. H. Gu
F. L. Guo
J. G. Guo
X. L. Guo
Y. Q. Guo
Y. Y. Guo
Y. A. Han
H. H. He
H. N. He
J. C. He
S. L. He
X. B. He
Y. He
M. Heller
Y. K. Hor
C. Hou
H. B. Hu
S. Hu
S. C. Hu
X. J. Hu
D. H. Huang
Q. L. Huang
W. H. Huang
X. T. Huang
X. Y. Huang
Z. C. Huang
F. Ji
X. L. Ji
H. Y. Jia
K. Jiang
Z. J. Jiang
C. Jin
T. Ke
D. Kuleshov
K. Levochkin
B. B. Li
Cheng Li
Cong Li
F. Li
H. B. Li
F. Aharonian
Q. An
Axikegu
L. X. Bai
Y. X. Bai
Y. W. Bao
D. Bastieri
X. J. Bi
Y. J. Bi
H. Cai
J. T. Cai
Zhe Cao
J. Chang
J. F. Chang
B. M. Chen
E. S. Chen
J. Chen
Liang Chen
Liang Chen
Long Chen
M. J. Chen
M. L. Chen
Q. H. Chen
S. H. Chen
S. Z. Chen
T. L. Chen
X. L. Chen
Y. Chen
N. Cheng
Y. D. Cheng
S. W. Cui
X. H. Cui
Y. D. Cui
B. D'Ettorre Piazzoli
B. Z. Dai
H. L. Dai
Z. G. Dai
Danzengluobu
D. Della Volpe
X. J. Dong
K. K. Duan
J. H. Fan
Y. Z. Fan
Z. X. Fan
J. Fang
K. Fang
C. F. Feng
L. Feng
S. H. Feng
Y. L. Feng
B. Gao
C. D. Gao
L. Q. Gao
Q. Gao
W. Gao
M. M. Ge
L. S. Geng
G. H. Gong
Q. B. Gou
M. H. Gu
F. L. Guo
J. G. Guo
X. L. Guo
Y. Q. Guo
Y. Y. Guo
Y. A. Han
H. H. He
H. N. He
J. C. He
S. L. He
X. B. He
Y. He
M. Heller
Y. K. Hor
C. Hou
H. B. Hu
S. Hu
S. C. Hu
X. J. Hu
D. H. Huang
Q. L. Huang
W. H. Huang
X. T. Huang
X. Y. Huang
Z. C. Huang
F. Ji
X. L. Ji
H. Y. Jia
K. Jiang
Z. J. Jiang
C. Jin
T. Ke
D. Kuleshov
K. Levochkin
B. B. Li
Cheng Li
Cong Li
F. Li
H. B. Li
Other Contributor(s)
State Key Laboratory of Particle Detection & Electronics
Nanjing University
Shanghai Astronomical Observatory Chinese Academy of Sciences
Institute for Nuclear Research of the Russian Academy of Sciences
Shandong University
Wuhan University
Yunnan University
Institute of High Energy Physics Chinese Academy of Science
University of Chinese Academy of Sciences
Guangzhou University
Tsinghua University
Sun Yat-Sen University
University of Science and Technology of China
Zhengzhou University
Dublin Institute for Advanced Studies
Università degli Studi di Napoli Federico II
Sichuan University
National Astronomical Observatories Chinese Academy of Sciences
Max-Planck-Institut für Kernphysik
Southwest Jiaotong University
Purple Mountain Observatory Chinese Academy of Sciences
Hebei Normal University
Tibet University
Universit'e de Gen ve
TIANFU Cosmic Ray Research Center
Nanjing University
Shanghai Astronomical Observatory Chinese Academy of Sciences
Institute for Nuclear Research of the Russian Academy of Sciences
Shandong University
Wuhan University
Yunnan University
Institute of High Energy Physics Chinese Academy of Science
University of Chinese Academy of Sciences
Guangzhou University
Tsinghua University
Sun Yat-Sen University
University of Science and Technology of China
Zhengzhou University
Dublin Institute for Advanced Studies
Università degli Studi di Napoli Federico II
Sichuan University
National Astronomical Observatories Chinese Academy of Sciences
Max-Planck-Institut für Kernphysik
Southwest Jiaotong University
Purple Mountain Observatory Chinese Academy of Sciences
Hebei Normal University
Tibet University
Universit'e de Gen ve
TIANFU Cosmic Ray Research Center
Abstract
We report the discovery of a new unidentified extended γ-ray source in the Galactic plane named LHAASO J0341+5258 with a pretrial significance of 8.2 standard deviations above 25 TeV. The best-fit position is R.A. = 55. 34 0. 11 and decl. = 52. 97 0. 07. The angular size of LHAASO J0341+5258 is 0. 29 0. 06stat 0. 02sys. The flux above 25 TeV is about 20% of the flux of the Crab Nebula. Although a power-law fit of the spectrum from 10 to 200 TeV with the photon index α = 2.98 0.19stat 0.02sys is not excluded, the LHAASO data together with the flux upper limit at 10 GeV set by the Fermi-LAT observation, indicate a noticeable steepening of an initially hard power-law spectrum with a cutoff at ≈50 TeV. We briefly discuss the origin of ultra-high-energy gamma rays. The lack of an energetic pulsar and a young supernova remnant inside or in the vicinity of LHAASO J0341+5258 challenge, but do not exclude, both the leptonic and hadronic scenarios of gamma-ray production.