Measurement of Ultra-High-Energy Diffuse Gamma-Ray Emission of the Galactic Plane from 10 TeV to 1 PeV with LHAASO-KM2A

Cao, Zhen; Aharonian, F.; An, Q.; Axikegu,; Bai, Y. X.; Bao, Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, J. T.; Cao, Q.; Cao, W. Y.; Cao, Zhe; Chang, J.; Chang, J. F.; Chen, A. M.; Chen, E. S.; Chen, Liang; Chen, Lin; Chen, Long; Chen, M. J.; Chen, M. L.; Chen, Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen, Y.; Cheng, N.; Cheng, Y. D.; Cui, M. Y.; Cui, S. W.; Cui, X. H.; Cui, Y. D.; Dai, B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu,; della Volpe, D.; Dong, X. Q.; Duan, K. K.; Fan, J. H.; Fan, Y. Z.; Fang, J.; Fang, K.; Feng, C. F.; Feng, L.; Feng, S. H.; Feng, X. T.; Feng, Y. L.; Gabici, S.; Gao, B.; Gao, C. D.; Gao, L. Q.; Gao, Q.; Gao, W.; Gao, W. K.; Ge, M. M.; Geng, L. S.; Giacinti, G.; Gong, G. H.; Gou, Q. B.; Gu, M. H.; Guo, F. L.; Guo, X. L.; Guo, Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.; He, H. N.; He, J. Y.; He, X. B.; He, Y.; Heller, M.; Hor, Y. K.; Hou, B. W.; Hou, C.; Hou, X.; Hu, H. B.; Hu, Q.; Hu, S. C.; Huang, D. H.; Huang, T. Q.; Huang, W. J.; Huang, X. T.; Huang, X. Y.; Huang, Y.; Huang, Z. C.; Ji, X. L.; Jia, H. Y.; Jia, K.; Jiang, K.; Jiang, X. W.; Jiang, Z. J.; Jin, M.; Kang, M. M.; Ke, T.; Kuleshov, D.; Kurinov, K.; Li, B. B.; Li, Cheng; Li, Cong; Li, D.; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.; Li, J.; Li, Jian; Li, Jie; Li, K.; Li, W. L.; Li, W. L.; Li, X. R.; Li, Xin; Li, Y. Z.; Li, Zhe; Li, Zhuo; Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu, C.; Liu, D.; Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. Y.; Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.; Liu, Y.; Liu, Y. N.; Lu, R.; Luo, Q.; Lv, H. K.; Ma, B. Q.; Ma, L. L.; Ma, X. H.; Mao, J. R.; Min, Z.; Mitthumsiri, W.; Mu, H. J.; Nan, Y. C.; Neronov, A.; Ou, Z. W.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi, M. Y.; Qi, Y. Q.; Qiao, B. Q.; Qin, J. J.; Ruffolo, D.; Sáiz, A.; Semikoz, D.; Shao, C. Y.; Shao, L.; Shchegolev, O.; Sheng, X. D.; Shu, F. W.; Song, H. C.; Stenkin, Yu. V.; Stepanov, V.; Su, Y.; Sun, Q. N.; Sun, X. N.; Sun, Z. B.; Tam, P. H. T.; Tang, Q. W.; Tang, Z. B.; Tian, W. W.; Wang, C.; Wang, C. B.; Wang, G. W.; Wang, H. G.; Wang, H. H.; Wang, J. C.; Wang, K.; Wang, L. P.; Wang, L. Y.; Wang, P. H.; Wang, R.; Wang, W.; Wang, X. G.; Wang, X. Y.; Wang, Y.; Wang, Y. D.; Wang, Y. J.; Wang, Z. H.; Wang, Z. X.; Wang, Zhen; Wang, Zheng; Wei, D. M.; Wei, J. J.; Wei, Y. J.; Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.; Wu, X. F.; Wu, Y. S.; Xi, S. Q.; Xia, J.; Xia, J. J.; Xiang, G. M.; Xiao, D. X.; Xiao, G.; Xin, G. G.; Xin, Y. L.; Xing, Y.; Xiong, Z.; Xu, D. L.; Xu, R. F.; Xu, R. X.; Xu, W. L.; Xue, L.; Yan, D. H.; Yan, J. Z.; Yan, T.; Yang, C. W.; Yang, F.; Yang, F. F.; Yang, H. W.; Yang, J. Y.; Yang, L. L.; Yang, M. J.; Yang, R. Z.; Yang, S. B.; Yao, Y. H.; Yao, Z. G.; Ye, Y. M.; Yin, L. Q.; Yin, N.; You, X. H.; You, Z. Y.; Yu, Y. H.; Yuan, Q.; Yue, H.; Zeng, H. D.; Zeng, T. X.; Zeng, W.; Zha, M.; Zhang, B. B.; Zhang, F.; Zhang, H. M.; Zhang, H. Y.; Zhang, J. L.; Zhang, L. X.; Zhang, Li; Zhang, P. F.; Zhang, P. P.; Zhang, R.; Zhang, S. B.; Zhang, S. R.; Zhang, S. S.; Zhang, X.; Zhang, X. P.; Zhang, Y. F.; Zhang, Yi; Zhang, Yong; Zhao, B.; Zhao, J.; Zhao, L.; Zhao, L. Z.; Zhao, S. P.; Zheng, F.; Zhou, B.; Zhou, H.; Zhou, J. N.; Zhou, M.; Zhou, P.; Zhou, R.; Zhou, X. X.; Zhu, C. G.; Zhu, F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.; ,

doi:10.1103/physrevlett.131.151001

Cited by 40 publications

(26 citation statements)

References 50 publications

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“…This indicates that they might be from a single population with spatial distribution close to supernova remnants or pulsars. We also note that the longitudinal distribution of the observed diffuse emission seems not to closely follow the gas distribution (Cao et al 2023a), which may further support the unresolved source origin of the excesses.…”

Section: Confronting Model Predictions With Measurementsmentioning

confidence: 71%

“…Motivated by recent measurements of diffuse γ-ray emission from the Galactic plane by LHAASO (Cao et al 2023a), we study an emission model of interactions between Galactic CRs and the ISM in a wide energy range from GeV to PeV. We reanalyze the Fermi-LAT data to derive the diffuse emission from 1 to 500 GeV in the two sky regions consistent with those adopted by LHAASO.…”

Section: Conclusion and Discussionmentioning

confidence: 97%

“…Through subtracting the model cube obtained above from the data, we get the residual photon counts that are expected to be mainly from the Galactic diffuse emission. To have consistent sky regions with the LHAASO measurements, we use the same mask method adopted in the LHAASO analysis (Cao et al 2023a). We divide the residual photon counts by the energy interval of the energy bin, the mean exposure, and the solid angle of selected regions, to obtain the fluxes.…”

Section: Fermi-lat Data Analysismentioning

confidence: 99%

“…The model-predicted diffuse γ-ray spectra, together with the measurements by LHAASO and Fermi-LAT, are shown in Figure 2. For all the model results, we apply the same masks as shown in Cao et al (2023a) to enable a consistent comparison. We can see that the model predictions are only consistent with the data at the lowest energies (less than a few GeV).…”

Section: Confronting Model Predictions With Measurementsmentioning

confidence: 99%

“…Very recently, significantly improved measurements of VHE-UHE diffuse emission from 10 to 1000 TeV from both the inner and outer Galactic plane (Cao et al 2023a) were obtained by the Large High Altitude Air Shower Observatory (LHAASO; Ma et al 2022). Particularly, LHAASO measured diffuse emission from the outer Galactic plane for the first time, which can give more comprehensive constraints on the CR distribution in the Galaxy.…”

Section: Introductionmentioning

confidence: 99%

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Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements

Zhang,

Huang,

et al. 2023

ApJ

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Diffuse γ-ray emission between 10 and 1000 TeV from the Galactic plane was recently measured by the Large High Altitude Air Shower Observatory (LHAASO). These observations will help tremendously in constraining the propagation and interaction of cosmic rays in the Milky Way. Additionally, new measurements of cosmic-ray spectra reach a very high precision of up to 100 TeV energies, revealing multiple spectral structures of various species. In this work, based on up-to-date measurements of local cosmic-ray spectra and a simplified propagation setup, we confront a model prediction of diffuse γ-ray emission with measurements of diffuse γ-rays. To better constrain the low-energy part of the model, we analyze the 14.6 yr of Fermi Large Area Telescope (Fermi-LAT) data to extract the Galactic diffuse emission between 1 and 500 GeV from the same sky regions of LHAASO, after subtracting the contribution from known sources and the isotropic diffuse γ-ray background. The joint Fermi-LAT and LHAASO spectra thus cover a very wide energy range from 1 GeV to 1 PeV with small gaps from 0.5 to 10 TeV. Compared with the prediction, we find that clear excesses between several GeV and ∼60 TeV of the diffuse emission exist. Possible reasons to explain the excesses may include unresolved sources or more complicated propagation models. We illustrate that an exponential cutoff power-law component with an index of −2.40 and a cutoff energy of ∼30 TeV is able to account for such excesses.

show abstract

Section: Confronting Model Predictions With Measurementsmentioning

confidence: 71%

Section: Conclusion and Discussionmentioning

confidence: 97%

Section: Fermi-lat Data Analysismentioning

confidence: 99%

Section: Confronting Model Predictions With Measurementsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements

Zhang,

Huang,

et al. 2023

ApJ

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Gamma-ray halos around pulsars: impact on pulsar wind physics and galactic cosmic ray transport

Amato,

Recchia

2024

Riv. Nuovo Cim.

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TeV haloes are a recently discovered class of very high energy gamma-ray emitters. These sources consist of extended regions of multi-TeV emission, originally observed around the two well-known and nearby pulsars, Geminga and PSR B0656+14 (Monogem), and possibly, with different degrees of confidence, around few more objects with similar age. Since their discovery, TeV haloes have raised much interest in a large part of the scientific community, for the implications their presence can have on a broad range of topics spanning from pulsar physics to cosmic ray physics and dark matter indirect searches. In this article, we review the reasons of interest for TeV haloes and the current status of observations. We discuss the proposed theoretical models and their implications, and conclude with an overlook on the prospects for better understanding this phenomenon.

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Data quality control system and long-term performance monitor of LHAASO-KM2A

Cao,

Aharonian,

Axikegu

et al. 2025

Astroparticle Physics

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Measurement of Ultra-High-Energy Diffuse Gamma-Ray Emission of the Galactic Plane from 10 TeV to 1 PeV with LHAASO-KM2A

Cited by 40 publications

References 50 publications

Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements

Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements

Gamma-ray halos around pulsars: impact on pulsar wind physics and galactic cosmic ray transport

Data quality control system and long-term performance monitor of LHAASO-KM2A

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