Extended Very-High-Energy Gamma-Ray Emission Surrounding PSR 
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi mathvariant="normal">J</mml:mi><mml:mn>0622</mml:mn><mml:mo>+</mml:mo><mml:mn>3749</mml:mn></mml:mrow></mml:math>
 Observed by LHAASO-KM2A

Aharonian, F.; An, Q.; Axikegu,; Bai, Lixin; Bai, Y.; Bao, Yiwei; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai, J. T.; Cao, Z.; Chang, J. F.; Chang, X. C.; Chen, B M; Chen, J; Chen, L; Chen, M J; Chen, Q H; Chen, S H; Chen, T L; Chen, X L; Chen, Y; Cheng, Ning; Cheng, Yaodong; Cui, S. W.; Cui, Xiaohong; Cui, Yudong; Dai, B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu,; Volpe, D. della; Piazzoli, B. D’Ettorre; Dong, X.; Fan, J. H.; Fan, Yi‐Zhong; Zhou, Fan; Fang, Jun; Fang, Kun; Feng, C.; Feng, Li; Feng, S. H.; Feng, Y. L.; Gao, Bo; Gao, Chengyong; Gao, Qi; Gao, Wei; Ge, M. M.; Geng, L. S.; Gong, Guanghua; Gou, Q. B.; Gu, M. H.; Guo, J. G.; Guo, Xiaolei; Guo, Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.; He, J.; He, S. L.; He, Xinyu; He, Y.; Heller, M.; Hor, Y. K.; Hou, Chao; Hou, X.; Hu, Hongbo; Hu, S. C.; Hu, X.; Huang, D.; Huang, Q.; Huang, Wenhao; Huang, X. T.; Huang, Z. C.; Ji, Fei; Ji, X. L.; Jia, H. Y.; Jiang, K.; Jiang, Z. J.; Jin, C.; Kuleshov, D.; Levochkin, K.; Li, B B; Li, C; Li, F; Li, H B; Li, J; Li, K; Li, W L; Li, X; Li, X R; Li, Y; Li, Y Z; Li, Z; Liang, En‐Wei; Liang, Yun-Feng; Lin, S. J.; Liu, B; Liu, C; Liu, D; Liu, H; Liu, H D; Liu, J; Liu, J L; Liu, J S; Liu, M Y; Liu, R Y; Liu, S M; Liu, W; Liu, Y N; Liu, Z X; Long, W. J.; Lü, Rui; Lv, Hongkui; Q, B; L, L; H, X; Mao, J.; Masood, A.; Mitthumsiri, W.; Montaruli, T.; Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi, M. Y.; Ruffolo, D.; Rulev, V.; Sáiz, A.; Shao, L.; Shchegolev, O. B.; Sheng, X. D.; Shi, Jingyan; Song, H. C.; Stenkin, Yu. V.; Stepanov, V.; Sun, Q. N.; Sun, Xiao-Na; Sun, Zhenyu; Tam, P. H. T.; Tang, Z.; Tian, Wei; Wang, B D; Wang, C; Wang, H; Wang, H G; Wang, J C; Wang, J S; Wang, L P; Wang, L Y; Wang, R N; Wang, W; Wang, X G; Wang, X J; Wang, X Y; Wang, Y D; Wang, Z; Wang, Z H; Wang, Z X; Wei, Da-Ming; Wei, J. J.; Wei, Y. J.; Wen, Tao; Wu, C. Y.; Wu, H. R.; Wu, San; Wu, W. X.; Wu, Xue-Feng; Xi, Shao-Qiang; Xia, J.; Xiang, G. M.; Xiao, G. C.; Xiao, H. B.; Xin, G. G.; Xin, Y.; Xing, Yongzhong; Xu, D. L.; Xu, R. X.; Xue, L.; Yan, Dahai; Yang, Chaowen; Yang, Fang; Yang, Jian-Huan; Yang, Lili; Yang, Min; Yang, R.; Yang, S. B.; Yao, Y. H.; Yao, Z. G.; Ye, Y M; Yin, L. Q.; Yin, Na; You, X. H.; You, Z. Y.; Yu, Y. H.; Yuan, Qiang; Zeng, Houdun; Zeng, Tingxuan; Zeng, W.; Zeng, Z. K.; Zha, M.; Zhai, X. X.; Zhang, B B; Zhang, H M; Zhang, H Y; Zhang, J L; Zhang, J W; Zhang, L; Zhang, L X; Zhang, P F; Zhang, P P; Zhang, R; Zhang, S R; Zhang, S S; Zhang, X; Zhang, X P; Zhang, Y; Zhang, Y F; Zhao, Bing; Zhao, J.; Liu, Zhao; Zhao, S. P.; Zheng, F.; Zheng, Y.; Zhou, Bin; Zhou, H.; Zhou, J. N.; Zhou, Ping; Zhou, Rong; Zhou, X. X.; Zhu, C. G.; Zhu, F. R.; Zhu, Hui; Zhu, K.; Zuo, Xin; Huang, Xianchao

doi:10.1103/physrevlett.126.241103

Cited by 98 publications

(57 citation statements)

References 50 publications

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“…In view of the results above, we conclude that, within the context of 1D simulations, the self-generation mechanism can be highly efficient in suppressing the diffusion coefficient surrounding TeV halos by 2-3 orders of magnitude at distances between 10-20 pc from the pulsar. Moreover, the diffusion coefficient is maximally suppressed on timescales of ∼100 kyr, consistent with the observations of extremely suppressed ISM diffusion in the TeV halos that surround multiple middle-aged pulsars [3][4][5][6][7][8][9]. We also note that diffusion remains relatively efficiency within the first ∼10 kyr, which may explain the lack of an observed TeV halo around the Crab nebula and the observation of only a dim halo around Vela (although we note that the PWN, which is not modeled in this analysis, also plays a significant role in electron propagation at such an early stage).…”

Section: B Robustness Of Resultssupporting

confidence: 84%

“…TeV halos are a distinct class of galactic γ-ray emission sources characterized by their hard γ-ray spectrum, spatially extended and roughly spherically symmetric morphology, and coincidence with middle-aged pulsars. Building on initial observations by the High Altitude Water Cherenkov (HAWC) telescope of two TeV halos surrounding the Geminga and Monogem pulsars [1,2], subsequent observations by HAWC, the High-Energy Steroscopic System (H.E.S.S) and Large High-Altitude Air Shower Observatory (LHAASO) have identified at least 8 TeV halo systems [3][4][5][6][7][8][9]. Dozens of other systems have been discussed as possible TeV halos, or TeV Halo/Pulsar Wind Nebulae (PWN) composite systems [3,7,10,11] , a distinction which primarily depends on the definition used to distinguish standard PWNe from the more extended and diffuse TeV halos [7,12].…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Self-Generated Cosmic-Ray Turbulence Can Explain the Morphology of TeV Halos

Mukhopadhyay,

Linden

2021

Preprint

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Observations have shown that spatially extended "TeV halos" are a common (and potentially generic) feature surrounding young and middle-aged pulsars. However, their morphology is not understood. They are larger than the "compact" region where the stellar remnant dominates the properties of the interstellar medium, but smaller than expected in models of cosmic-ray diffusion through the standard interstellar medium. Several explanations have been proposed, but all have shortcomings. Here, we revisit a class of models where the cosmic-ray gradient produced by the central source induces a streaming stability that "self-confines" the cosmic-ray population. We find that previous studies significantly underpredicted the degree of cosmic-ray confinement and show that corrected models can significantly inhibit cosmic-ray diffusion throughout the TeV halo, especially when similar contributions from the coincident supernova remnant are included.

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Section: B Robustness Of Resultssupporting

confidence: 84%

Section: Introductionmentioning

confidence: 99%

Self-Generated Cosmic-Ray Turbulence Can Explain the Morphology of TeV Halos

Mukhopadhyay,

Linden

2021

Preprint

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show abstract

“…As shown in Ref. [17], the two-zone model can explain the spectrum in the energy range from a few tens of GeV to ∼ 100 TeV.…”

Section: Introductionmentioning

confidence: 68%

“…Recently, the LHAASO collaboration reports an extended TeV gamma-ray source named LHAASO J0621+3755, which is very likely to be a new pulsar halo [17]. The associated pulsar, PSR J0622+3749, is located right in the center of the gamma-ray halo and has a similar age and spin-down luminosity to Geminga.…”

Section: Introductionmentioning

confidence: 99%

Self-consistent interpretations of the multi-wavelength gamma-ray spectrum of LHAASO J0621$+$3755

Fang,

Xi,

2021

Preprint

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LHAASO J0621+3755 is a TeV gamma-ray halo newly identified by LHAASO-KM2A. It is likely to be generated by electrons trapped in a slow-diffusion zone around PSR J0622+3749 through inverse Compton scattering. When the gamma-ray spectrum of LHAASO-KM2A is fitted, the GeV fluxes derived by the commonly used one-zone normal diffusion model for electron propagation are significantly higher than the upper limits (ULs) of Fermi-LAT. In this work, we respectively adopt the one-zone superdiffusion and two-zone normal diffusion models to solve this conflict. For the superdiffusion scenario, we find that a model with superdiffusion index α 1.2 can meet the constraints of Fermi-LAT observation. For the two-zone diffusion scenario, the size of the slow-diffusion zone is required to be smaller than ∼ 50 pc, which is consistent with theoretical expectations. Future precise measurements of the Geminga halo may further distinguish between these two scenarios for the electron propagation in pulsar halos.

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“…Work from [9] at GeV energies with Fermi-LAT observed the halos around Geminga and Monogem and confirmed the presence of a slow diffusion region up to 100 parsecs. The recent observations from [10] measured region slow diffusion at ∼ 160 TeV region for halo around PSR J0622+3749 which claims slow diffusion is a property of TeV halos.…”

Section: Introductionmentioning

confidence: 91%

Follow-up Analysis to Geminga's contribution to the Local Positron Excess with HAWC Gamma-Ray Observatory

Escobedo¹,

Zhou²,

Fuente³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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Two cosmic-ray experiments, PAMELA and AMS-02, measured an abnormal positron excess above 10 GeV. This excess is well understood, but it has been considered direct evidence of dark matter. However, this excess could be produced by nearby pulsars too. The HAWC collaboration previously studied the extended gamma-ray emission of two nearby pulsars, Geminga and PSR B0656+14, but found no significant contribution to this excess from these pulsars. The previous study of HAWC led to the reinterpretation of our result and initiated the concept of inverse Compton (IC) halos. Fitting a new halo model and 1343 days of data from the HAWC gamma-ray observatory may better constrain the contribution of these pulsars to the positron excess. This halo model utilizes 3D templates of gamma-ray emission from electron IC interactions to fit the diffusion coefficient and electron injection spectral index. This model can further help to study the energy-dependent diffusion and incorporate anisotropic diffusion with the proper motion of the pulsar.

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Extended Very-High-Energy Gamma-Ray Emission Surrounding PSR J0622+3749 Observed by LHAASO-KM2A

Cited by 98 publications

References 50 publications

Self-Generated Cosmic-Ray Turbulence Can Explain the Morphology of TeV Halos

Self-Generated Cosmic-Ray Turbulence Can Explain the Morphology of TeV Halos

Self-consistent interpretations of the multi-wavelength gamma-ray spectrum of LHAASO J0621$+$3755

Follow-up Analysis to Geminga's contribution to the Local Positron Excess with HAWC Gamma-Ray Observatory

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