Extended Very-High-Energy Gamma-Ray Emission Surrounding PSRJ0622+3749Observed by LHAASO-KM2A,Physical Review Letters

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Extended Very-High-Energy Gamma-Ray Emission Surrounding PSRJ0622+3749Observed by LHAASO-KM2A
Physical Review Letters ( IF 8.1 ) Pub Date : 2021-06-16 , DOI: 10.1103/physrevlett.126.241103
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Affiliation

Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, 2 Dublin, Ireland.
Max-Planck-Institut for Nuclear Physics, P.O. Box 103980, 69029 Heidelberg, Germany.
State Key Laboratory of Particle Detection and Electronics, 100049 Beijing, China.
University of Science and Technology of China, 230026 Hefei, Anhui, China.
School of Physical Science and Technology & School of Information Science and Technology, Southwest Jiaotong University, 610031 Chengdu, Sichuan, China.
College of Physics, Sichuan University, 610065 Chengdu, Sichuan, China.
Key Laboratory of Particle Astrophyics & Experimental Physics Division & Computing Center, Institute of High Energy Physics, Chinese Academy of Sciences, 100049 Beijing, China.
TIANFU Cosmic Ray Research Center, Chengdu, 610000 Sichuan, China.
School of Astronomy and Space Science, Nanjing University, 210023 Nanjing, Jiangsu, China.
Center for Astrophysics, Guangzhou University, 510006 Guangzhou, Guangdong, China.
University of Chinese Academy of Sciences, 100049 Beijing, China.
School of Physics and Technology, Wuhan University, 430072 Wuhan, Hubei, China.
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, 210023 Nanjing, Jiangsu, China.
Hebei Normal University, 050024 Shijiazhuang, Hebei, China.
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 200030 Shanghai, China.
Key Laboratory of Cosmic Rays (Tibet University), Ministry of Education, 850000 Lhasa, Tibet, China.
National Astronomical Observatories, Chinese Academy of Sciences, 100101 Beijing, China.
School of Physics and Astronomy & School of Physics (Guangzhou), Sun Yat-sen University, 519082 Zhuhai, Guangdong, China.
School of Physics and Astronomy, Yunnan University, 650091 Kunming, Yunnan, China.
Département de Physique Nucléaire et Corpusculaire, Faculté de Sciences, Université de Genève, 24 Quai Ernest Ansermet, 1211 Geneva, Switzerland.
Dipartimento di Fisica dell'Università di Napoli "Federico II," Complesso Universitario di Monte Sant'Angelo, via Cinthia, 80126 Napoli, Italy.
Institute of Frontier and Interdisciplinary Science, Shandong University, 266237 Qingdao, Shandong, China.
Department of Engineering Physics, Tsinghua University, 100084 Beijing, China.
School of Physics and Microelectronics, Zhengzhou University, 450001 Zhengzhou, Henan, China.
Yunnan Observatories, Chinese Academy of Sciences, 650216 Kunming, Yunnan, China.
Institute for Nuclear Research of Russian Academy of Sciences, 117312 Moscow, Russia.
School of Physics, Peking University, 100871 Beijing, China.
School of Physical Science and Technology, Guangxi University, 530004 Nanning, Guangxi, China.
Tsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong University, 200240 Shanghai, China.
Department of Physics, Faculty of Science, Mahidol University, 10400 Bangkok, Thailand.
Moscow Institute of Physics and Technology, 141700 Moscow, Russia.
National Space Science Center, Chinese Academy of Sciences, 100190 Beijing, China.

We report the discovery of an extended very-high-energy (VHE) gamma-ray source around the location of the middle-aged (207.8 kyr) pulsar PSR

J 0622 + 3749

with the Large High-Altitude Air Shower Observatory (LHAASO). The source is detected with a significance of

8.2 σ

for

E > 25 TeV

assuming a Gaussian template. The best-fit location is (right ascension, declination)

= (95.47 ° \pm 0.11 °, 37.92 ° \pm 0.09 °)

, and the extension is

0.40 ° \pm 0.07 °

. The energy spectrum can be described by a power-law spectrum with an index of

- 2.92 \pm {0.17}_{stat} \pm {0.02}_{sys}

. No clear extended multiwavelength counterpart of the LHAASO source has been found from the radio to sub-TeV bands. The LHAASO observations are consistent with the scenario that VHE electrons escaped from the pulsar, diffused in the interstellar medium, and scattered the interstellar radiation field. If interpreted as the pulsar halo scenario, the diffusion coefficient, inferred for electrons with median energies of

\sim 160 TeV

, is consistent with those obtained from the extended halos around Geminga and Monogem and much smaller than that derived from cosmic ray secondaries. The LHAASO discovery of this source thus likely enriches the class of so-called pulsar halos and confirms that high-energy particles generally diffuse very slowly in the disturbed medium around pulsars.

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