Gamma-Ray Observation of the Cygnus Region in the 100-TeV Energy Region

Amenomori, M.; Bao, Yiwei; Bi, X. J.; Chen, D.; Chen, T. L.; Chen, Wen-Yun; Chen, Xu; Chen, Y.; Cirennima,; Cui, S. W.; Danzengluobu,; Ding, L. K.; Fang, J.; Fang, Kun; Feng, C.; Feng, Z.; Feng, Z. Y.; Gao, Qi; Gomi, A.; Gou, Q. B.; Guo, Y. Q.; He, H. H.; He, Ze; Hibino, K.; Hotta, N.; Hu, Haibing; Hu, Hongbo; Huang, J.; Jia, H. Y.; Jiang, L.; Jiang, Ping; Jin, Hong-Bo; Kasahara, K.; Katayose, Y.; Kato, C.; Kato, Shinsuke; Kawata, K.; Kozai, M.; Kurashige, D.; Labaciren,; Le, G. M.; Li, A. F.; Li, H. J.; Li, W. J.; Li, Y.; Lin, Yu-Hui; Liu, B.; Liu, C.; Liu, J. S.; Liu, L. Y.; Liu, M. Y.; Liu, Wenlong; Liu, X. L.; Lou, Y.; Lü, H.; Meng, X. R.; Munakata, K.; Nakada, H.; Nakamura, Yuya; Nakazawa, Yu; Nanjo, H.; Ning, C. C.; Nakamura, Masaki; Ohnishi, M.; Ohura, T.; Okukawa, S.; Ozawa, S.; Qian, Lei; Qian, X. L.; Qu, X. B.; Saito, T.; Sakata, M.; Sako, T. K.; Shao, J.; Shibata, M.; Shiomi, A.; Sugimoto, H.; Takano, W.; Takita, M.; Tan, Y. H.; Tateyama, N.; Torii, Shoji; Tsuchiya, H.; Udo, S.; Wang, H.; Wang, Y. P.; Wangdui,; Wu, H. R.; Wu, Qingwen; Xu, Jun; Xue, L.; Yamamoto, Y.; Yang, Z.; Yao, Yixu; Yin, J. H.; Yokoe, Y.; Yu, Nian; Yuan, A. F.; Zhai, L. M.; Zhang, C. P.; Zhang, H. M.; Zhang, J. L.; Zhang, Xiang; Zhang, X. Y.; Zhang, Y.; Zhang, Yi; Zhang, Ying; Zhao, S. P.; Zhaxisangzhu,; Zhou, X. X.; γ<, mrow>; mrow,; msub,

doi:10.1103/physrevlett.127.031102

Cited by 26 publications

(12 citation statements)

References 44 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…It has been proposed that particles can be accelerated by the colliding winds of binaries (e.g., Eichler & Usov 1993) and/or the young massive clusters (Aharonian et al 2019) which are the ionising sources of HIIRs. This is supported by the TeV γ-ray observations towards η Car (H. E. S. S. Collaboration et al 2020) for the colliding winds and the Cygnus region (Aliu et al 2014;Bartoli et al 2014;Amenomori et al 2021;Abeysekara et al 2021) for the massive star clusters. In HIIR G35.6−0.5, although there are not massive stars detected as yet, Paron & Giacani (2010) found six young stellar object (YSO) candidates toward the molecular clump at ∼+53 km s −1 (namely the southern clump in their paper) and concluded that there is an active star-formation region.…”

Section: Origin Of Gamma-raysmentioning

confidence: 53%

“…These Galactic γ-ray sources may be the accelerators of cosmic ray (CRs) below the "knee" energy around ∼ 3 × 10 15 eV if they have the hadronic origin and have the maximum energy of γ-rays above ∼100 TeV. For example, based on the observations toward the typical HIIRs in Milky way, e.g., the Cygnus Region (Aliu et al 2014; Bartoli et al 2014;Amenomori et al 2021;Abeysekara et al 2021), it is suggested that HIIRs are efficient particle accelerators and may be a type of contributors of Galactic CRs. Due to the TeV spectrum without an obvious cutoff, the unidentified TeV source HESS J1858+020 (Aharonian et al 2008; H. E. S. S. Collaboration et al 2018), likely associated with an SNR-HIIR complex 1 G35.6−0.4, may be a good candidate of CR source and provide an unique opportunity to distinguish the contribution of high energy γ-rays from the two components.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

GeV Gamma-ray Emission and Molecular Clouds towards Supernova Remnant G35.6$-$0.4 and the TeV Source HESS J1858+020

Zhang,

Chen,

Zheng

et al. 2022

Preprint

View full text Add to dashboard Cite

It is difficult to distinguish hadronic process from the leptonic one in γ-ray observation, which is however crucial in revealing the origin of cosmic rays. As an endeavor in the regard, we focus in this work on the complex γ-ray emitting region, which partially overlaps with the unidentified TeV source HESS J1858+020 and includes supernova remnant (SNR) G35.6−0.4 and HII region G35.6−0.5. We reanalyze CO-line, HI, and Fermi-LAT GeV γ-ray emission data of this region. The analysis of the molecular and HI data suggests that SNR G35.6−0.4 and HII region G35.6−0.5 are located at different distances. The analysis the GeV γ-rays shows that GeV emission arises from two point sources: one (SrcA) coincident with the SNR, and the other (SrcB) coincident with both HESS J1858+020 and HII region G35.6−0.5. The GeV emission of SrcA can be explained by the hadronic process in the SNR-MC association scenario. The GeV-band spectrum of SrcB and the TeV-band spectrum of HESS J1858+020 can be smoothly connected by a power-law function, with an index of ∼2.2. The connected spectrum is well explained with a hadronic emission, with the cutoff energy of protons above 1 PeV. It thus indicates that there is a potential PeVatron in the HII region and should be further verified with ultra-high energy observations with, e.g., LHAASO.

show abstract

Section: Origin Of Gamma-raysmentioning

confidence: 53%

Section: Introductionmentioning

confidence: 99%

GeV Gamma-ray Emission and Molecular Clouds towards Supernova Remnant G35.6$-$0.4 and the TeV Source HESS J1858+020

Zhang,

Chen,

Zheng

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…The flare flux is well above the fluxes in the TeV regime detected from the population of γ-ray sources in the region (see e.g. Amenomori et al 2021). It also highly exceeds the fluxes from known γ-ray sources including the γ-ray pulsars, supernova remnants (e.g.…”

Section: Introductionmentioning

confidence: 70%

PeV photon and neutrino flares from galactic gamma-ray binaries

Bykov,

Petrov,

Kalyashova

et al. 2021

Preprint

View full text Add to dashboard Cite

The high-energy radiation from short period binaries containing a massive star with a compact relativistic companion was detected from radio to TeV gamma rays. We show here that PeV regime protons can be efficiently accelerated in the regions of collision of relativistic outflows of a compact object with stellar winds in these systems. The accelerated proton spectra in the presented Monte Carlo model have an upturn in the PeV regime and can provide very hard spectra of sub-PeV photons and neutrinos by photo-meson processes in the stellar radiation field. Recent report of a possible sub-PeV gamma-ray flare in coincidence with a high-energy neutrino can be understood in the frame of this model. The gamma-ray binaries may contribute substantially to the Galactic component of the detected high-energy neutrino flux.

show abstract

“…These Galactic γ-ray sources may be the accelerators of cosmic rays (CRs) below the "knee" energy around ∼3 × 10 15 eV if they have the hadronic origin and have the maximum energy of γ-rays above ∼100 TeV. For example, based on the observations of the typical HIIRs in the Milky Way, e.g., the Cygnus Region (Aliu et al 2014;Bartoli et al 2014;Abeysekara et al 2021;Amenomori et al 2021), it is suggested that HIIRs are efficient particle accelerators and may be a type of contributors of Galactic CRs. Due to the TeV spectrum without an obvious cutoff, the unidentified TeV source HESS J1858+020 (Aharonian et al 2008;H.E.S.S.…”

Section: Introductionmentioning

confidence: 99%

GeV Gamma-Ray Emission and Molecular Clouds toward Supernova Remnant G35.6–0.4 and the TeV Source HESS J1858+020

Zhang

Chen

Zheng

et al. 2022

ApJ

View full text Add to dashboard Cite

It is difficult to distinguish the hadronic process from the leptonic one in γ-ray observation, which is however crucial in revealing the origin of cosmic rays. As an endeavor in this regard, we focus in this work on the complex γ-ray emitting region, which partially overlaps with the unidentified TeV source HESS J1858+020 and includes supernova remnant (SNR) G35.6−0.4 and H ii region G35.6−0.5. We reanalyze CO line, H i, and Fermi-LAT GeV γ-ray emission data of this region. The analysis of the molecular and H i data suggests that SNR G35.6−0.4 and H ii region G35.6−0.5 are located at different distances. The analysis of the GeV γ-rays shows that GeV emission arises from two point sources: one (SrcA) coincident with the SNR, and the other (SrcB) coincident with both HESS J1858+020 and H ii region G35.6−0.5. The GeV emission of SrcA can be explained by the hadronic process in the SNR–molecular cloud association scenario. The GeV-band spectrum of SrcB and the TeV-band spectrum of HESS J1858+020 can be smoothly connected by a power-law function, with an index of ∼2.2. The connected spectrum is well explained with a hadronic emission, with the cutoff energy of protons above 1 PeV. It thus indicates that there is a potential PeVatron in the H ii region and should be further verified with ultrahigh-energy observations with, e.g., LHAASO.

show abstract

Gamma-Ray Observation of the Cygnus Region in the 100-TeV Energy Region

Cited by 26 publications

References 44 publications

GeV Gamma-ray Emission and Molecular Clouds towards Supernova Remnant G35.6$-$0.4 and the TeV Source HESS J1858+020

GeV Gamma-ray Emission and Molecular Clouds towards Supernova Remnant G35.6$-$0.4 and the TeV Source HESS J1858+020

PeV photon and neutrino flares from galactic gamma-ray binaries

GeV Gamma-Ray Emission and Molecular Clouds toward Supernova Remnant G35.6–0.4 and the TeV Source HESS J1858+020

Contact Info

Product

Resources

About