Detection of GeV Gamma-Ray Emission in the Direction of HESS J1731-347 with Fermi-LAT

Guo, Xiaolei; Xin, Y.; Liao, Neng-Hui; Yuan, Qiang; Gao, Wei-Hong; Fan, Yi‐Zhong

doi:10.3847/1538-4357/aaa3f8

Cited by 11 publications

(5 citation statements)

References 59 publications

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“…data performed by Abramowski et al (2011) showed a shell structure in the TeV band and a powerlaw spectrum with a high-energy cutoff. In the GeV band, no emission was found in early studies (Yang et al 2014;Acero et al 2015), but a point source with hard spectrum toward this remnant was detected by Fermi-LAT with more accumulated data (Condon et al 2017;Guo et al 2018). These observational features are very similar to the young SNR RX J1713.7−3946, but their ages are quiet different.…”

Section: Rcw 86 (G3154−23)mentioning

confidence: 84%

Electron Acceleration in Middle-age Shell-type γ-Ray Supernova Remnants

Zhang

Liu²

2019

ApJ

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Over the past decade, γ-ray observations of supernova remnants (SNRs) and accurate cosmic-ray (CR) spectral measurements have significantly advanced our understanding of particle acceleration in SNRs. In combination with multiwavelength observations of a large sample of SNRs, it has been proposed that the highest energy particles are mostly accelerated in young remnants, and the maximum energy that middle-age and old SNRs can accelerate particles to decreases rapidly with the decrease in shock speed. If SNRs dominate the CR flux observed at Earth, a large number of particles need to be accelerated in old SNRs for the soft CR spectrum even though they cannot produce very high-energy CRs. With radio, X-ray, and γ-ray observations of seven middle-age shell-type SNRs, we derive the distribution of high-energy electrons trapped in these remnants via a simple one-zone leptonic emission model and find that their spectral evolution is consistent with such a scenario. In particular, we find that particle acceleration by shocks in middle-age SNRs with an age of t can be described by a unified model with the maximum energy decreasing as t −3.1 and the number of GeV electrons increasing as t 2.5 in the absence of escape from SNRs.

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Section: Rcw 86 (G3154−23)mentioning

confidence: 84%

Electron Acceleration in Middle-age Shell-type γ-Ray Supernova Remnants

Zhang

Liu²

2019

ApJ

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“…In addition, we found that the GeV spectrum is harder than previous work. Such a hard spectrum is similar to SNR RCW 86 [17], RX J0852.0-4622 [18] and HESS J1731-347 [19]. Future more multi-wavelength observations will be helpful to explore the radiation mechanism.…”

Section: Pos(icrc2021)629mentioning

confidence: 67%

Observations of SNR Candidate HESS J1614-518 with Fermi-LAT

Guo¹,

Xin²

2021

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

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is a TeV gamma-ray source discovered by H.E.S.S., and shows a shell-like morphology in TeV band. Since no associated supernova remnant (SNR) is observed in other wavelengths, it is classified as a SNR candidate. In this work, we analyze the GeV gamma-ray emission from HESS J1614-518 using more than 12 years of Fermi Large Area Telescope data. We refine the morphology of the GeV emission. We find that the GeV spectrum is harder than previous work, and the GeV spectrum connects smoothly with the TeV spectrum of HESS J1614-518.

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“…We compare HESS J1640-465 with other SNRs which have the similar γ-ray spectra with HESS J1640-465 (Funk 2015;Guo et al 2017a), such as RX J1713-3946 (Abdo et al 2011;Yuan et al 2011;Zeng et al 2017), RX J0852-4622 (Tanaka et al 2011), RCW 86 (Yuan et al 2014, SN1006 (Acero et al 2010;Araya & Frutos 2012;Xing et al 2016;Condon et al 2017), and HESS J1731-347 (H.E.S.S. Collaboration et al 2011;Guo et al 2018;Condon et al 2017). These SNRs are dynamically younger with fast efficient shocks.…”

Section: Discussionmentioning

confidence: 90%

“…While for dynamically younger SNRs with fast efficient shocks, such as RX J1713-3946 (Yuan et al 2011;Zeng et al 2017; H. E. S. S. Collaboration et al 2016a), RCW 86 (Yuan et al 2014;Ajello et al 2016), and HESS J1731-347 (H.E.S.S. Collaboration et al 2011;Guo et al 2018;Condon et al 2017), the γ-ray emission is usually thought to be from the leptonic process. For PWNe, however, the γ-ray emission is mostly contributed by the leptonic process, such as Vela X (Abdo et al 2010a;Aharonian et al 2006a; H. E. S. S. Collaboration et al 2012), MSH 15-52 (Abdo et al 2010b;Aharonian et al 2005), and HESS J1825-137 (Aharonian et al 2006b;Grondin et al 2011).…”

Section: Introductionmentioning

confidence: 99%

HESS J1640-465: A Gamma-Ray Emitting Pulsar Wind Nebula?

Xin

Liao

Guo

et al. 2018

ApJ

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HESS J1640-465 is an extended TeV γ-ray source and its γ-ray emission whether from the shell of a supernova remnant (SNR) or a pulsar wind nebula (PWN) is still under debate. We reanalyze the GeV γ-ray data in the field of HESS J1640-465 using eight years of Pass 8 data recorded by the Fermi Large Area Telescope. An extended GeV γ-ray source positionally coincident with HESS J1640-465 is found. Its photon spectrum can be described by a power-law with an index of 1.42 ± 0.19 in the energy range of 10-500 GeV, and smoothly connects with the TeV spectrum of HESS J1640-465. The broadband spectrum of HESS J1640-465 can be well fit by a leptonic model with a broken power-law spectrum of electrons with an exponential cut-off at ∼ 300 TeV. The spectral properties of HESS J1640-465 are broadly consistent with the characteristics of other sources identified as PWNe, such as the correlations between high-energy luminosity ratios and the physical parameters of pulsar, including spin-down luminosityĖ and characteristic age τ c . All these pieces of evidence support that the γ-ray emission of HESS J1640-465 may originate from the PWN powered by PSR J1640-4631 rather than the shell of the SNR G338.3-0.0.

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Detection of GeV Gamma-Ray Emission in the Direction of HESS J1731-347 with Fermi-LAT

Cited by 11 publications

References 59 publications

Electron Acceleration in Middle-age Shell-type γ-Ray Supernova Remnants

Electron Acceleration in Middle-age Shell-type γ-Ray Supernova Remnants

Observations of SNR Candidate HESS J1614-518 with Fermi-LAT

HESS J1640-465: A Gamma-Ray Emitting Pulsar Wind Nebula?

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