GeV Emission in the Region of HESS J1809−193 and HESS J1813−178: Is HESS J1809−193 a Proton Pevatron?

Araya, Miguel

doi:10.3847/1538-4357/aabd7e

Cited by 24 publications

(37 citation statements)

References 53 publications

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“…The -ray emission toward HESS J1813-178 with Fermi-LAT Yu-Liang Xin of the uniform disk, following the analysis result by Araya [11], is much larger than that of the TeV -ray emission of HESS J1813-178. Besides, there is a point source (4FGL J1814.1-1710) located in the region of 4FGL J1813.1-1737e, which is suggested to be associated with SNR G13.5+0.2 in the 4FGL catalog.…”

Section: Pos(icrc2021)625mentioning

confidence: 55%

“…Fang & Zhang [10] predicted that the TeV -ray emission is mainly originated from the PWN, although the contribution from the SNR shell could be enhanced with a denser medium. With the Fermi-LAT data, Araya [11] found a much extended GeV -ray emission (radius ∼ 0.6 • ) around HESS J1813-178. The global spectrum in the energy range of 0.5 -500 GeV can be fitted by a power-law with an index of 2.14±0.04, which is not consistent with the IC emission characteristic from leptons in a PWN.…”

Section: Introductionmentioning

confidence: 99%

“…The global spectrum in the energy range of 0.5 -500 GeV can be fitted by a power-law with an index of 2.14±0.04, which is not consistent with the IC emission characteristic from leptons in a PWN. And Araya [11] argued that the extended GeV emission may be related to the star-forming regions around HESS J1813-178, like W33.…”

Section: Introductionmentioning

confidence: 99%

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The gamma-ray emission toward HESS J1813-178 with Fermi-LAT

Xin¹,

Guo²

2021

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

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is one of the brightest and most compact objects detected by the HESS Galactic Plane Survey and MAGIC observations. A young supernova remnant (SNR) G12.8-0.0 locates within the TeV extent of HESS J1813-178. And a pulsar wind nebula (PWN) driven by an energetic X-ray pulsar PSR J1813-1749 is embedded in the SNR, together with a young stellar cluster, C1 1813-178, detected in this region. The origin of the -ray emission from HESS J1813-178 is still not clear. Previous studies show that the GeV emission around HESS J1813-178 is much more extended than its TeV emission. With the Fermi-LAT data analysis, we did a detailed morphological and spectral analysis in the region of HESS J1813-178 and found that the GeV -ray morphology above 20 GeV is much smaller, which is close to the TeV -ray contours. Meanwhile, the GeV spectrum above 20 GeV is hard with an index of ∼ 2.07, which connects smoothly with that of HESS J1813-178.

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Section: Pos(icrc2021)625mentioning

confidence: 55%

Section: Introductionmentioning

confidence: 99%

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The gamma-ray emission toward HESS J1813-178 with Fermi-LAT

Xin¹,

Guo²

2021

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

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“…HAWC has also recently detected the TeV source 2HWC J1809−190, associated with HESS J1809−193 (Abeysekara et al 2017). Araya (2018) recently found extended GeV emission associated with HESS J1809−193.…”

Section: Hess J1809-193mentioning

confidence: 98%

“…Castelletti et al 2016, and more recently Araya (2018), have discussed the hadronic scenario in which they assume the SNR G011.0−0.0 to be located at a distance d ∼3.0 kpc. We focus here on how MCs at d ∼ 3.7 kpc can affect the TeV emission produced by the PWN powered by PSR J1809−1917 and SNR G011.0−0.0, in which we argue they are physically connected.…”

Section: Hess J1809−193mentioning

confidence: 99%

Connecting the ISM to TeV PWNe and PWN candidates

Voisin

Rowell

Burton

et al. 2019

Publ. Astron. Soc. Aust.

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We investigate the interstellar medium (ISM) towards seven TeV gamma-ray sources thought to be pulsar wind nebulae (PWNe) using Mopra molecular line observations at 7mm [CS(1-0), SiO(1-0,v=0)], Nanten CO(1-0) data and the SGPS/GASS Hi survey. We have discovered several dense molecular clouds co-located to these TeV gamma-ray sources, which allows us to search for cosmic-rays (CRs) coming from progenitor SNRs or, potentially, from PWNe. We notably found SiO(1-0,v=0) emission towards HESS J1809−193, highlighting possible interaction between the adjacent supernova remnant SNR G011.0−0.0 and the molecular cloud at d ∼ 3.7 kpc. Using morphological features, and comparative studies of our column densities with those obtained from X-ray measurements, we claim a distance d ∼ 8.6 − 9.7 kpc for SNR G292.2−00.5, d ∼ 3.5 − 5.6 kpc for PSR J1418−6058 and d ∼ 1.5 kpc for the new SNR candidate found towards HESS J1303−631. From our mass and density estimates of selected molecular clouds, we discuss signatures of hadronic/leptonic components from PWNe and their progenitor SNRs. Interestingly, the molecular gas, which overlaps HESS J1026−582 at d ∼5 kpc, may support a hadronic origin. We find however that this scenario requires an undetected cosmic-ray accelerator to be located at d < 10 pc from the molecular cloud. For HESS J1809−193, the cosmic-rays which have escaped SNR G011.0−0.0 could contribute to the TeV gamma-ray emission. Finally, from the hypothesis that at most 20% the pulsar spin down power could be converted into CRs, we find that, among the studied PWNe, only those from PSR J1809−1917 could potentially contribute to the TeV emission.

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