Multiwavelength Observations of 2HWC J1928+177: Dark Accelerator or New TeV Gamma-Ray Binary?

Mori, Kaya; An, Hongjun; Feng, Q.; Malone, K.; Prado, R. R.; Schutt, Yve E.; Dingus, B. L.; Gotthelf, E. V.; Hailey, Charles J.; Hare, Jeremy; Kargaltsev, Oleg; Mukherjee, R.

doi:10.3847/1538-4357/ab9631

Cited by 9 publications

(9 citation statements)

References 40 publications

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“…Note that NAIMA does not model the secondary electron energy distribution self-consistently from the proton−proton collisions in the PionDecay model component. Hence, following the method of Mori et al (2020), we added separate Synchrotron and Inverse-Compton components to account for the contribution of secondary electrons in the X-ray and TeV bands. We assumed the same energy spectrum for protons and secondary electrons (electron α = 1.5 and cutoff energy E cut = 100 TeV for HAWC J1826−128).…”

Section: Hadronic Model Fitting In Naimamentioning

confidence: 99%

“…We assumed the same energy spectrum for protons and secondary electrons (electron α = 1.5 and cutoff energy E cut = 100 TeV for HAWC J1826−128). We adjusted the flux normalizations of the synchrotron and ICS components by imposing that the total energy of secondary electrons (W e ) is 1/3 of the total energy of injected protons, which accounts for the branching ratios of charged pions produced from p-p collisions (Coerver et al 2019;Mori et al 2020).…”

Section: Hadronic Model Fitting In Naimamentioning

confidence: 99%

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The Eel Pulsar Wind Nebula: A PeVatron-candidate Origin for HAWC J1826−128 and HESS J1826−130

Burgess

Mori

Gelfand

et al. 2022

ApJ

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HAWC J1826−128 is one of the brightest Galactic TeV γ-ray sources detected by the High Altitude Water Cherenkov (HAWC) observatory, with photon energies extending up to nearly ∼100 TeV. This HAWC source spatially coincides with the H.E.S.S. TeV source HESS J1826−130 and the “Eel” pulsar wind nebula (PWN), which is associated with the GeV pulsar PSR J1826−1256. In the X-ray band, Chandra and XMM-Newton revealed that the Eel PWN is composed of both a compact nebula (∼15″) and diffuse X-ray emission (∼6′ × 2′) extending away from the pulsar. Our NuSTAR observation detected hard X-ray emission from the compact PWN up to ∼20 keV and evidence of the synchrotron burn-off effect. In addition to the spatial coincidence between HESS J1826−130 and the diffuse X-ray PWN, our multiwavelength spectral energy distribution (SED) analysis using X-ray and γ-ray data establishes a leptonic origin of the TeV emission associated with the Eel PWN. Furthermore, our evolutionary PWN SED model suggests (1) a low PWN B-field of ∼1 μG, (2) a significantly younger pulsar age (t ∼ 5.7 kyr) than the characteristic age (τ = 14.4 kyr), and (3) a maximum electron energy of E max = 2 PeV. The low B-field, as well as the putative supersonic motion of the pulsar, may account for the asymmetric morphology of the diffuse X-ray emission. Our results suggest that the Eel PWN may be a leptonic PeVatron particle accelerator powered by the ∼6 kyr old pulsar PSR J1826−1256 with a spin-down power of 3.6 × 1036 erg s−1.

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Section: Hadronic Model Fitting In Naimamentioning

confidence: 99%

Section: Hadronic Model Fitting In Naimamentioning

confidence: 99%

The Eel Pulsar Wind Nebula: A PeVatron-candidate Origin for HAWC J1826−128 and HESS J1826−130

Burgess

Mori

Gelfand

et al. 2022

ApJ

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“…A dedicated study of this source suggested an association with the energetic pulsar PSR J1928+1746, implying a leptonic, PWN origin for the gamma-ray emission (Lopez-Coto et al 2017). More recently, alternative scenarios including an illuminated molecular cloud or a gamma-ray binary were shown to remain plausible by Mori et al (2020). They also state that further X-ray observations are necessary to clarify a PWN association for the emission.…”

Section: Potentially Bright Clouds Observable By Hawcmentioning

confidence: 86%

Using interstellar clouds to search for Galactic PeVatrons: gamma-ray signatures from supernova remnants

Mitchell

Rowell

Celli

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Interstellar clouds can act as target material for hadronic cosmic rays; gamma rays subsequently produced through inelastic proton-proton collisions and spatially associated with such clouds can provide a key indicator of efficient particle acceleration. However, even in the case that particle acceleration proceeds up to PeV energies, the system of accelerator and nearby target material must fulfil a specific set of conditions in order to produce a detectable gamma-ray flux. In this study, we rigorously characterise the necessary properties of both cloud and accelerator. By using available Supernova Remnant (SNR) and interstellar cloud catalogues, we produce a ranked shortlist of the most promising target systems, those for which a detectable gamma-ray flux is predicted, in the case that particles are accelerated to PeV energies in a nearby SNR. We discuss detection prospects for future facilities including CTA, LHAASO and SWGO; and compare our predictions with known gamma-ray sources. The four interstellar clouds with the brightest predicted fluxes >100 TeV identified by this model are located at (l,b) = (330.05, 0.13), (15.82, -0.46), (271.09, -1.26), and (21.97, -0.29). These clouds are consistently bright under a range of model scenarios, including variation in the diffusion coefficient and particle spectrum. On average, a detectable gamma-ray flux is more likely for more massive clouds; systems with lower separation distance between the SNR and cloud; and for slightly older SNRs.

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“…LHAASO J1929+1745 is even one of the dimmest LHAASO sources at 100 TeV energy (Cao et al 2021a). Mori et al (2020) have tried to explain the gamma-rays from 2HWC J1928+177 (0.10 • from LHAASO J1929+1745) with a hadronic accelerator model.…”

Section: Summary and Discussionmentioning

confidence: 99%

Neutrino Observations of LHAASO Sources: Present Constraints and Future Prospects

Huang,

2021

Preprint

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The Large High Altitude Air Shower Observatory (LHAASO) observed a dozen of gamma-ray sources with significant emission above 100 TeV, which are the possible accelerators of PeV cosmic-rays. The neutrino observations are required to answer whether these high energy gamma-rays are generated through hadronic process (by cosmic-rays) or leptonic process (by electrons). We use the Bayesian method and the ten-year (2008)(2009)(2010)(2011)(2012)(2013)(2014)(2015)(2016)(2017)(2018) IceCube data to constrain the hadronic gamma-ray flux from LHAASO sources. The current observations constrain that the hadronic component contributes no more than ∼70% to the gamma-rays from Crab Nebula, which disfavors the hadronic origin of gamma-rays below hundreds of TeV. For other LHAASO sources, the 90% C.L. upper limits on hadronic gamma-ray flux are still higher than the gamma-ray flux observed. The uncertainties due to the source extension assumption and statistical approach are discussed quantitatively. We also evaluate the neutrino observation of LHAASO sources in the combined search using the current and future neutrino telescopes.

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Multiwavelength Observations of 2HWC J1928+177: Dark Accelerator or New TeV Gamma-Ray Binary?

Cited by 9 publications

References 40 publications

The Eel Pulsar Wind Nebula: A PeVatron-candidate Origin for HAWC J1826−128 and HESS J1826−130

The Eel Pulsar Wind Nebula: A PeVatron-candidate Origin for HAWC J1826−128 and HESS J1826−130

Using interstellar clouds to search for Galactic PeVatrons: gamma-ray signatures from supernova remnants

Neutrino Observations of LHAASO Sources: Present Constraints and Future Prospects

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