LHAASO J2226+6057 as a pulsar wind nebula

Sarkar, Agnibha De; Zhang, W.; Martín, J.; Torres, D. F.; Li, J.; Hou, X.

doi:10.1051/0004-6361/202244841

Cited by 7 publications

(3 citation statements)

References 57 publications

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“…However, an overlap of the later LHAASO and Tibet ASγ data on both their models makes it clear that neither model is confirmed (see Figure 16, bottom), requiring a further analysis with constraints on parameters computed using the LHAASO results. In both [176,205], the authors developed a simplistic one-zone leptonic model (but complete with reverberation effect and PWN age estimation), assuming that the UHE emission comes from the Boomerang PWN. They obtained a good fit but a challenging low value for the magnetic field and a PWN size too large, maybe due to the very simple model used.…”

Section: Lhaaso J2226+6057mentioning

confidence: 99%

The LHAASO PeVatron Bright Sky: What We Learned

Cardillo

Giuliani

2023

Applied Sciences

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The recent detection of 12 γ-ray galactic sources well above E>100 TeV by the LHAASO observatory has been a breakthrough in the context of the search for the origin of cosmic rays (CR). Although most of these sources remain unidentified, they are often spatially correlated with leptonic accelerators, such as pulsar and pulsar wind nebulae (PWNe). This dramatically affects the paradigm for which a γ-ray detection at E>100 TeV implies the presence of a hadronic accelerator of PeV particles (PeVatron). Moreover, the LHAASO results support the idea that sources other than the standard candidates, supernova remnants, can accelerate galactic CRs. In this context, the good angular resolution of future Cherenkov telescopes, such as the ASTRI Mini-Array and CTA, and the higher sensitivity of future neutrino detectors, such as KM3NeT and IceCube-Gen2, will be of crucial importance. In this brief review, we want to summarize the efforts made up to now, from both theoretical and experimental points of view, to fully understand the LHAASO results in the context of the CR acceleration issue.

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Section: Lhaaso J2226+6057mentioning

confidence: 99%

The LHAASO PeVatron Bright Sky: What We Learned

Cardillo

Giuliani

2023

Applied Sciences

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“…After Crab PWN was confirmed to be a PeVatron (Cao et al 2021b), the PWN interpretation of PeVatrons began to be heavily favored. However, recent efforts have suggested that even if a powerful pulsar is present in the vicinity of a UHE gamma-ray source, it is not guaranteed that the corresponding PWN is a PeVatron (De Sarkar et al 2022b). Furthermore, detailed studies also dictated that SNRs associated with dense MCs are viable candidates for being PeVatrons (De Sarkar & Gupta 2022;De Sarkar 2023;Abe et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Dissecting the emission from LHAASO J0341+5258: Implications for future multiwavelength observations

De Sarkar,

Majumdar

2024

A&A

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Context. The Large High Altitude Air Shower Observatory (LHAASO) has detected multiple ultra-high-energy (UHE; Eγ ≥ 100 TeV) gamma-ray sources in the Milky Way Galaxy, which are associated with Galactic “PeVatrons” that accelerate particles up to PeV (=1015 eV) energies. Although supernova remnants (SNRs) and pulsar wind nebulae (PWNe), as source classes, are considered the leading candidates, further theoretical and observational efforts are needed to find conclusive proof that can confirm the nature of these PeVatrons. Aims. The aim of this work is to provide a phenomenological model to account for the emission observed from the direction of LHAASO J0341+5258, an unidentified UHE gamma-ray source observed by LHAASO. Further, we also aim to provide the implications of our model in order to support future observations at multiple wavelengths. Methods. We analyzed 15 yr of Fermi-LAT data to find the high-energy (HE; 100 MeV ≤ Eγ ≤ 100 GeV) GeV gamma-ray counterpart of LHAASO J0341+5258 in the 4FGL-DR3 catalog. We explain the spectrum of the closest 4FGL source, 4FGL J0340.4+5302, by a synchro-curvature emission formalism. We explored the escape-limited hadronic interaction between protons accelerated in an old, now invisible SNR and cold protons inside associated molecular clouds (MCs) and leptonic emission from a putative TeV halo in an effort to explain the multiwavelength (MWL) spectral energy distribution (SED) observed from the LHAASO source region. Results. The spectrum of 4FGL J0340.4+5302 is explained well by the synchro-curvature emission, which, along with its point-like nature, indicates that this object is likely a GeV pulsar. A combined lepto-hadronic emission from SNR+MC and TeV halo scenarios explains the MWL SED of the LHAASO source. In addition, we find that leptonic emission from an individual TeV halo is also consistent with the observed MWL emission. We discuss possible observational avenues that can be explored in the near future and predict the outcome of those observational efforts from the model explored in this paper.

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“…By exploring spectral energy distributions (SEDs) of PWNe, we can investigate the origin of the γ-rays and the distribution of high-energy particles. Some of these UHE γ-ray sources may originate from PWNe (Fang et al 2020;Wen et al 2021;De Sarkar et al 2022;Yu et al 2022;Wu et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Investigating the Multiband Nonthermal Radiative Properties of HESS J1420−607

Tian,

Zhou,

Gong

et al. 2023

PASP

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HESS J1420−607 is a γ-ray emitting source associated with the pulsar wind nebula (PWN) powered by the energetic pulsar PSR J1420−6048. Based on 14 yr of data obtained with the Fermi Large Area Telescope, we re-analyzed its GeV γ-ray radiative properties, resulting in detailed spectra obtained within the band 10–200 GeV. Moreover, we use a one-zone time-dependent model for the multiband nonthermal emission from pulsar wind nebulae to investigate the radiative properties of the nebula associated with HESS J1420−607. Assuming that the electrons/positrons are injected into the PWN with a broken power law spectrum with indexes of ∼1.6 and ∼2.7, as well as a break Lorentz factor of ∼5 × 106, the results indicate that the multi-wavelength spectral energy distribution is consistent with the detected fluxes in both X-rays and γ-rays. The results support that the γ-rays detected can be produced via inverse Compton scattering of the energetic electrons/positrons within the PWN.

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LHAASO J2226+6057 as a pulsar wind nebula

Cited by 7 publications

References 57 publications

The LHAASO PeVatron Bright Sky: What We Learned

The LHAASO PeVatron Bright Sky: What We Learned

Dissecting the emission from LHAASO J0341+5258: Implications for future multiwavelength observations

Investigating the Multiband Nonthermal Radiative Properties of HESS J1420−607

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