Investigating 
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-ray halos around three HAWC bright sources in 
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-LAT data

Mauro, Mattia Di; Manconi, Silvia; Negro, Michela; Donato, Fiorenza

doi:10.1103/physrevd.104.103002

Cited by 16 publications

(4 citation statements)

References 62 publications

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“…The observed emission is interpreted as coming from CR e ± escaping from the PWN system and ICS low-energy photons of the interstellar radiation field (ISRF). Similar extended gamma-ray halos surrounding pulsars have been recently observed by HAWC, by LHAASO at even higher energies [21,22], and also by Fermi-LAT at tens of GeV implying even larger angular scales [23], suggesting that they might be a general feature of Galactic pulsars [24][25][26]. While the mechanism shaping e ± transport in these halos, and consequently the gamma-ray emission, is not yet fully understood [27][28][29][30][31], the observed extension is well above the typical PWN size inferred at radio and X-ray wavelengths [25].…”

supporting

confidence: 76%

Constraining positron emission from pulsar populations with AMS-02 data

Orusa,

Manconi,

Donato

et al. 2021

Preprint

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The cosmic-ray flux of positrons is measured with high precision by the spaceborne particle spectrometer AMS-02. The hypothesis that pulsar wind nebulae (PWNe) can significantly contribute to the excess of the positron (e + ) cosmic-ray flux has been consolidated after the observation of a γ-ray emission at TeV energies of a few degree size around Geminga and Monogem PWNe. In this work we undertake massive simulations of galactic pulsars populations, adopting different distributions for their position in the Galaxy, intrinsic physical properties, pair emission models, in order to overcome the incompleteness of the ATNF catalogue. We fit the e + AMS-02 data together with a secondary component due to collisions of primary cosmic rays with the interstellar medium. We find that several mock galaxies have a pulsar population able to explain the observed e + flux, typically by few, bright sources. We determine the physical parameters of the pulsars dominating the e + flux, and assess the impact of different assumptions on radial distributions, spin-down properties, Galactic propagation scenarios and e + emission time.

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supporting

confidence: 76%

Constraining positron emission from pulsar populations with AMS-02 data

Orusa,

Manconi,

Donato

et al. 2021

Preprint

Self Cite

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“…Acero et al (2013) calculated upper limits for a GeV PWN of PSR J2021+3651, assuming a size of MGRO J2019+37. Di Mauro et al (2021) used an IC scattering template with the best-fit diffusion coefficient for eHWC J2019+368 to place GeV upper limits on the PWN. Both works resulted in GeV upper limits similar to the flux of eHWC J2019+368.…”

Section: Fermi Analysismentioning

confidence: 99%

Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”

Woo,

An,

Gelfand

et al. 2023

ApJ

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We studied the PeVatron nature of the pulsar wind nebula (PWN) G75.2+0.1 (“Dragonfly”) as part of our NuSTAR observational campaign of energetic PWNe. The Dragonfly is spatially coincident with LHAASO J2018+3651, whose maximum photon energy is 0.27 PeV. We detected a compact (radius 1 ′ ) inner nebula of the Dragonfly without a spectral break in 3–20 keV using NuSTAR. A joint analysis of the inner nebula with archival Chandra and XMM-Newton (XMM) observations yields a power-law spectrum with Γ = 1.49 ± 0.03. Synchrotron burnoff is observed from the shrinkage of the NuSTAR nebula at higher energies, from which we infer the magnetic field in the inner nebula of 24 μG at 3.5 kpc. Our analysis of archival XMM data and 13 yr of Fermi-LAT data confirms the detection of an extended ( ∼ 10 ′ ) outer nebula in 2–6 keV (Γ = 1.82 ± 0.03) and the nondetection of a GeV nebula, respectively. Using the VLA, XMM, and HAWC data, we modeled a multiwavelength spectral energy distribution of the Dragonfly as a leptonic PeVatron. The maximum injected particle energy of 1.4 PeV from our model suggests that the Dragonfly is likely a PeVatron. Our model prediction of the low magnetic field (2.7 μG) in the outer nebula and recent interaction with the host supernova remnant’s reverse shock (4 kyr ago) align with common features of PeVatron PWNe. The origin of its highly asymmetric morphology, pulsar proper motion, PWN–supernova remnant (SNR) interaction, and source distance will require further investigations in the future, including a multiwavelength study using radio, X-ray, and gamma-ray observations.

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“…To verify the non-detection results in the off-pulse data, we calculated 0.1-500 GeV TS maps for the two pulsar regions. PWNe or teraelectronvolt halos may show extended weak emission at gigaelectronvolt energies (e.g., Di Mauro et al 2021). However, as shown by the TS maps (Figure 3), no residual emissions are seen in each of the pulsar regions.…”

Section: Notesmentioning

confidence: 93%

Two Candidate Pulsar TeV Halos Identified from Property-similarity Studies

Zheng,

Wang

2023

ApJ

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Teraelectronvolt halos have been suggested to be a common phenomenon associated with middle-aged pulsars. Based on our recent work on the middle-aged pulsar J0631+1036, which is the only known source positionally coincident with a hard teraelectronvolt γ-ray source and likely powers the latter as a teraelectronvolt halo, we select three candidate teraelectronvolt halos from the first Large High Altitude Air Shower Observatory (LHAASO) catalog of γ-ray sources. The corresponding pulsars, given by the positional coincidences and property similarities, are PSR J1958+2846, PSR J2028+3332, and PSR J1849-0001. We analyze the gigaelectronvolt γ-ray data obtained with the Large Area Telescope on board the Fermi Gamma-ray Space Telescope for the first two pulsars, as the last is γ-ray quiet. We remove the pulsed emissions of the pulsars from the source regions from timing analysis, and determine that there are no residual gigaelectronvolt emissions in the regions as any possible counterparts to the teraelectronvolt sources. Considering the previous observational results for the source regions and comparing the two pulsars to Geminga (and Monogem), the LHAASO-detected teraelectronvolt sources are likely the pulsars’ respective teraelectronvolt halos. We find that the candidate and identified teraelectronvolt halos, including that of PSR J1849-0001, have luminosities at 50 TeV (estimated from the differential fluxes) approximately proportional to the spin-down energy E ̇ of the pulsars, and the ratios of the former to the latter are ∼6 × 10−4.

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Investigating γ -ray halos around three HAWC bright sources in Fermi -LAT data

Cited by 16 publications

References 62 publications

Constraining positron emission from pulsar populations with AMS-02 data

Constraining positron emission from pulsar populations with AMS-02 data

Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”

Two Candidate Pulsar TeV Halos Identified from Property-similarity Studies

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