Unidentified VHE γ-ray sources and evolved pulsar wind nebulae - A possible connection?

Mayer, M.; Brucker, J.; Holler, M.; Jung, I.; Valerius, K.; Stegmann, C.

doi:10.1063/1.4772267

Cited by 5 publications

(9 citation statements)

References 8 publications

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“…This magnetic field evolution is similar to the t −1.3 − t −2 behavior derived by Reynolds & Chevalier (1984) and the t −1.7 evolution of Gelfand et al (2009) during the initial expansion phase. The power-law evolution of the magnetic field is similar to that adopted by Zhang et al (2008), Lemiere et al (2009), Mayer et al (2012 for similarly aged PWNe.…”

Section: Discussionsupporting

confidence: 53%

Fermi-LAT constraints on the pulsar wind nebula nature of HESS J1857+026

Rousseau

Grondin

Etten

et al. 2012

A&A

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Context. Since its launch, the Fermi satellite has firmly identified 5 pulsar wind nebulae plus a large number of candidates, all powered by young and energetic pulsars. HESS J1857+026 is a spatially extended γ-ray source detected by H.E.S.S. and classified as a possible pulsar wind nebula candidate powered by PSR J1856+0245. Aims. We search for γ-ray pulsations from PSR J1856+0245 and explore the characteristics of its associated pulsar wind nebula. Methods. Using a rotational ephemeris obtained from the Lovell telescope at Jodrell Bank Observatory at 1.5 GHz, we phase-fold 36 months of γ-ray data acquired by the Large Area Telescope (LAT) aboard Fermi. We also perform a complete γ-ray spectral and morphological analysis. Results. No γ-ray pulsations were detected from PSR J1856+0245. However, significant emission is detected at a position coincident with the TeV source HESS J1857+026. The γ-ray spectrum is well described by a simple power-law with a spectral index of Γ = 1.53 ± 0.11 stat ± 0.55 syst and an energy flux of G(0.1-100 GeV) = (2.71 ± 0.52 stat ± 1.51 syst ) × 10 −11 erg cm −2 s −1 . The γ-ray luminosity is L γ PWN (0.1-100 GeV) = (2.5 ± 0.5 stat ± 1.5 syst ) × 10 35 d 9 kpc 2 erg s −1 , assuming a distance of 9 kpc. This implies a γ-ray efficiency of ∼5% forĖ = 4.6 × 10 36 erg s −1 , in the range expected for pulsar wind nebulae. Detailed multi-wavelength modeling provides new constraints on its pulsar wind nebula nature.

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Section: Discussionsupporting

confidence: 53%

Fermi-LAT constraints on the pulsar wind nebula nature of HESS J1857+026

Rousseau

Grondin

Etten

et al. 2012

A&A

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“…This means that the linear function improves the fit at only the 1σ level. This coefficient and this comparison show that, contrary to the expectation (Mayer et al 2012), no downward correlation is observed. However, this correlation might be obscured by the usage of the characteristic age of the pulsar, which may not be a good age estimator for the PWN.…”

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confidence: 65%

“…These figures show that the Fermi-LAT mainly detects young and middle-aged PWNe (1-30 kyr) around energetic pulsars with spin-down powers between 10 36 and 10 39 erg s −1 . One can see from these figures that the VHE sources older than 30 kyr are not detected by the LAT, while Mayer et al (2012) predict a higher flux in the LAT energy range than in the VHE experiments' energy range. However, it should be noted that among these nine VHE sources, at least seven suffer one or several biases.…”

Section: Table 11mentioning

confidence: 87%

“…We assumed that the emission measured in the TeV and GeV bands comes from the falling and rising edges, respectively, of the IC peak in the SED produced by the same population of electrons, and we studied the spectral shape of this IC peak. Mayer et al (2012) have shown that a negative correlation between the energy of the peak and the pulsar characteristic age would be expected from the evolution of the cooling time with energy. We attempted to find this relation starting from the LAT and VHE data.…”

Section: Discussionmentioning

confidence: 99%

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CONSTRAINTS ON THE GALACTIC POPULATION OF TeV PULSAR WIND NEBULAE USINGFERMILARGE AREA TELESCOPE OBSERVATIONS

Acero¹,

Ackermann²,

Ajello³

et al. 2013

ApJ

Self Cite

114

124

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Pulsar wind nebulae (PWNe) have been established as the most populous class of TeV γ-ray emitters. Since launch, the Fermi Large Area Telescope (LAT) has identified five high-energy (100 MeV < E < 100 GeV) γ-ray sources as PWNe and detected a large number of PWN candidates, all powered by young and energetic pulsars. The wealth of multi-wavelength data available and the new results provided by Fermi-LAT give us an opportunity to find new PWNe and to explore the radiative processes taking place in known ones. The TeV γ-ray unidentified (UNID) sources are the best candidates for finding new PWNe. Using 45 months of Fermi-LAT data for energies above 10 GeV, an analysis was performed near the position of 58 TeV PWNe and UNIDs within 5 • of the Galactic plane to establish new constraints on PWN properties and find new clues on the nature of UNIDs. Of the 58 sources, 30 were detected, and this work provides their γ-ray fluxes for energies above 10 GeV. The spectral energy distributions and upper limits, in the multi-wavelength context, also provide new information on the source nature and can help distinguish between emission scenarios, i.e., between classification as a pulsar candidate or as a PWN candidate. Six new GeV PWN candidates are described in detail and compared with existing models. A population study of GeV PWN candidates as a function of the pulsar/PWN system characteristics is presented.

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“…An estimate of the contribution to the measured diffuse emission from sources with lower fluxes would require a model of a full synthetic population of PWNe based on H.E.S.S. and Fermi data and on the current theories of PWN evolution (e.g., Bucciantini et al 2011;Mayer et al 2012;Torres et al 2014). This study is beyond the scope of the present paper.…”

Section: Treatment Of the Unresolved Sourcesmentioning

confidence: 99%

Study of the diffuse gamma ray emission from the Galactic plane with ARGO-YBJ

Ma¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The events recorded by ARGO-YBJ in more than fiveyears of data collection have been analyzed to determine the diffuse gamma-ray emission in the Galactic plane at Galactic longitudes 25°< l < 100°and Galactic latitudes b 5 | | <°. The energy range covered by this analysis, from ∼350 GeV to ∼2 TeV, allows the connection of the region explored by Fermi with the multi-TeV measurements carried out by Milagro. Our analysis has been focused on two selected regions of the Galactic plane, i.e., 40°< l < 100°and 65°< l < 85°(the Cygnus region), where Milagro observed an excess with respect to the predictions of current models. Great care has been taken in order to mask the most intense gamma-ray sources, including the TeV counterpart of the Cygnus cocoon recently identified by ARGO-YBJ, and to remove residual contributions. The ARGO-YBJ results do not show any excess at sub-TeV energies corresponding to the excess found by Milagro, and are consistent with the predictions of the Fermi model for the diffuse Galactic emission. From the measured energy distribution we derive spectral indices and the differential flux at 1 TeV of the diffuse gamma-ray emission in the sky regions investigated.

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Unidentified VHE γ-ray sources and evolved pulsar wind nebulae - A possible connection?

Cited by 5 publications

References 8 publications

Fermi-LAT constraints on the pulsar wind nebula nature of HESS J1857+026

Fermi-LAT constraints on the pulsar wind nebula nature of HESS J1857+026

CONSTRAINTS ON THE GALACTIC POPULATION OF TeV PULSAR WIND NEBULAE USINGFERMILARGE AREA TELESCOPE OBSERVATIONS

Study of the diffuse gamma ray emission from the Galactic plane with ARGO-YBJ

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