Very High Energy Gamma Rays from the Vela Pulsar Direction

Yoshikoshi, T.; Kifune, T.; Dazeley, S.; Edwards, Philip; Hara, T.; Hayami, Y.; Kakimoto, F.; Konishi, T.; Masaike, A.; Matsubara, Y.; Matsuoka, Taro; Mizumoto, Y.; Mori, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Nishijima, K.; Oda, S.; Ogio, S.; Ohsaki, T.; Patterson, J. R.; Roberts, M.; Rowell, G.; Sako, T.; Sakurazawa, K.; Susukita, R.; Suzuki, A.; Tamura, T.; Tanimori, T.; Thornton, G.; Yanagita, S.; Yoshida, Tatsuo

doi:10.1086/310874

Cited by 73 publications

(60 citation statements)

References 22 publications

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“…A region of extended γ-ray emission is detected, to the south of the pulsar position (previously reported by Khélifi et al (2005). This region was previously observed by the CANGAROO collaboration (Yoshikoshi et al 1997) and emission of VHE γ-rays was claimed from a source 0.13…”

Section: Introductionsupporting

confidence: 64%

First detection of a VHE gamma-ray spectral maximum from a cosmic source: HESS discovery of the Vela X nebula

Aharonian

Akhperjanian

Bazer‐Bachi

et al. 2006

A&A

185

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The Vela supernova remnant (SNR) is a complex region containing a number of sources of non-thermal radiation. The inner section of this SNR, within 2 degrees of the pulsar PSR B0833−45, has been observed by the HESS γ-ray atmospheric Cherenkov detector in 2004 and 2005. A strong signal is seen from an extended region to the south of the pulsar, within an integration region of radius 0.8• around the position (α = 08 h 35 m 00 s , δ = −45• 36 J2000.0). The excess coincides with a region of hard X-ray emission seen by the ROSAT and ASCA satellites. The observed energy spectrum of the source between 550 GeV and 65 TeV is well fit by a power law function with photon index Γ = 1.45 ± 0.09 stat ± 0.2 sys and an exponential cutoff at an energy of 13.8 ± 2.3 stat ± 4.1 sys TeV. The integral flux above 1 TeV is (1.28 ± 0.17 stat ± 0.38 sys ) × 10 −11 cm −2 s −1 . This result is the first clear measurement of a peak in the spectral energy distribution from a VHE γ-ray source, likely related to inverse Compton emission. A fit of an Inverse Compton model to the HESS spectral energy distribution gives a total energy in non-thermal electrons of ∼2 × 10 45 erg between 5 TeV and 100 TeV, assuming a distance of 290 parsec to the pulsar. The best fit electron power law index is 2.0, with a spectral break at 67 TeV.

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Section: Introductionsupporting

confidence: 64%

First detection of a VHE gamma-ray spectral maximum from a cosmic source: HESS discovery of the Vela X nebula

Aharonian

Akhperjanian

Bazer‐Bachi

et al. 2006

A&A

185

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“…None of the considered PWNe should be comparable in brightness to the Crab Nebula. significantly lower than earlier positive reports [3,4,5]. PSR 1951+32 [29], PSR J0205+6449 [30], or PSR B1823-13 [31].…”

Section: Discussioncontrasting

confidence: 56%

“…the Crab Nebula [2], the nebulae around the Vela pulsar [3], PSR 1706-44 [4,5], and PSR 1509-58 [6]. the Crab Nebula [2], the nebulae around the Vela pulsar [3], PSR 1706-44 [4,5], and PSR 1509-58 [6].…”

Section: Introductionmentioning

confidence: 99%

Gamma-rays from the Pulsar Wind Nebulae

Bednarek

Bartosik

2005

AIP Conference Proceedings

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We estimate the gamma-ray fluxes expected from the northern sky pulsar wind nebulae (PWNe) applying time dependent hadronic-leptonic radiation model for the high energy processes inside the PWNe. This model base on the hypothesis, proposed by Arons and collaborators[1], which postulate that heavy nuclei are efficiently accelerated in the vicinity of young pulsars. We calculate the equilibrium spectra of leptons and hadrons at an arbitrary time after the pulsar formation. From normalization of the calculated synchrotron spectrum to the observed spectrum at low energies, the expected TeV gamma-ray fluxes from a population of the PWNe are estimated and its possible detectability by the future TeV telescopes is discussed.

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“…However, as for pulsed TeV radiation, only the upper limits, as a rule, have been obtained (Akerlof et al 1993 ;Borione et al 1997 ;Srinivasan et al 1997 ;Yoshikoshi et al 1997 ;Sako et al 2000). If the VHE emission originates in the pulsar magnetosphere, a signiÐcant fraction of it can be expected to show pulsation.…”

Section: Introductionmentioning

confidence: 99%

Electrodynamic Structure of an Outer Gap Accelerator: Location of the Gap and the Gamma‐Ray Emission from the Crab Pulsar

Hirotani

Shibata

2001

ApJ

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We investigate a stationary pair-production cascade in the outer magnetosphere of a spinning neutron star. The charge depletion due to global Ñows of charged particles causes a large electric Ðeld along the magnetic Ðeld lines. Migratory electrons and/or positrons are accelerated by this Ðeld to radiate curvature gamma rays, some of which collide with the X-rays to materialize as pairs in the gap. The replenished charges partially screen the electric Ðeld, which is self-consistently solved together with the distribution functions of particles and gamma rays. If no current is injected at either of the boundaries of the accelerator, the gap is located around the conventional null surface, where the local Goldreich-Julian charge density vanishes. However, we Ðrst Ðnd that the gap position shifts outward (or inward) when particles are injected at the inner (or outer) boundary. Applying the theory to the Crab pulsar, we demonstrate that the pulsed TeV Ñux does not exceed the observational upper limit for moderate infrared photon density and that the gap should be located near to or outside of the conventional null surface so that the observed spectrum of pulsed GeV Ñuxes may be emitted via a curvature process. Some implications of the existence of a solution for a super Goldreich-Julian current are discussed.

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Very High Energy Gamma Rays from the Vela Pulsar Direction

Cited by 73 publications

References 22 publications

First detection of a VHE gamma-ray spectral maximum from a cosmic source: HESS discovery of the Vela X nebula

First detection of a VHE gamma-ray spectral maximum from a cosmic source: HESS discovery of the Vela X nebula

Gamma-rays from the Pulsar Wind Nebulae

Electrodynamic Structure of an Outer Gap Accelerator: Location of the Gap and the Gamma‐Ray Emission from the Crab Pulsar

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