Present status of the 7–10 m telescope of CANGAROO II

Yoshikoshi, T.; Dazeley, S.; Gunji, Shuichi; Hara, Shinji; Hara, T.; Holder, J.; Jimbo, J.; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Bohec, S. Le; Matsubara, Y.; Mizumoto, Y.; Mori, M.; Moriya, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Nishijima, K.; Patterson, J. R.; Roberts, M.; Rowell, G.; Sakurazawa, K.; Susukita, R.; Tamura, T.; Tanimori, T.; Yanagita, S.; Yoshida, Tatsuo; Akizuki, Yuki

doi:10.1016/s0927-6505(99)00063-8

Cited by 8 publications

(5 citation statements)

References 1 publication

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“…In calculating the inverse Compton emission spectra we optimistically assume that none of the wind momentum is carried by ions and that the wind is not terminated via pressure balance with the companion star outflow. The results indicate that if the initial Lorentz factor of the wind is in the range 10 6 −10 7 the inverse Compton emission from the unshocked wind at epochs near periastron could be as much as a factor of 100−1000 above the sensitivity threshold of the new CANGAROO II imaging Cerenkov detector [Yoshikoshi et al 1999] which should be operational before the end of 1999. If the pulsar wind is slower, the inverse Compton emission should be detectable by the GLAST observatory at energies in the range 20 MeV-300 GeV if γ w (0) ∼ 10 4 − 10 5 , or by the INTEGRAL project at energies up to 10 MeV if γ w (0) ∼ 10 3 .…”

Section: Discussionmentioning

confidence: 99%

Probing pulsar winds using inverse Compton scattering

Ball

Kirk

2000

Astroparticle Physics

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We investigate the effects of inverse Compton scattering by electrons and positrons in the unshocked winds of rotationally-powered binary pulsars. This process can scatter low energy target photons to produce gamma rays with energies from MeV to TeV. The binary radio pulsars PSR B1259−63 and PSR J0045−73 are both in close eccentric orbits around bright main sequence stars which provide a huge density of low energy target photons. The inverse Compton scattering process transfers momentum from the pulsar wind to the scattered photons, and therefore provides a drag which tends to decelerate the pulsar wind. We present detailed calculations of the dynamics of a pulsar wind which is undergoing inverse Compton scattering, showing that the deceleration of the wind of PSR B1259−63 due to 'inverse Compton drag' is small, but that this process may confine the wind of PSR J0045−73 before it attains pressure balance with the outflow of its companion star. We calculate the spectra and light curves of the resulting inverse Compton emission from PSR B1259−63 and show that if the size of the pulsar wind nebula is comparable to the binary separation, then the γ-ray emission from the unshocked wind may be detectable by atmospheric Cerenkov detectors or by the new generation of satellite-borne γ-ray detectors such as INTEGRAL and GLAST. This mechanism may therefore provide a direct probe of the freely-expanding regions of pulsar winds, previously thought to be invisible.

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Section: Discussionmentioning

confidence: 99%

Probing pulsar winds using inverse Compton scattering

Ball

Kirk

2000

Astroparticle Physics

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“…The CANGAROO-III instrument [30] is a four telescope system continuing the CANGAROO project [31,32] on a site near Woomera, Australia. The array of 3 new 10 m diameter telescopes was completed in 2004.…”

Section: Current Instrumentsmentioning

confidence: 99%

Ground-based gamma-ray astronomy with Cherenkov telescopes

Hinton

2009

New J. Phys.

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Very-high-energy (>100 GeV) γ-ray astronomy is emerging as an important discipline in both high energy astrophysics and astro-particle physics. This field is currently dominated by Imaging Atmospheric-Cherenkov Telescopes (IACTs) and arrays of these telescopes. Such arrays have achieved the best angular resolution and energy flux sensitivity in the γ-ray domain and are still far from the fundamental limits of the technique. Here I will summarise some key aspects of this technique and go on to review the current status of the major instruments and to highlight selected recent results.

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“…The best opportunity for detecting such emission in the near future is afforded by the new CANGAROO II imaging Cherenkov telescope located in Australia [Yoshikoshi et al 1999]. When the present lack of operational γ-ray telescopes is relieved by the launch of the GLAST and INTE-GRAL observatories, inverse Compton emission from this pulsar system may well be detectable at lower energies in the MeV-GeV range.…”

Section: Discussionmentioning

confidence: 99%

Shock Geometry and Inverse Compton Emission from the Wind of a Binary Pulsar

Ball

Dodd

2001

Publ. – Astron. Soc. Aust

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PSR B1259 – 63 is a 47 ms radio pulsar with a high spin-down luminosity which is in a close, highly eccentric 3·5 yr orbit about a bright stellar companion. The binary system may be a detectable source of hard ã γ-rays produced by inverse Compton scattering of photons from the B2e star SS2883 by electrons and positrons in the pulsar wind. The star provides an enormous density of optical photons in the vicinity of the pulsar, particularly at epochs near periastron. We calculate the emission from the unshocked region of the pulsar wind, assuming that it terminates at a shock where it attains pressure balance with the companion’s wind. The spectra and light curves for the inverse Compton emission from the shock-terminated wind are compared with those for an unterminated wind. If the pulsar’s wind is weaker than that from the companion star, the termination of the wind decreases the inverse Compton flux, particularly near periastron. The termination shock geometry has the effect of decreasing the asymmetry of the γ-ray light curve around periastron, which arises because of the asymmetrical variation of the scattering angle.

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Present status of the 7–10 m telescope of CANGAROO II

Cited by 8 publications

References 1 publication

Probing pulsar winds using inverse Compton scattering

Probing pulsar winds using inverse Compton scattering

Ground-based gamma-ray astronomy with Cherenkov telescopes

Shock Geometry and Inverse Compton Emission from the Wind of a Binary Pulsar

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