Search for point sources of ultrahigh energy<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>γ</mml:mi></mml:math>rays in the southern sky

Allen, William H.; Bond, I. A.; Budding, E.; Conway, M. J.; Daniel, A.; Fenton, K. B.; Fujii, Hirofumi; Fujii, Z.; Hayashida, N.; Hibino, K.; Honda, M.; Humble, J. E.; Kabe, S.; Kasahara, K.; Kifune, T.; Lythe, Grant; Masaike, A.; Matsubara, Y.; Mitsui, K.; Miura, Yoshio; Mori, M.; Muraki, Y.; Nagano, M.; Nakamura, Takashi; Nakamura, Masaki; Morris, Paula; Ogio, S.; Saito, T.; Sakata, M.; Sato, H.; Shimizu, Hideyuki; Spencer, M.; Storey, J. R.; Tanimori, T.; Teshima, M.; Torii, Shoji; Wadsworth, A.; Watase, Y.; Woodhams, Michael D.; Yamamoto, Y.; Yock, P. C. M.; Yuda, T.

doi:10.1103/physrevd.48.466

Cited by 8 publications

(2 citation statements)

References 40 publications

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“…PKS 2155−304 is an IDV source, which shows unusually strong X‐ray emission. It is known to show rapid X‐ray, optical and UV variability (Allen et al 1993). This is the only source that was included in our Survey purely for its interesting properties (it violates the flux density limit in our selection criteria).…”

Section: Discussionmentioning

confidence: 99%

The ATCA intraday variability survey of extragalactic radio sources

Kedziora-Chudczer

Jauncey

Wieringa

et al. 2001

Monthly Notices of the Royal Astronomical Society

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We present the results of an Australia Telescope Compact Array (ATCA) survey for intraday variability (IDV) of the total and polarized flux densities of 118 compact, flat‐spectrum, extragalactic radio sources from the Parkes 2.7‐GHz Survey. A total of 22 total flux density IDV sources were discovered and 15 sources were found to show IDV of their polarized flux density. We discuss the statistical properties of the IDV sources, including the distribution of source modulation indices, and the dependence of the variability amplitude on source spectral index and on Galactic position. We suggest interstellar scintillation (ISS) in the Galactic interstellar medium as the most likely mechanism for IDV. Even so, the inferred high brightness temperatures cannot be easily explained.

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Section: Discussionmentioning

confidence: 99%

The ATCA intraday variability survey of extragalactic radio sources

Kedziora-Chudczer

Jauncey

Wieringa

et al. 2001

Monthly Notices of the Royal Astronomical Society

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“…Young supernova remnants are probably sites of acceleration of particles to high energies and, as a result of interactions, also sources of high energy neutrinos and γ-rays [1][2][3][4][5][6]. Following the occurrence of SN1987A it was expected that high energy γ-rays would be detected from this object, but the observations have so far been negative [7][8][9][10][11][12][13][14]. Also, some models required the formation of a pulsar during the supernova (SN) explosion which has not yet been discovered.…”

Section: Introductionmentioning

confidence: 99%

Gamma-rays and neutrinos from very young supernova remnants

Protheroe

Bednarek

Luo

1998

Astroparticle Physics

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We consider the result of acceleration of heavy ions in the slot gap potential of a very young pulsar with a hot polar cap. Photodisintegration of the heavy ions in the radiation field of the polar cap and pulsar surface gives rise to a flux of energetic neutrons. Some fraction of these neutrons interact with target nuclei in the supernova shell to produce neutrino and gamma-ray signals which should be observable from very young supernova remnants in our galaxy for a range of pulsar parameters.

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Low Threshold Particle Arrays

Bernlöhr

1996

TeV Gamma-Ray Astrophysics

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While atmospheric Cherenkov telescopes have a small eld of view and a small duty fraction, arrays of particle detectors on ground have a 1 sr eld of view and a 100% duty fraction. On the other hand, particle detector arrays have a much higher energy threshold and an inferior hadron rejection as compared to Cherenkov telescopes. Low threshold particle detector arrays would have potential advantages over Cherenkov telescopes in the search for episodic or unexpected sources of gamma rays in the multi-TeV energy range. Ways to improve the threshold and hadron rejection of arrays are shown, based on existing technology for the timing method (with scintillator or water Cherenkov counters) and the tracking method (with tracking detectors). The performance that could be achieved is shown by examples for both methods. At mountain altitude (about 4000 m or above) an energy threshold close to 1 TeV could be achieved. For any signi cant reduction of the hadronic background by selecting muon-poor showers a muon detection area of at least 1000 m 2 is required, even for a compact array.

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Search for point sources of ultrahigh energyγrays in the southern sky

Cited by 8 publications

References 40 publications

The ATCA intraday variability survey of extragalactic radio sources

The ATCA intraday variability survey of extragalactic radio sources

Gamma-rays and neutrinos from very young supernova remnants

Low Threshold Particle Arrays

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