Observations of cosmic TeV γ-rays in the southern sky by means of stereoscopic and timing analyses of Cherenkov light.

Details Observations of cosmic TeV γ-rays in the southern sky by means of stereoscopic and timing analyses of Cherenkov light. Observations of cosmic TeV γ-rays in the southern sky by means of stereoscopic and timing analyses of Cherenkov light.

Mar 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mmkyo..40r...1s&link_type=abstract

Memoirs of the Faculty of Sciences University of Kyoto Ser. Phys., Astrophys., Geophys., Chem., Vol. 40, No. 2, p. 1 - 51

Astronomy and Astrophysics

Astrophysics

Pulsars: Gamma Rays, Gamma-Ray Sources: Ultrahigh Energy, Radio Galaxies: Gamma Rays

Scientific paper

A search for TeV γ-rays from the pulsars PSR B1706-44 and PSR B1055-52 and from the radio galaxy Centaurus A were made as a project of the CANGAROO collaboration with two atmospheric Cherenkov telescopes, the 3.8 m telescope and the BIGRAT, at Woomera, Australia in 1994 and 1995. Two images of Cherenkov light from one shower detected with the two telescopes equipped with different resolution cameras have been utilized in the stereoscopic analysis. In the timing analysis the arrival direction of the shower has been determined from the fact that the arrival time of a Cherenkov photon on the detector depends upon the direction of the photon. The improvement of S/N by using the stereoscopic analysis and timing analysis has been shown in the case of observational data of PSR B1706-44. TeV gamma rays from this pulsar have been detected with 4.9σ significance.The flux above the energy threshold of 2 TeV is found to be (1.3±0.4)×10-11 (E/TeV)-1.9 cm-2s-1, if the power-law index is assumed to be -2.9. From observations during 1992 to 1995, it is confirmed that PSR B1706-44 is a stable TeV gamma-ray emitter. There is no evidence for TeV gamma rays from PSR B1055-52. Similarly, there is no evidence for TeV gamma rays from Cen A. For this source, the upper limit for the flux above 2 TeV is 1.5×10-12 cm-2s-1.

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