Gamma-ray observations of the Crab Nebula at TeV energies

The Crab Nebula was observed in TeV gamma rays with the Whipple Observatory high-resolution atmospheric Cherenkov camera and a signal was detected at the 20 σ level. The energy spectrum derived has the form N(E) × dE = 2.5 × 10 -10 (E/0.4 TeV) -2.4±0.3 photons cm -2 s -1 TeV -1 between 0.4 and 4 TeV...

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Detalles Bibliográficos
Autores principales: Vacanti, G., Cawley, M.F., Colombo, E., Fegan, D.J., Hillas, A.M., Kwok, P.W., Lang, M.J., Lamb, R.C., Lewis, D.A., Macomb, D.J., O'Klaherty, K.S., Reynolds, P.T., Weekes, T.C.
Formato: JOUR
Materias:
Gamma rays: general
Nebulae: Crab Nebula
Pulsars
Radiation mechanisms
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_0004637X_v377_n2PART1_p467_Vacanti
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
Descripción
Sumario:The Crab Nebula was observed in TeV gamma rays with the Whipple Observatory high-resolution atmospheric Cherenkov camera and a signal was detected at the 20 σ level. The energy spectrum derived has the form N(E) × dE = 2.5 × 10 -10 (E/0.4 TeV) -2.4±0.3 photons cm -2 s -1 TeV -1 between 0.4 and 4 TeV. There is no evidence for the pulsar periodicity, and the flux is steady on a monthly time scale. If this signal is used to optimize the technique for gamma-ray detection, then a flux one-tenth that of the Crab can be detected at the 3 σ level in 60 hr of integration time. For an on-axis source the angular resolution is shown to be ±0°1.

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