Association of the 6-ms pulsar PSR1953 with the COS-B γ-ray source 2CG065

A systematic search for fast radio pulsars in the error boxes of the low energy γ-ray sources detected by the COS-B collaboration led to the discovery¹ of a 6.1-ms radio pulsar PSR1953 + 29 in a binary system with orbital period of 120+/-4 days inside the error box of 2CG065 + 0. It was not possible to associate unambiguously the two objects without either a precise position for the γ-ray source or the detection of 6.1-ms pulsed γ rays. Following the determination of a more accurate orbital ephemeris for the radio pulsar, we have examined our data for evidence for pulsed TeV γ rays. Here, we report the detection of such γ rays with the characteristic 6.1-ms periodicity of the radio pulsar. The γ rays were detected using the ground-based atmospheric Cerenkov technique at the University of Durham γ-ray facility at Dugway, Utah². This result, significant at the 5.4σ level, provides evidence for the association of the 6-ms radio pulsar PSR1953 + 29 with the γ-ray source 2CG065 + 0.