{"paper":{"title":"Very High Energy Gamma Rays from the Vela Pulsar Direction","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Masaike, A. Suzuki, F. Kakimoto, G. J. Thornton, G. P. Rowell, H. Muraishi, J. R. Patterson, K. Nishijima, K. Sakurazawa, M. D. Roberts, M. Mori, P. G. Edwards, R. Susukita, S. A. Dazeley, S. Oda, S. Ogio, S. Yanagita, T. Hara, T. Kifune, T. Konishi, T. Matsuoka, T. Naito, T. Ohsaki, T. Sako, T. Tamura, T. Tanimori, T. Yoshida, T. Yoshikoshi, Y. Hayami, Y. Matsubara, Y. Mizumoto, Y. Muraki","submitted_at":"1997-07-17T10:59:34Z","abstract_excerpt":"We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Cherenkov telescope near Woomera, South Australia between January 1993 and March 1995. Evidence of an unpulsed gamma-ray signal has been detected at the 5.8 sigma level. The detected gamma-ray flux is (2.9 +/- 0.5 +/- 0.4) x 10^-12 photons cm^-2 sec^-1 above 2.5 +/- 1.0 TeV and the signal is consistent with steady emission over the two years. The gamma-ray emission region is offset from the Vela pulsar position to the southeast by about 0.13 deg. No pulsed emission modulated with the pulsar period has been detected"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9707203","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}