{"paper":{"title":"The SNR W28 at TeV Energies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Kawachi, G.J. Thornton, G.P. Rowell, H. Muraishi, J. Holder, J.R. Patterson, K. Nishijima, K. Sakurazawa, M.D. Roberts, M. Mori, P.G. Edwards, R. Susukita, S.A. Dazeley, S. Gunji, S. Ogio, S. Yanagita, T. Hara, T. Kifune, T. Naito, T. Sako, T. Tamura, T. Tanimori, T. Yoshida, T. Yoshikoshi, Y. Matsubara, Y. Mizumoto, Y. Muraki","submitted_at":"1999-11-30T06:08:07Z","abstract_excerpt":"The southern supernova remnant (SNR)W28 was observed in 1994 and 1995 by the CANGAROO 3.8m telescope in a search formulti-TeV gamma ray emission, using the Cerenkov imaging technique. We obtained upper limits for a variety of point-like and extended features within a +-1 degree-region and briefly discuss these results, together with that of EGRET within the framework of a shock acceleration model of the W28 SNR."},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9911511","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/9911511/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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"}