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We use a Bayesian analysis to calculate a best-fit luminosity law, or dependence of L on P and \\dot{P}, including different methods for modeling the beaming factor. An outer gap (OG) magnetosphere geometry provides the best-fit model, which is L \\propto P^{-a} \\dot{P}^{b} where a=1.36\\pm0.03 and b=0.44\\pm0.02, similar to but not identical to the commonly assu"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1309.1982","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2013-09-08T17:33:49Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"4f5990915086528cb16446ae9d67dbbdc807a224bf55b0eff220d648295e7e5c","abstract_canon_sha256":"91d09551f2edacc77b92c0e43bc9a3c00a0801b763a8393784a584755c14f9a3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:47:48.669266Z","signature_b64":"WtQykOoZmWR4u+PljOutrT36Rm5voRdr8Xzw0/krv6iMb/xzhexrMqm0DwOPfnA5d1BzJnchank5zgcU6mzCBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"932ff3c1d3cc464ba5918335662f4d6cb382dc085b2f61ac74fe566fd474b4ff","last_reissued_at":"2026-05-18T01:47:48.668708Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:47:48.668708Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Modeling the non-recycled Fermi gamma-ray pulsar population","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"A. 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