{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:VF4YRS2MGDMPEY2KA5KODY3USE","short_pith_number":"pith:VF4YRS2M","schema_version":"1.0","canonical_sha256":"a97988cb4c30d8f2634a0754e1e3749138ffe63fd710ef62615bf6964945909d","source":{"kind":"arxiv","id":"1609.08449","version":2},"attestation_state":"computed","paper":{"title":"Photometric Variability of the Be Star Population","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"B. Scott Gaudi, Daniel J. Stevens, David J. James, J. E. Bjorkman, Jonathan Labadie-Bartz, Joseph E. Rodriguez, Joshua Pepper, Keivan G. Stassun, K. S. Bjorkman, Michael B. Lund, M. Virginia McSwain, Robert J. Siverd, Rudolf B. Kuhn, Thomas G. Beatty","submitted_at":"2016-09-27T13:55:00Z","abstract_excerpt":"Be stars have generally been characterized by the emission lines in their spectra, and especially the time variability of those spectroscopic features. They are known to also exhibit photometric variability at multiple timescales, but have not been broadly compared and analyzed by that behavior. We have taken advantage of the advent of wide-field, long-baseline, and high-cadence photometric surveys that search for transiting exoplanets to perform a comprehensive analysis of brightness variations among a large number of known Be stars. The photometric data comes from the KELT transit survey, wi"},"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":"1609.08449","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2016-09-27T13:55:00Z","cross_cats_sorted":[],"title_canon_sha256":"e20eaf35afd1f7b0b3f17fd9b818b020af986ef8098c494b0dd726dd7eefad52","abstract_canon_sha256":"e73831ee96f0dc073a80f92850aa70d80514a8d9f2645ed755a4e084a4256712"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:43:59.967050Z","signature_b64":"N4wyPwYm0AwnPNanffGj9NY9fdAYUsu+eBzkAt9RKWI97BmfNZmNTAvDNSmfFZ/9m3KTCHt38DYxndVCgezQDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a97988cb4c30d8f2634a0754e1e3749138ffe63fd710ef62615bf6964945909d","last_reissued_at":"2026-05-18T00:43:59.966461Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:43:59.966461Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Photometric Variability of the Be Star Population","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"B. Scott Gaudi, Daniel J. Stevens, David J. James, J. E. Bjorkman, Jonathan Labadie-Bartz, Joseph E. Rodriguez, Joshua Pepper, Keivan G. Stassun, K. S. Bjorkman, Michael B. Lund, M. Virginia McSwain, Robert J. Siverd, Rudolf B. Kuhn, Thomas G. Beatty","submitted_at":"2016-09-27T13:55:00Z","abstract_excerpt":"Be stars have generally been characterized by the emission lines in their spectra, and especially the time variability of those spectroscopic features. They are known to also exhibit photometric variability at multiple timescales, but have not been broadly compared and analyzed by that behavior. We have taken advantage of the advent of wide-field, long-baseline, and high-cadence photometric surveys that search for transiting exoplanets to perform a comprehensive analysis of brightness variations among a large number of known Be stars. The photometric data comes from the KELT transit survey, wi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1609.08449","kind":"arxiv","version":2},"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"},"aliases":[{"alias_kind":"arxiv","alias_value":"1609.08449","created_at":"2026-05-18T00:43:59.966546+00:00"},{"alias_kind":"arxiv_version","alias_value":"1609.08449v2","created_at":"2026-05-18T00:43:59.966546+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1609.08449","created_at":"2026-05-18T00:43:59.966546+00:00"},{"alias_kind":"pith_short_12","alias_value":"VF4YRS2MGDMP","created_at":"2026-05-18T12:30:48.956258+00:00"},{"alias_kind":"pith_short_16","alias_value":"VF4YRS2MGDMPEY2K","created_at":"2026-05-18T12:30:48.956258+00:00"},{"alias_kind":"pith_short_8","alias_value":"VF4YRS2M","created_at":"2026-05-18T12:30:48.956258+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VF4YRS2MGDMPEY2KA5KODY3USE","json":"https://pith.science/pith/VF4YRS2MGDMPEY2KA5KODY3USE.json","graph_json":"https://pith.science/api/pith-number/VF4YRS2MGDMPEY2KA5KODY3USE/graph.json","events_json":"https://pith.science/api/pith-number/VF4YRS2MGDMPEY2KA5KODY3USE/events.json","paper":"https://pith.science/paper/VF4YRS2M"},"agent_actions":{"view_html":"https://pith.science/pith/VF4YRS2MGDMPEY2KA5KODY3USE","download_json":"https://pith.science/pith/VF4YRS2MGDMPEY2KA5KODY3USE.json","view_paper":"https://pith.science/paper/VF4YRS2M","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1609.08449&json=true","fetch_graph":"https://pith.science/api/pith-number/VF4YRS2MGDMPEY2KA5KODY3USE/graph.json","fetch_events":"https://pith.science/api/pith-number/VF4YRS2MGDMPEY2KA5KODY3USE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VF4YRS2MGDMPEY2KA5KODY3USE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VF4YRS2MGDMPEY2KA5KODY3USE/action/storage_attestation","attest_author":"https://pith.science/pith/VF4YRS2MGDMPEY2KA5KODY3USE/action/author_attestation","sign_citation":"https://pith.science/pith/VF4YRS2MGDMPEY2KA5KODY3USE/action/citation_signature","submit_replication":"https://pith.science/pith/VF4YRS2MGDMPEY2KA5KODY3USE/action/replication_record"}},"created_at":"2026-05-18T00:43:59.966546+00:00","updated_at":"2026-05-18T00:43:59.966546+00:00"}