{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:XYYDA53IRRPEALHV6PQLZ6UVBK","short_pith_number":"pith:XYYDA53I","schema_version":"1.0","canonical_sha256":"be303077688c5e402cf5f3e0bcfa950a99ca9fb20d34d34f2544e71a541ed689","source":{"kind":"arxiv","id":"1807.10669","version":1},"attestation_state":"computed","paper":{"title":"Flux Density Variations at 3.6 cm in the Massive Star-Forming Region W49A","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"B. Presler-Marshall, C. G. De Pree, D. Wilner, J. Bates, M.-M. Mac Low, R. Galv\\'an-Madrid, R. S. Klessen, R. Webb-Forgus, T. Melo, T. Peters, W. M. Goss","submitted_at":"2018-07-27T15:07:19Z","abstract_excerpt":"A number of ultracompact H II regions in Galactic star forming environments have been observed to vary significantly in radio flux density on timescales of 10-20 years. Theory predicted that such variations should occur when the accretion flow that feeds a young massive star becomes unstable and clumpy. We have targeted the massive star-forming region W49A with the Karl G. Jansky Very Large Array (VLA) for observations at 3.6 cm with the B-configuration at 0.8'' resolution, to compare to nearly identical observations taken almost 21 years earlier (February 2015 and August 1994). Most of the so"},"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":"1807.10669","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-07-27T15:07:19Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"a78e41c611299eabbc2a6fe4dc577a51c66812ee72b470fa2ee415080de9fe17","abstract_canon_sha256":"6e10389921e2381a3692d09bd7dc571ea49522cfc742287199cadfed1ea8620a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:08:05.795313Z","signature_b64":"z8FoEqLLYRryKtOPdHRbJUl1cmA4BN+nn0ojwpKo0LwYAPUpUFhUPVvtAwrWBEruW22Sh1aUnGr31bpDfqHQCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"be303077688c5e402cf5f3e0bcfa950a99ca9fb20d34d34f2544e71a541ed689","last_reissued_at":"2026-05-18T00:08:05.794879Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:08:05.794879Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Flux Density Variations at 3.6 cm in the Massive Star-Forming Region W49A","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"B. Presler-Marshall, C. G. De Pree, D. Wilner, J. Bates, M.-M. Mac Low, R. Galv\\'an-Madrid, R. S. Klessen, R. Webb-Forgus, T. Melo, T. Peters, W. M. Goss","submitted_at":"2018-07-27T15:07:19Z","abstract_excerpt":"A number of ultracompact H II regions in Galactic star forming environments have been observed to vary significantly in radio flux density on timescales of 10-20 years. Theory predicted that such variations should occur when the accretion flow that feeds a young massive star becomes unstable and clumpy. We have targeted the massive star-forming region W49A with the Karl G. Jansky Very Large Array (VLA) for observations at 3.6 cm with the B-configuration at 0.8'' resolution, to compare to nearly identical observations taken almost 21 years earlier (February 2015 and August 1994). Most of the so"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1807.10669","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"},"aliases":[{"alias_kind":"arxiv","alias_value":"1807.10669","created_at":"2026-05-18T00:08:05.794943+00:00"},{"alias_kind":"arxiv_version","alias_value":"1807.10669v1","created_at":"2026-05-18T00:08:05.794943+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1807.10669","created_at":"2026-05-18T00:08:05.794943+00:00"},{"alias_kind":"pith_short_12","alias_value":"XYYDA53IRRPE","created_at":"2026-05-18T12:33:04.347982+00:00"},{"alias_kind":"pith_short_16","alias_value":"XYYDA53IRRPEALHV","created_at":"2026-05-18T12:33:04.347982+00:00"},{"alias_kind":"pith_short_8","alias_value":"XYYDA53I","created_at":"2026-05-18T12:33:04.347982+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/XYYDA53IRRPEALHV6PQLZ6UVBK","json":"https://pith.science/pith/XYYDA53IRRPEALHV6PQLZ6UVBK.json","graph_json":"https://pith.science/api/pith-number/XYYDA53IRRPEALHV6PQLZ6UVBK/graph.json","events_json":"https://pith.science/api/pith-number/XYYDA53IRRPEALHV6PQLZ6UVBK/events.json","paper":"https://pith.science/paper/XYYDA53I"},"agent_actions":{"view_html":"https://pith.science/pith/XYYDA53IRRPEALHV6PQLZ6UVBK","download_json":"https://pith.science/pith/XYYDA53IRRPEALHV6PQLZ6UVBK.json","view_paper":"https://pith.science/paper/XYYDA53I","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1807.10669&json=true","fetch_graph":"https://pith.science/api/pith-number/XYYDA53IRRPEALHV6PQLZ6UVBK/graph.json","fetch_events":"https://pith.science/api/pith-number/XYYDA53IRRPEALHV6PQLZ6UVBK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XYYDA53IRRPEALHV6PQLZ6UVBK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XYYDA53IRRPEALHV6PQLZ6UVBK/action/storage_attestation","attest_author":"https://pith.science/pith/XYYDA53IRRPEALHV6PQLZ6UVBK/action/author_attestation","sign_citation":"https://pith.science/pith/XYYDA53IRRPEALHV6PQLZ6UVBK/action/citation_signature","submit_replication":"https://pith.science/pith/XYYDA53IRRPEALHV6PQLZ6UVBK/action/replication_record"}},"created_at":"2026-05-18T00:08:05.794943+00:00","updated_at":"2026-05-18T00:08:05.794943+00:00"}