{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:B7UNGYI35NERNXDLZX7ICFJDLI","short_pith_number":"pith:B7UNGYI3","schema_version":"1.0","canonical_sha256":"0fe8d3611beb4916dc6bcdfe8115235a1c2c2b3e480cd10f734dc9c43b230f99","source":{"kind":"arxiv","id":"1112.2228","version":1},"attestation_state":"computed","paper":{"title":"X-ray and Multiwavelength Insights into the Nature of Weak Emission-Line Quasars at Low Redshift","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"Aleksandar M. Diamond-Stanic, Donald P. Schneider, Jianfeng Wu, Ohad Shemmer, Patrick B. Hall, Richard M. Plotkin, Scott F. Anderson, W. N. Brandt","submitted_at":"2011-12-09T22:50:06Z","abstract_excerpt":"(Abridged) We report on the X-ray and multiwavelength properties of 11 radio-quiet quasars with weak or no emission lines identified by the Sloan Digital Sky Survey (SDSS) with redshift z=0.4-2.5. The distribution of relative X-ray brightness for our low-redshift weak-line quasar (WLQ) candidates is significantly different from that of typical radio-quiet quasars, having an excess of X-ray weak sources, but it is consistent with that of high-redshift WLQs. The X-ray weak sources generally show similar UV emission-line properties to those of the X-ray weak quasar PHL 1811; they may belong to th"},"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":"1112.2228","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2011-12-09T22:50:06Z","cross_cats_sorted":["astro-ph.GA","astro-ph.HE"],"title_canon_sha256":"b45ae39f0af0f1c9b72d1719eb80501e60c2c42af767e6ebe925ad6b73c64a0f","abstract_canon_sha256":"a6baf1570b5249726d018785472c0b0f13b3b4f2633d2575b3d6a86f3808d973"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:20:11.112199Z","signature_b64":"0Cw4HssMt4hiGBKT5C+XskqoWmtJURWAfy9K8gV0HO5Evqnh6zoqoHWTytkfPqj5J3Wssaw12bFSZRWr7Q4OCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0fe8d3611beb4916dc6bcdfe8115235a1c2c2b3e480cd10f734dc9c43b230f99","last_reissued_at":"2026-05-18T02:20:11.111562Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:20:11.111562Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"X-ray and Multiwavelength Insights into the Nature of Weak Emission-Line Quasars at Low Redshift","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"Aleksandar M. Diamond-Stanic, Donald P. Schneider, Jianfeng Wu, Ohad Shemmer, Patrick B. Hall, Richard M. Plotkin, Scott F. Anderson, W. N. Brandt","submitted_at":"2011-12-09T22:50:06Z","abstract_excerpt":"(Abridged) We report on the X-ray and multiwavelength properties of 11 radio-quiet quasars with weak or no emission lines identified by the Sloan Digital Sky Survey (SDSS) with redshift z=0.4-2.5. The distribution of relative X-ray brightness for our low-redshift weak-line quasar (WLQ) candidates is significantly different from that of typical radio-quiet quasars, having an excess of X-ray weak sources, but it is consistent with that of high-redshift WLQs. The X-ray weak sources generally show similar UV emission-line properties to those of the X-ray weak quasar PHL 1811; they may belong to th"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1112.2228","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":"1112.2228","created_at":"2026-05-18T02:20:11.111654+00:00"},{"alias_kind":"arxiv_version","alias_value":"1112.2228v1","created_at":"2026-05-18T02:20:11.111654+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1112.2228","created_at":"2026-05-18T02:20:11.111654+00:00"},{"alias_kind":"pith_short_12","alias_value":"B7UNGYI35NER","created_at":"2026-05-18T12:26:24.575870+00:00"},{"alias_kind":"pith_short_16","alias_value":"B7UNGYI35NERNXDL","created_at":"2026-05-18T12:26:24.575870+00:00"},{"alias_kind":"pith_short_8","alias_value":"B7UNGYI3","created_at":"2026-05-18T12:26:24.575870+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.00992","citing_title":"Understanding the Broad-line Region of Active Galactic Nuclei with Photoionization. II. Slim disks, Self-shadowing, and BLR sizes","ref_index":45,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/B7UNGYI35NERNXDLZX7ICFJDLI","json":"https://pith.science/pith/B7UNGYI35NERNXDLZX7ICFJDLI.json","graph_json":"https://pith.science/api/pith-number/B7UNGYI35NERNXDLZX7ICFJDLI/graph.json","events_json":"https://pith.science/api/pith-number/B7UNGYI35NERNXDLZX7ICFJDLI/events.json","paper":"https://pith.science/paper/B7UNGYI3"},"agent_actions":{"view_html":"https://pith.science/pith/B7UNGYI35NERNXDLZX7ICFJDLI","download_json":"https://pith.science/pith/B7UNGYI35NERNXDLZX7ICFJDLI.json","view_paper":"https://pith.science/paper/B7UNGYI3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1112.2228&json=true","fetch_graph":"https://pith.science/api/pith-number/B7UNGYI35NERNXDLZX7ICFJDLI/graph.json","fetch_events":"https://pith.science/api/pith-number/B7UNGYI35NERNXDLZX7ICFJDLI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/B7UNGYI35NERNXDLZX7ICFJDLI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/B7UNGYI35NERNXDLZX7ICFJDLI/action/storage_attestation","attest_author":"https://pith.science/pith/B7UNGYI35NERNXDLZX7ICFJDLI/action/author_attestation","sign_citation":"https://pith.science/pith/B7UNGYI35NERNXDLZX7ICFJDLI/action/citation_signature","submit_replication":"https://pith.science/pith/B7UNGYI35NERNXDLZX7ICFJDLI/action/replication_record"}},"created_at":"2026-05-18T02:20:11.111654+00:00","updated_at":"2026-05-18T02:20:11.111654+00:00"}