{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:B6FTMIMD2CCIC7S6VRBMTP7WQO","short_pith_number":"pith:B6FTMIMD","schema_version":"1.0","canonical_sha256":"0f8b362183d084817e5eac42c9bff683bea335a02fa5f678a944b46ca90b0dc9","source":{"kind":"arxiv","id":"1104.3861","version":1},"attestation_state":"computed","paper":{"title":"A Population of X-ray Weak Quasars: PHL 1811 Analogs at High 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":"Dennis W. Just, Donald P. Schneider, Gordon T. Richards, Jianfeng Wu, Ohad Shemmer, Patrick B. Hall, Robert R. Gibson, Sarah J. Schmidt, W. N. Brandt","submitted_at":"2011-04-19T20:00:03Z","abstract_excerpt":"We report the results from Chandra and XMM-Newton observations of a sample of 10 type 1 quasars selected to have unusual UV emission-line properties (weak and blueshifted high-ionization lines; strong UV Fe emission) similar to those of PHL 1811, a confirmed intrinsically X-ray weak quasar. These quasars were identified by the Sloan Digital Sky Survey at high redshift (z~2.2); eight are radio quiet while two are radio intermediate. All of the radio-quiet PHL 1811 analogs are notably X-ray weak by a mean factor of ~13. These sources lack broad absorption lines and have blue UV/optical continua,"},"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":"1104.3861","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2011-04-19T20:00:03Z","cross_cats_sorted":["astro-ph.GA","astro-ph.HE"],"title_canon_sha256":"84ce8be43f53bf25ee6d76c6b8417c52e85d0053b801c72d098d5f55cd368002","abstract_canon_sha256":"4680a1122a2211b9a8657ebf4bdb442ce267bf00f6cbcc2e9ba957785c193236"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:20:11.217080Z","signature_b64":"emXycttjUwXT99Iwj3jJfeCvnAvqL9UoFs5wqGUTgvJrzn4d3fvfs/8kZA6ppQyvlIR3JaeryKxDewNRE9PvCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0f8b362183d084817e5eac42c9bff683bea335a02fa5f678a944b46ca90b0dc9","last_reissued_at":"2026-05-18T02:20:11.216584Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:20:11.216584Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Population of X-ray Weak Quasars: PHL 1811 Analogs at High 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":"Dennis W. Just, Donald P. Schneider, Gordon T. Richards, Jianfeng Wu, Ohad Shemmer, Patrick B. Hall, Robert R. Gibson, Sarah J. Schmidt, W. N. Brandt","submitted_at":"2011-04-19T20:00:03Z","abstract_excerpt":"We report the results from Chandra and XMM-Newton observations of a sample of 10 type 1 quasars selected to have unusual UV emission-line properties (weak and blueshifted high-ionization lines; strong UV Fe emission) similar to those of PHL 1811, a confirmed intrinsically X-ray weak quasar. These quasars were identified by the Sloan Digital Sky Survey at high redshift (z~2.2); eight are radio quiet while two are radio intermediate. All of the radio-quiet PHL 1811 analogs are notably X-ray weak by a mean factor of ~13. These sources lack broad absorption lines and have blue UV/optical continua,"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1104.3861","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":"1104.3861","created_at":"2026-05-18T02:20:11.216663+00:00"},{"alias_kind":"arxiv_version","alias_value":"1104.3861v1","created_at":"2026-05-18T02:20:11.216663+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1104.3861","created_at":"2026-05-18T02:20:11.216663+00:00"},{"alias_kind":"pith_short_12","alias_value":"B6FTMIMD2CCI","created_at":"2026-05-18T12:26:24.575870+00:00"},{"alias_kind":"pith_short_16","alias_value":"B6FTMIMD2CCIC7S6","created_at":"2026-05-18T12:26:24.575870+00:00"},{"alias_kind":"pith_short_8","alias_value":"B6FTMIMD","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":"2605.22918","citing_title":"Strong X-ray Variability of I Zwicky 1: Obscuration from Clumpy Accretion-Disk Winds","ref_index":48,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/B6FTMIMD2CCIC7S6VRBMTP7WQO","json":"https://pith.science/pith/B6FTMIMD2CCIC7S6VRBMTP7WQO.json","graph_json":"https://pith.science/api/pith-number/B6FTMIMD2CCIC7S6VRBMTP7WQO/graph.json","events_json":"https://pith.science/api/pith-number/B6FTMIMD2CCIC7S6VRBMTP7WQO/events.json","paper":"https://pith.science/paper/B6FTMIMD"},"agent_actions":{"view_html":"https://pith.science/pith/B6FTMIMD2CCIC7S6VRBMTP7WQO","download_json":"https://pith.science/pith/B6FTMIMD2CCIC7S6VRBMTP7WQO.json","view_paper":"https://pith.science/paper/B6FTMIMD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1104.3861&json=true","fetch_graph":"https://pith.science/api/pith-number/B6FTMIMD2CCIC7S6VRBMTP7WQO/graph.json","fetch_events":"https://pith.science/api/pith-number/B6FTMIMD2CCIC7S6VRBMTP7WQO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/B6FTMIMD2CCIC7S6VRBMTP7WQO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/B6FTMIMD2CCIC7S6VRBMTP7WQO/action/storage_attestation","attest_author":"https://pith.science/pith/B6FTMIMD2CCIC7S6VRBMTP7WQO/action/author_attestation","sign_citation":"https://pith.science/pith/B6FTMIMD2CCIC7S6VRBMTP7WQO/action/citation_signature","submit_replication":"https://pith.science/pith/B6FTMIMD2CCIC7S6VRBMTP7WQO/action/replication_record"}},"created_at":"2026-05-18T02:20:11.216663+00:00","updated_at":"2026-05-18T02:20:11.216663+00:00"}