{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:I2XABJYN4TBEJXRO3K5AK3F6MU","short_pith_number":"pith:I2XABJYN","schema_version":"1.0","canonical_sha256":"46ae00a70de4c244de2edaba056cbe65062982ff4ce2023083828a75933506ec","source":{"kind":"arxiv","id":"1101.3342","version":2},"attestation_state":"computed","paper":{"title":"The near-infrared broad emission line region of active galactic nuclei. II. The one-micron continuum","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"(2) Harvard-Smithsonian CfA, (3) University of Durham, (4) University of California Irvine, (5) Western Michigan University), Hermine Landt (1), Kirk T. Korista (5), Margarita Karovska (2) ((1) University of Melbourne, Martin Elvis (2), Martin J. Ward (3), Misty C. Bentz (4)","submitted_at":"2011-01-17T22:08:32Z","abstract_excerpt":"We use quasi-simultaneous near-infrared (near-IR) and optical spectroscopy from four observing runs to study the continuum around 1 micron in 23 well-known broad-emission line active galactic nuclei (AGN). We show that, after correcting the optical spectra for host galaxy light, the AGN continuum around this wavelength can be approximated by the sum of mainly two emission components, a hot dust blackbody and an accretion disc. The accretion disc spectrum appears to dominate the flux at ~1 micron, which allows us to derive a relation for estimating AGN black hole masses based on the near-IR vir"},"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":"1101.3342","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2011-01-17T22:08:32Z","cross_cats_sorted":[],"title_canon_sha256":"9b2b566ec76349d3e9c057a4f4fb96b459f724b1d4d7c2c90a2bf3fe069798be","abstract_canon_sha256":"80657d5bcbb9864b8144347d06e27872ed35ff8b6348c609197ca672acf580af"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:03:27.042340Z","signature_b64":"Y0E3Tzw2x/uQS/c7z3fiAGIYhr+LA3WLd+UlS/BijLcSMWYziQkVkHIQKWbf9JC+jqB/9WwjQW/jLjKN7dvgDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"46ae00a70de4c244de2edaba056cbe65062982ff4ce2023083828a75933506ec","last_reissued_at":"2026-05-18T02:03:27.041827Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:03:27.041827Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The near-infrared broad emission line region of active galactic nuclei. II. The one-micron continuum","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"(2) Harvard-Smithsonian CfA, (3) University of Durham, (4) University of California Irvine, (5) Western Michigan University), Hermine Landt (1), Kirk T. Korista (5), Margarita Karovska (2) ((1) University of Melbourne, Martin Elvis (2), Martin J. Ward (3), Misty C. Bentz (4)","submitted_at":"2011-01-17T22:08:32Z","abstract_excerpt":"We use quasi-simultaneous near-infrared (near-IR) and optical spectroscopy from four observing runs to study the continuum around 1 micron in 23 well-known broad-emission line active galactic nuclei (AGN). We show that, after correcting the optical spectra for host galaxy light, the AGN continuum around this wavelength can be approximated by the sum of mainly two emission components, a hot dust blackbody and an accretion disc. The accretion disc spectrum appears to dominate the flux at ~1 micron, which allows us to derive a relation for estimating AGN black hole masses based on the near-IR vir"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1101.3342","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":"1101.3342","created_at":"2026-05-18T02:03:27.041917+00:00"},{"alias_kind":"arxiv_version","alias_value":"1101.3342v2","created_at":"2026-05-18T02:03:27.041917+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1101.3342","created_at":"2026-05-18T02:03:27.041917+00:00"},{"alias_kind":"pith_short_12","alias_value":"I2XABJYN4TBE","created_at":"2026-05-18T12:26:30.835961+00:00"},{"alias_kind":"pith_short_16","alias_value":"I2XABJYN4TBEJXRO","created_at":"2026-05-18T12:26:30.835961+00:00"},{"alias_kind":"pith_short_8","alias_value":"I2XABJYN","created_at":"2026-05-18T12:26:30.835961+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/I2XABJYN4TBEJXRO3K5AK3F6MU","json":"https://pith.science/pith/I2XABJYN4TBEJXRO3K5AK3F6MU.json","graph_json":"https://pith.science/api/pith-number/I2XABJYN4TBEJXRO3K5AK3F6MU/graph.json","events_json":"https://pith.science/api/pith-number/I2XABJYN4TBEJXRO3K5AK3F6MU/events.json","paper":"https://pith.science/paper/I2XABJYN"},"agent_actions":{"view_html":"https://pith.science/pith/I2XABJYN4TBEJXRO3K5AK3F6MU","download_json":"https://pith.science/pith/I2XABJYN4TBEJXRO3K5AK3F6MU.json","view_paper":"https://pith.science/paper/I2XABJYN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1101.3342&json=true","fetch_graph":"https://pith.science/api/pith-number/I2XABJYN4TBEJXRO3K5AK3F6MU/graph.json","fetch_events":"https://pith.science/api/pith-number/I2XABJYN4TBEJXRO3K5AK3F6MU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/I2XABJYN4TBEJXRO3K5AK3F6MU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/I2XABJYN4TBEJXRO3K5AK3F6MU/action/storage_attestation","attest_author":"https://pith.science/pith/I2XABJYN4TBEJXRO3K5AK3F6MU/action/author_attestation","sign_citation":"https://pith.science/pith/I2XABJYN4TBEJXRO3K5AK3F6MU/action/citation_signature","submit_replication":"https://pith.science/pith/I2XABJYN4TBEJXRO3K5AK3F6MU/action/replication_record"}},"created_at":"2026-05-18T02:03:27.041917+00:00","updated_at":"2026-05-18T02:03:27.041917+00:00"}