{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:GYIK6SVQNFJVIQL27IV5XOBZYP","short_pith_number":"pith:GYIK6SVQ","schema_version":"1.0","canonical_sha256":"3610af4ab0695354417afa2bdbb839c3c08489eb87c27ba7ce9bb977812cedaa","source":{"kind":"arxiv","id":"1010.5129","version":1},"attestation_state":"computed","paper":{"title":"The Mid-Infrared High-Ionization Lines from Active Galactic Nuclei and Star-Forming Galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Aleksandar M. Diamond-Stanic, Almudena Alonso-Herrero, George H. Rieke, Miguel Pereira-Santaella","submitted_at":"2010-10-25T13:55:03Z","abstract_excerpt":"We used Spitzer/IRS spectroscopic data on 426 galaxies including quasars, Seyferts, LINER and HII galaxies to investigate the relationship among the mid-IR emission lines. There is a tight linear correlation between the [Ne V]14.3 um and 24.3 um (97.1 eV) and the [O IV]25.9 um (54.9 eV) high-ionization emission lines. The correlation also holds for these high-ionization emission lines and the [Ne III]15.56 um (41 eV) emission line, although only for active galaxies. We used these correlations to calculate the [Ne III] excess due to star formation in Seyfert galaxies. We also estimated the [O I"},"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":"1010.5129","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2010-10-25T13:55:03Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"85eb6f14b6ec79dcff406b97599b33766049b95ba3aeacada2360998e05f18e1","abstract_canon_sha256":"7968fda7efce39b52d61080f12bc4f4828cba5f8cbe220e2c92ed5790754910c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:04:58.870966Z","signature_b64":"QOJKT5aY4Rke46s9bi2L2VGQRA4Y0nSiqSKh7vSkEmIinlORzSEw+6/qETRKcROBqR59fY9Ww5+7p/sxxT3tBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3610af4ab0695354417afa2bdbb839c3c08489eb87c27ba7ce9bb977812cedaa","last_reissued_at":"2026-05-18T02:04:58.870506Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:04:58.870506Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Mid-Infrared High-Ionization Lines from Active Galactic Nuclei and Star-Forming Galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Aleksandar M. Diamond-Stanic, Almudena Alonso-Herrero, George H. Rieke, Miguel Pereira-Santaella","submitted_at":"2010-10-25T13:55:03Z","abstract_excerpt":"We used Spitzer/IRS spectroscopic data on 426 galaxies including quasars, Seyferts, LINER and HII galaxies to investigate the relationship among the mid-IR emission lines. There is a tight linear correlation between the [Ne V]14.3 um and 24.3 um (97.1 eV) and the [O IV]25.9 um (54.9 eV) high-ionization emission lines. The correlation also holds for these high-ionization emission lines and the [Ne III]15.56 um (41 eV) emission line, although only for active galaxies. We used these correlations to calculate the [Ne III] excess due to star formation in Seyfert galaxies. We also estimated the [O I"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1010.5129","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":"1010.5129","created_at":"2026-05-18T02:04:58.870576+00:00"},{"alias_kind":"arxiv_version","alias_value":"1010.5129v1","created_at":"2026-05-18T02:04:58.870576+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1010.5129","created_at":"2026-05-18T02:04:58.870576+00:00"},{"alias_kind":"pith_short_12","alias_value":"GYIK6SVQNFJV","created_at":"2026-05-18T12:26:07.630475+00:00"},{"alias_kind":"pith_short_16","alias_value":"GYIK6SVQNFJVIQL2","created_at":"2026-05-18T12:26:07.630475+00:00"},{"alias_kind":"pith_short_8","alias_value":"GYIK6SVQ","created_at":"2026-05-18T12:26:07.630475+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/GYIK6SVQNFJVIQL27IV5XOBZYP","json":"https://pith.science/pith/GYIK6SVQNFJVIQL27IV5XOBZYP.json","graph_json":"https://pith.science/api/pith-number/GYIK6SVQNFJVIQL27IV5XOBZYP/graph.json","events_json":"https://pith.science/api/pith-number/GYIK6SVQNFJVIQL27IV5XOBZYP/events.json","paper":"https://pith.science/paper/GYIK6SVQ"},"agent_actions":{"view_html":"https://pith.science/pith/GYIK6SVQNFJVIQL27IV5XOBZYP","download_json":"https://pith.science/pith/GYIK6SVQNFJVIQL27IV5XOBZYP.json","view_paper":"https://pith.science/paper/GYIK6SVQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1010.5129&json=true","fetch_graph":"https://pith.science/api/pith-number/GYIK6SVQNFJVIQL27IV5XOBZYP/graph.json","fetch_events":"https://pith.science/api/pith-number/GYIK6SVQNFJVIQL27IV5XOBZYP/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GYIK6SVQNFJVIQL27IV5XOBZYP/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GYIK6SVQNFJVIQL27IV5XOBZYP/action/storage_attestation","attest_author":"https://pith.science/pith/GYIK6SVQNFJVIQL27IV5XOBZYP/action/author_attestation","sign_citation":"https://pith.science/pith/GYIK6SVQNFJVIQL27IV5XOBZYP/action/citation_signature","submit_replication":"https://pith.science/pith/GYIK6SVQNFJVIQL27IV5XOBZYP/action/replication_record"}},"created_at":"2026-05-18T02:04:58.870576+00:00","updated_at":"2026-05-18T02:04:58.870576+00:00"}