{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:MBBJ6AZ3RAVZDYOJBSKPI6FU2U","short_pith_number":"pith:MBBJ6AZ3","schema_version":"1.0","canonical_sha256":"60429f033b882b91e1c90c94f478b4d50c23f416b2559db70a2f7264ea8a1400","source":{"kind":"arxiv","id":"0704.2305","version":2},"attestation_state":"computed","paper":{"title":"c2d Spitzer IRS Spectra of Disks around T Tauri Stars. III. [Ne II], [Fe I], and H_2 gas-phase lines","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Ewine F. van Dishoeck, Fred Lahuis, Geoffrey A. Blake, Jacqueline E. Kessler-Silacci, Klaus M. Pontoppidan, Neal J. Evans II","submitted_at":"2007-04-18T09:49:43Z","abstract_excerpt":"We present a survey of mid-infrared gas-phase lines toward a sample of 76 circumstellar disks around low mass pre-main sequence stars from the Spitzer \"Cores to Disks\" legacy program. We report the first detections of [Ne II] and [Fe I] toward classical T Tauri stars in ~20% respectively ~9% of our sources. The observed [Ne II] line fluxes and upper limits are consistent with [Ne II] excitation in an X-ray irradiated disk around stars with X-ray luminosities L_X=10^{29}-10^{31} erg s^{-1}. [Fe I] is detected at ~10^-5-10^-4 L_Sun, but no [S I] or [Fe II] is detected down to ~10^{-6} L_Sun. The"},"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":"0704.2305","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-04-18T09:49:43Z","cross_cats_sorted":[],"title_canon_sha256":"133669216ca2777785f2b216098d32c17e81ed2dfd44c835dce5edbdc9a8a71e","abstract_canon_sha256":"6da5c58944a91538390c4bdc508a92ce97105f4c9e4af3d2de87883e572b3847"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:44:14.935539Z","signature_b64":"io7nCjVRWCtsDf6AzfEwuIiYxovl6+YpI5OzctSo63mfeJa157st+VT+8myTWWy4PEvsPrF3a9IlVGcpQyGNBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"60429f033b882b91e1c90c94f478b4d50c23f416b2559db70a2f7264ea8a1400","last_reissued_at":"2026-07-04T15:44:14.935172Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:44:14.935172Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"c2d Spitzer IRS Spectra of Disks around T Tauri Stars. III. [Ne II], [Fe I], and H_2 gas-phase lines","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Ewine F. van Dishoeck, Fred Lahuis, Geoffrey A. Blake, Jacqueline E. Kessler-Silacci, Klaus M. Pontoppidan, Neal J. Evans II","submitted_at":"2007-04-18T09:49:43Z","abstract_excerpt":"We present a survey of mid-infrared gas-phase lines toward a sample of 76 circumstellar disks around low mass pre-main sequence stars from the Spitzer \"Cores to Disks\" legacy program. We report the first detections of [Ne II] and [Fe I] toward classical T Tauri stars in ~20% respectively ~9% of our sources. The observed [Ne II] line fluxes and upper limits are consistent with [Ne II] excitation in an X-ray irradiated disk around stars with X-ray luminosities L_X=10^{29}-10^{31} erg s^{-1}. [Fe I] is detected at ~10^-5-10^-4 L_Sun, but no [S I] or [Fe II] is detected down to ~10^{-6} L_Sun. The"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0704.2305","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/0704.2305/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"0704.2305","created_at":"2026-07-04T15:44:14.935233+00:00"},{"alias_kind":"arxiv_version","alias_value":"0704.2305v2","created_at":"2026-07-04T15:44:14.935233+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0704.2305","created_at":"2026-07-04T15:44:14.935233+00:00"},{"alias_kind":"pith_short_12","alias_value":"MBBJ6AZ3RAVZ","created_at":"2026-07-04T15:44:14.935233+00:00"},{"alias_kind":"pith_short_16","alias_value":"MBBJ6AZ3RAVZDYOJ","created_at":"2026-07-04T15:44:14.935233+00:00"},{"alias_kind":"pith_short_8","alias_value":"MBBJ6AZ3","created_at":"2026-07-04T15:44:14.935233+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.27477","citing_title":"From Young to Older Disks: JWST/MIRI Evidence for Fading Molecular Emission and Hints for Elevated C/O in Upper Scorpius","ref_index":130,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MBBJ6AZ3RAVZDYOJBSKPI6FU2U","json":"https://pith.science/pith/MBBJ6AZ3RAVZDYOJBSKPI6FU2U.json","graph_json":"https://pith.science/api/pith-number/MBBJ6AZ3RAVZDYOJBSKPI6FU2U/graph.json","events_json":"https://pith.science/api/pith-number/MBBJ6AZ3RAVZDYOJBSKPI6FU2U/events.json","paper":"https://pith.science/paper/MBBJ6AZ3"},"agent_actions":{"view_html":"https://pith.science/pith/MBBJ6AZ3RAVZDYOJBSKPI6FU2U","download_json":"https://pith.science/pith/MBBJ6AZ3RAVZDYOJBSKPI6FU2U.json","view_paper":"https://pith.science/paper/MBBJ6AZ3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0704.2305&json=true","fetch_graph":"https://pith.science/api/pith-number/MBBJ6AZ3RAVZDYOJBSKPI6FU2U/graph.json","fetch_events":"https://pith.science/api/pith-number/MBBJ6AZ3RAVZDYOJBSKPI6FU2U/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MBBJ6AZ3RAVZDYOJBSKPI6FU2U/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MBBJ6AZ3RAVZDYOJBSKPI6FU2U/action/storage_attestation","attest_author":"https://pith.science/pith/MBBJ6AZ3RAVZDYOJBSKPI6FU2U/action/author_attestation","sign_citation":"https://pith.science/pith/MBBJ6AZ3RAVZDYOJBSKPI6FU2U/action/citation_signature","submit_replication":"https://pith.science/pith/MBBJ6AZ3RAVZDYOJBSKPI6FU2U/action/replication_record"}},"created_at":"2026-07-04T15:44:14.935233+00:00","updated_at":"2026-07-04T15:44:14.935233+00:00"}