{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:6S6YP24GYXWVEL3RHD6OGRWXUB","short_pith_number":"pith:6S6YP24G","schema_version":"1.0","canonical_sha256":"f4bd87eb86c5ed522f7138fce346d7a04e5b91dc55b4f4a96ed538d96040398e","source":{"kind":"arxiv","id":"0908.0018","version":1},"attestation_state":"computed","paper":{"title":"Imaging Atomic and Highly Excited Molecular Gas in a z=6.42 Quasar Host Galaxy: Copious Fuel for an Eddington-Limited Starburst at the End of Cosmic Reionization","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"2, 7), Axel Weiss (6), Christopher L. Carilli (4), Dominik A. Riechers (1, Fabian Walter (2), France; (6) MPIfR, Frank Bertoldi (3), Germany; (3) AIfA Bonn, Germany; (4) NRAO, Germany; (7) Hubble Fellow), Karl M. Menten (6) ((1) Caltech, Manuel Aravena (3), Pierre Cox (5), Roberto Neri (5), USA; (2) MPIA, USA; (5) IRAM","submitted_at":"2009-07-31T22:42:57Z","abstract_excerpt":"We have imaged CO(J=7-6) and CI(3P2-3P1) emission in the host galaxy of the z=6.42 quasar SDSS J114816.64+525150.3 (hereafter: J1148+5251) through observations with the Plateau de Bure Interferometer. The region showing CO(J=7-6) emission is spatially resolved, and its size of 5 kpc is in good agreement with earlier CO(J=3-2) observations. In combination with a revised model of the collisional line excitation in this source, this indicates that the highly excited molecular gas traced by the CO J=7-6 line is subthermally excited (showing only 58+/-8% of the CO J=3-2 luminosity), but not more ce"},"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":"0908.0018","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-07-31T22:42:57Z","cross_cats_sorted":[],"title_canon_sha256":"555d752da11608c904cb66a301fd7073d8413930a740cfe47fd0a22cbb3ac9eb","abstract_canon_sha256":"a670cad87035f63aecbeb0726fa486ac26a67251a4587885def18e96cc0d394d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:40:20.574727Z","signature_b64":"OnknPweR+429GWGwFFmEr/YHWmp+YrmpRx/+ndmpnaQ+uRPKQzOBRvZUQKeeXTk1+b5vju/adtv6CBm8L5LWDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f4bd87eb86c5ed522f7138fce346d7a04e5b91dc55b4f4a96ed538d96040398e","last_reissued_at":"2026-05-18T04:40:20.574188Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:40:20.574188Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Imaging Atomic and Highly Excited Molecular Gas in a z=6.42 Quasar Host Galaxy: Copious Fuel for an Eddington-Limited Starburst at the End of Cosmic Reionization","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"2, 7), Axel Weiss (6), Christopher L. Carilli (4), Dominik A. Riechers (1, Fabian Walter (2), France; (6) MPIfR, Frank Bertoldi (3), Germany; (3) AIfA Bonn, Germany; (4) NRAO, Germany; (7) Hubble Fellow), Karl M. Menten (6) ((1) Caltech, Manuel Aravena (3), Pierre Cox (5), Roberto Neri (5), USA; (2) MPIA, USA; (5) IRAM","submitted_at":"2009-07-31T22:42:57Z","abstract_excerpt":"We have imaged CO(J=7-6) and CI(3P2-3P1) emission in the host galaxy of the z=6.42 quasar SDSS J114816.64+525150.3 (hereafter: J1148+5251) through observations with the Plateau de Bure Interferometer. The region showing CO(J=7-6) emission is spatially resolved, and its size of 5 kpc is in good agreement with earlier CO(J=3-2) observations. In combination with a revised model of the collisional line excitation in this source, this indicates that the highly excited molecular gas traced by the CO J=7-6 line is subthermally excited (showing only 58+/-8% of the CO J=3-2 luminosity), but not more ce"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0908.0018","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":"0908.0018","created_at":"2026-05-18T04:40:20.574266+00:00"},{"alias_kind":"arxiv_version","alias_value":"0908.0018v1","created_at":"2026-05-18T04:40:20.574266+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0908.0018","created_at":"2026-05-18T04:40:20.574266+00:00"},{"alias_kind":"pith_short_12","alias_value":"6S6YP24GYXWV","created_at":"2026-05-18T12:25:58.837520+00:00"},{"alias_kind":"pith_short_16","alias_value":"6S6YP24GYXWVEL3R","created_at":"2026-05-18T12:25:58.837520+00:00"},{"alias_kind":"pith_short_8","alias_value":"6S6YP24G","created_at":"2026-05-18T12:25:58.837520+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/6S6YP24GYXWVEL3RHD6OGRWXUB","json":"https://pith.science/pith/6S6YP24GYXWVEL3RHD6OGRWXUB.json","graph_json":"https://pith.science/api/pith-number/6S6YP24GYXWVEL3RHD6OGRWXUB/graph.json","events_json":"https://pith.science/api/pith-number/6S6YP24GYXWVEL3RHD6OGRWXUB/events.json","paper":"https://pith.science/paper/6S6YP24G"},"agent_actions":{"view_html":"https://pith.science/pith/6S6YP24GYXWVEL3RHD6OGRWXUB","download_json":"https://pith.science/pith/6S6YP24GYXWVEL3RHD6OGRWXUB.json","view_paper":"https://pith.science/paper/6S6YP24G","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0908.0018&json=true","fetch_graph":"https://pith.science/api/pith-number/6S6YP24GYXWVEL3RHD6OGRWXUB/graph.json","fetch_events":"https://pith.science/api/pith-number/6S6YP24GYXWVEL3RHD6OGRWXUB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6S6YP24GYXWVEL3RHD6OGRWXUB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6S6YP24GYXWVEL3RHD6OGRWXUB/action/storage_attestation","attest_author":"https://pith.science/pith/6S6YP24GYXWVEL3RHD6OGRWXUB/action/author_attestation","sign_citation":"https://pith.science/pith/6S6YP24GYXWVEL3RHD6OGRWXUB/action/citation_signature","submit_replication":"https://pith.science/pith/6S6YP24GYXWVEL3RHD6OGRWXUB/action/replication_record"}},"created_at":"2026-05-18T04:40:20.574266+00:00","updated_at":"2026-05-18T04:40:20.574266+00:00"}