{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2004:3AMYNKTZXUC5ZD6QI7HXMULPZ5","short_pith_number":"pith:3AMYNKTZ","schema_version":"1.0","canonical_sha256":"d81986aa79bd05dc8fd047cf76516fcf491c94ce449737bb09311d0c7df2e72c","source":{"kind":"arxiv","id":"astro-ph/0406349","version":1},"attestation_state":"computed","paper":{"title":"Parsec-scale X-ray Flows in High-mass Star-forming Regions","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"E. Feigelson, G. Garmire, K. Getman, L. Townsley, P. Broos, T. Montmerle, Y.-H. Chu","submitted_at":"2004-06-15T16:47:37Z","abstract_excerpt":"We present Chandra/ACIS images of several high-mass star-forming regions. The massive stellar clusters powering these HII regions are resolved at the arcsecond level into hundreds of stellar sources, similar to those seen in closer young stellar clusters. However, we also detect diffuse X-ray emission on parsec scales that is spatially and spectrally distinct from the point source population. For nearby regions (e.g. M17 and Rosette) the emission is soft, with plasma temperatures less than 10 million degrees, in contrast to what is seen in more distant complexes (e.g. RCW49, W51).\n  This exten"},"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":"astro-ph/0406349","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2004-06-15T16:47:37Z","cross_cats_sorted":[],"title_canon_sha256":"2b4e924d4fde140bacafa76bf621ef7896f1315e60391f82a91982ea06cbdfb7","abstract_canon_sha256":"9a09d818b24da753c16dc78b1907a3798bd04a81189d20aa80f99b71989ffa0b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T14:13:31.715458Z","signature_b64":"B6MkL0+insRcQp/vIELuDxR7jva5dYlNxZJBEi0Zccq+02DdG47sx0s8Ko26lXqB0qGcONICtleaFTuZc/GWBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d81986aa79bd05dc8fd047cf76516fcf491c94ce449737bb09311d0c7df2e72c","last_reissued_at":"2026-07-04T14:13:31.715030Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T14:13:31.715030Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Parsec-scale X-ray Flows in High-mass Star-forming Regions","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"E. Feigelson, G. Garmire, K. Getman, L. Townsley, P. Broos, T. Montmerle, Y.-H. Chu","submitted_at":"2004-06-15T16:47:37Z","abstract_excerpt":"We present Chandra/ACIS images of several high-mass star-forming regions. The massive stellar clusters powering these HII regions are resolved at the arcsecond level into hundreds of stellar sources, similar to those seen in closer young stellar clusters. However, we also detect diffuse X-ray emission on parsec scales that is spatially and spectrally distinct from the point source population. For nearby regions (e.g. M17 and Rosette) the emission is soft, with plasma temperatures less than 10 million degrees, in contrast to what is seen in more distant complexes (e.g. RCW49, W51).\n  This exten"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0406349","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0406349/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":"astro-ph/0406349","created_at":"2026-07-04T14:13:31.715087+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0406349v1","created_at":"2026-07-04T14:13:31.715087+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0406349","created_at":"2026-07-04T14:13:31.715087+00:00"},{"alias_kind":"pith_short_12","alias_value":"3AMYNKTZXUC5","created_at":"2026-07-04T14:13:31.715087+00:00"},{"alias_kind":"pith_short_16","alias_value":"3AMYNKTZXUC5ZD6Q","created_at":"2026-07-04T14:13:31.715087+00:00"},{"alias_kind":"pith_short_8","alias_value":"3AMYNKTZ","created_at":"2026-07-04T14:13:31.715087+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/3AMYNKTZXUC5ZD6QI7HXMULPZ5","json":"https://pith.science/pith/3AMYNKTZXUC5ZD6QI7HXMULPZ5.json","graph_json":"https://pith.science/api/pith-number/3AMYNKTZXUC5ZD6QI7HXMULPZ5/graph.json","events_json":"https://pith.science/api/pith-number/3AMYNKTZXUC5ZD6QI7HXMULPZ5/events.json","paper":"https://pith.science/paper/3AMYNKTZ"},"agent_actions":{"view_html":"https://pith.science/pith/3AMYNKTZXUC5ZD6QI7HXMULPZ5","download_json":"https://pith.science/pith/3AMYNKTZXUC5ZD6QI7HXMULPZ5.json","view_paper":"https://pith.science/paper/3AMYNKTZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0406349&json=true","fetch_graph":"https://pith.science/api/pith-number/3AMYNKTZXUC5ZD6QI7HXMULPZ5/graph.json","fetch_events":"https://pith.science/api/pith-number/3AMYNKTZXUC5ZD6QI7HXMULPZ5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3AMYNKTZXUC5ZD6QI7HXMULPZ5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3AMYNKTZXUC5ZD6QI7HXMULPZ5/action/storage_attestation","attest_author":"https://pith.science/pith/3AMYNKTZXUC5ZD6QI7HXMULPZ5/action/author_attestation","sign_citation":"https://pith.science/pith/3AMYNKTZXUC5ZD6QI7HXMULPZ5/action/citation_signature","submit_replication":"https://pith.science/pith/3AMYNKTZXUC5ZD6QI7HXMULPZ5/action/replication_record"}},"created_at":"2026-07-04T14:13:31.715087+00:00","updated_at":"2026-07-04T14:13:31.715087+00:00"}