{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:M3Y42FQKJEXDIU4AA47JIBJRA2","short_pith_number":"pith:M3Y42FQK","schema_version":"1.0","canonical_sha256":"66f1cd160a492e345380073e94053106a3527e3f345ca3263cebee981385d53f","source":{"kind":"arxiv","id":"0802.1929","version":1},"attestation_state":"computed","paper":{"title":"Submillimeter Line Emission from LMC N159W: a Dense, Clumpy PDR in a Low Metallicity Environment","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Kawamura, C. Kramer, D. Rabanus, F. Bensch, F. Bertoldi, H. Jakob, H. Sasago, H. Yamamoto, J. L. Pineda, J. May, J. Stutzki, K. Fujishita, K. Jacobs, K. Sun, L. Bronfman, M. Aravena, M. Cubick, M. Hitschfeld, M. Miller, M. R\\\"ollig, M. Rubio, N. Honingh, N. Mizuno, N. Volgenau, P. M\\\"uller, R. Schieder, R. Simon, T. Onishi, U. Klein, U.U. Graf, V. Ossenkopf, Y. Fukui, Y. Mizuno","submitted_at":"2008-02-14T10:59:18Z","abstract_excerpt":"Star formation at earlier cosmological times takes place in an interstellar medium with low metallicity. The Large Magellanic Cloud (LMC) is ideally suited to study star formation in such an environment. The physical and chemical state of the ISM in a star forming environment can be constrained by observations of submm and FIR spectral lines of the main carbon carrying species, CO, CI and CII, which originate in the surface layers of molecular clouds illuminated by the UV radiation of the newly formed, young stars. We present high-angular resolution sub-millimeter observations in the N159W reg"},"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":"0802.1929","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2008-02-14T10:59:18Z","cross_cats_sorted":[],"title_canon_sha256":"01cde79445cd8b06f0108d4dc2048960c2dfb5dc53de11c81282207b134aa210","abstract_canon_sha256":"13d5fe854bdc63104d6d918a076e4e4de505506bb682036778c70344d1a0c0cf"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:09:18.533712Z","signature_b64":"yLDrRFEmEY/shFIxFUJEuiLh6gnXtPONInhX/LHqLbJv+zx1T0y4tAww7AK3/Ud+19jc2Y8KmZ3YZXrLYMQ/Aw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"66f1cd160a492e345380073e94053106a3527e3f345ca3263cebee981385d53f","last_reissued_at":"2026-07-04T17:09:18.533269Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:09:18.533269Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Submillimeter Line Emission from LMC N159W: a Dense, Clumpy PDR in a Low Metallicity Environment","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Kawamura, C. Kramer, D. Rabanus, F. Bensch, F. Bertoldi, H. Jakob, H. Sasago, H. Yamamoto, J. L. Pineda, J. May, J. Stutzki, K. Fujishita, K. Jacobs, K. Sun, L. Bronfman, M. Aravena, M. Cubick, M. Hitschfeld, M. Miller, M. R\\\"ollig, M. Rubio, N. Honingh, N. Mizuno, N. Volgenau, P. M\\\"uller, R. Schieder, R. Simon, T. Onishi, U. Klein, U.U. Graf, V. Ossenkopf, Y. Fukui, Y. Mizuno","submitted_at":"2008-02-14T10:59:18Z","abstract_excerpt":"Star formation at earlier cosmological times takes place in an interstellar medium with low metallicity. The Large Magellanic Cloud (LMC) is ideally suited to study star formation in such an environment. The physical and chemical state of the ISM in a star forming environment can be constrained by observations of submm and FIR spectral lines of the main carbon carrying species, CO, CI and CII, which originate in the surface layers of molecular clouds illuminated by the UV radiation of the newly formed, young stars. We present high-angular resolution sub-millimeter observations in the N159W reg"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0802.1929","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/0802.1929/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":"0802.1929","created_at":"2026-07-04T17:09:18.533340+00:00"},{"alias_kind":"arxiv_version","alias_value":"0802.1929v1","created_at":"2026-07-04T17:09:18.533340+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0802.1929","created_at":"2026-07-04T17:09:18.533340+00:00"},{"alias_kind":"pith_short_12","alias_value":"M3Y42FQKJEXD","created_at":"2026-07-04T17:09:18.533340+00:00"},{"alias_kind":"pith_short_16","alias_value":"M3Y42FQKJEXDIU4A","created_at":"2026-07-04T17:09:18.533340+00:00"},{"alias_kind":"pith_short_8","alias_value":"M3Y42FQK","created_at":"2026-07-04T17:09:18.533340+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/M3Y42FQKJEXDIU4AA47JIBJRA2","json":"https://pith.science/pith/M3Y42FQKJEXDIU4AA47JIBJRA2.json","graph_json":"https://pith.science/api/pith-number/M3Y42FQKJEXDIU4AA47JIBJRA2/graph.json","events_json":"https://pith.science/api/pith-number/M3Y42FQKJEXDIU4AA47JIBJRA2/events.json","paper":"https://pith.science/paper/M3Y42FQK"},"agent_actions":{"view_html":"https://pith.science/pith/M3Y42FQKJEXDIU4AA47JIBJRA2","download_json":"https://pith.science/pith/M3Y42FQKJEXDIU4AA47JIBJRA2.json","view_paper":"https://pith.science/paper/M3Y42FQK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0802.1929&json=true","fetch_graph":"https://pith.science/api/pith-number/M3Y42FQKJEXDIU4AA47JIBJRA2/graph.json","fetch_events":"https://pith.science/api/pith-number/M3Y42FQKJEXDIU4AA47JIBJRA2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/M3Y42FQKJEXDIU4AA47JIBJRA2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/M3Y42FQKJEXDIU4AA47JIBJRA2/action/storage_attestation","attest_author":"https://pith.science/pith/M3Y42FQKJEXDIU4AA47JIBJRA2/action/author_attestation","sign_citation":"https://pith.science/pith/M3Y42FQKJEXDIU4AA47JIBJRA2/action/citation_signature","submit_replication":"https://pith.science/pith/M3Y42FQKJEXDIU4AA47JIBJRA2/action/replication_record"}},"created_at":"2026-07-04T17:09:18.533340+00:00","updated_at":"2026-07-04T17:09:18.533340+00:00"}