{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:N7BAH4IMNGVTX4XB2UTXUTAJVI","short_pith_number":"pith:N7BAH4IM","schema_version":"1.0","canonical_sha256":"6fc203f10c69ab3bf2e1d5277a4c09aa118dca174dff3921af158ab8a9723f69","source":{"kind":"arxiv","id":"0911.1409","version":1},"attestation_state":"computed","paper":{"title":"CO J=3-2 Emission from the \"Water Fountain\" Sources IRAS 16342-3814 and IRAS 18286-0959","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"(2) National Astronomical Observatories/Yunnan Observatory, (3) Department of Physics, (4) ALMA Project Office, (5) Nobeyama Radio Observatory, (6) Department of Physics, Astronomy, Chinese Academy of Sciences, Engineering, Hiroshi Imai (1), Jin-Hua He (2), Jun-ichi Nakashima (3), Kagoshima University, National Astronomical Observatory of Japan, Nico Koning (6) ((1) Graduate School of Science, Nobuharu Ukita (4), Shuji Deguchi (5), University of Calgary), University of Hong Kong","submitted_at":"2009-11-07T11:47:41Z","abstract_excerpt":"We observed CO J=3-2 emission from the \"water fountain\" sources, which exhibit high-velocity collimated stellar jets traced by water maser emission, with the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope. We detected the CO emission from two sources, IRAS 16342-3814 and IRAS 18286-0959. The IRAS 16342-3814 CO emission exhibits a spectrum that is well fit to a Gaussian profile, rather than to a parabolic profile, with a velocity width (FWHM) of 158+/-6 km/s and an intensity peak at VLSR = 50+/-2 km/s. The mass loss rate of the star is estimated to be ~2.9x10^-5 M_sun/yr. Our "},"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":"0911.1409","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2009-11-07T11:47:41Z","cross_cats_sorted":[],"title_canon_sha256":"a6d8dbc29b4eebadf6ec1715380513b86bd3f4bbb6098d71029dce3bb36b2666","abstract_canon_sha256":"eb55c121280947b9331b9c66760cae7f15787f04cddeb55846de36012d0d594e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:10:58.417865Z","signature_b64":"8eoSCsSmcLJG2ibljoeet8K5czKImFnY8OiQbDMiyZwqcb3E+hnJYs6u6Y/LhkY+WCFepywQ9SQDycwQ4r9CBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6fc203f10c69ab3bf2e1d5277a4c09aa118dca174dff3921af158ab8a9723f69","last_reissued_at":"2026-05-18T02:10:58.417130Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:10:58.417130Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"CO J=3-2 Emission from the \"Water Fountain\" Sources IRAS 16342-3814 and IRAS 18286-0959","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"(2) National Astronomical Observatories/Yunnan Observatory, (3) Department of Physics, (4) ALMA Project Office, (5) Nobeyama Radio Observatory, (6) Department of Physics, Astronomy, Chinese Academy of Sciences, Engineering, Hiroshi Imai (1), Jin-Hua He (2), Jun-ichi Nakashima (3), Kagoshima University, National Astronomical Observatory of Japan, Nico Koning (6) ((1) Graduate School of Science, Nobuharu Ukita (4), Shuji Deguchi (5), University of Calgary), University of Hong Kong","submitted_at":"2009-11-07T11:47:41Z","abstract_excerpt":"We observed CO J=3-2 emission from the \"water fountain\" sources, which exhibit high-velocity collimated stellar jets traced by water maser emission, with the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope. We detected the CO emission from two sources, IRAS 16342-3814 and IRAS 18286-0959. The IRAS 16342-3814 CO emission exhibits a spectrum that is well fit to a Gaussian profile, rather than to a parabolic profile, with a velocity width (FWHM) of 158+/-6 km/s and an intensity peak at VLSR = 50+/-2 km/s. The mass loss rate of the star is estimated to be ~2.9x10^-5 M_sun/yr. Our "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0911.1409","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":"0911.1409","created_at":"2026-05-18T02:10:58.417241+00:00"},{"alias_kind":"arxiv_version","alias_value":"0911.1409v1","created_at":"2026-05-18T02:10:58.417241+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0911.1409","created_at":"2026-05-18T02:10:58.417241+00:00"},{"alias_kind":"pith_short_12","alias_value":"N7BAH4IMNGVT","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_16","alias_value":"N7BAH4IMNGVTX4XB","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_8","alias_value":"N7BAH4IM","created_at":"2026-05-18T12:26:00.592388+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/N7BAH4IMNGVTX4XB2UTXUTAJVI","json":"https://pith.science/pith/N7BAH4IMNGVTX4XB2UTXUTAJVI.json","graph_json":"https://pith.science/api/pith-number/N7BAH4IMNGVTX4XB2UTXUTAJVI/graph.json","events_json":"https://pith.science/api/pith-number/N7BAH4IMNGVTX4XB2UTXUTAJVI/events.json","paper":"https://pith.science/paper/N7BAH4IM"},"agent_actions":{"view_html":"https://pith.science/pith/N7BAH4IMNGVTX4XB2UTXUTAJVI","download_json":"https://pith.science/pith/N7BAH4IMNGVTX4XB2UTXUTAJVI.json","view_paper":"https://pith.science/paper/N7BAH4IM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0911.1409&json=true","fetch_graph":"https://pith.science/api/pith-number/N7BAH4IMNGVTX4XB2UTXUTAJVI/graph.json","fetch_events":"https://pith.science/api/pith-number/N7BAH4IMNGVTX4XB2UTXUTAJVI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/N7BAH4IMNGVTX4XB2UTXUTAJVI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/N7BAH4IMNGVTX4XB2UTXUTAJVI/action/storage_attestation","attest_author":"https://pith.science/pith/N7BAH4IMNGVTX4XB2UTXUTAJVI/action/author_attestation","sign_citation":"https://pith.science/pith/N7BAH4IMNGVTX4XB2UTXUTAJVI/action/citation_signature","submit_replication":"https://pith.science/pith/N7BAH4IMNGVTX4XB2UTXUTAJVI/action/replication_record"}},"created_at":"2026-05-18T02:10:58.417241+00:00","updated_at":"2026-05-18T02:10:58.417241+00:00"}