{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:DYQEYEM6E3KJ46TY2UUF3JM6EA","short_pith_number":"pith:DYQEYEM6","schema_version":"1.0","canonical_sha256":"1e204c119e26d49e7a78d5285da59e202603472deb0f5f3b79e158e0deffee95","source":{"kind":"arxiv","id":"1103.5347","version":1},"attestation_state":"computed","paper":{"title":"TIMASSS: The IRAS16293-2422 Millimeter And Submillimeter Spectral Survey. I. Observations, calibration and analysis of the line kinematics","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Bacmann, A. Castets, A. Coutens, A.G.G.M. Tielens, A. Walters, B. Lefloch, B. Parise, C. Ceccarelli, C. Comito, C. Kahane, C. Vastel, E. Caux, E. van Dishoeck, F.P. Helmich, P. Schilke, S. Bisshop, S. Bottinelli, V. Wakelam","submitted_at":"2011-03-28T13:23:30Z","abstract_excerpt":"While unbiased surveys observable from ground-based telescopes have previously been obtained towards several high mass protostars, very little exists on low mass protostars. To fill up this gap, we carried out a complete spectral survey of the bands at 3, 2, 1 and 0.8 mm towards the solar type protostar IRAS16293-2422. The observations covered about 200\\,GHz and were obtained with the IRAM-30m and JCMT-15m telescopes. Particular attention was devoted to the inter-calibration of the obtained spectra with previous observations. All the lines detected with more than 3 sigma and free from obvious "},"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":"1103.5347","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2011-03-28T13:23:30Z","cross_cats_sorted":[],"title_canon_sha256":"917ae2422d13a1bfcb904f12311b7acacafc429f3007a2c587e400916576d6e3","abstract_canon_sha256":"df1e52cecfa554d3901cbf35c3ae1cb1cdfefeb6a6976e9ac3b186ffe4a2f943"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:02:44.266168Z","signature_b64":"SKXu+euSvgJuufdRaRaFbhIppCdcKb/+MjNwVm4Bw5raawZehFYVrzUk/iZr4cMvUxrzQOg9AklH+wVdHfdoDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1e204c119e26d49e7a78d5285da59e202603472deb0f5f3b79e158e0deffee95","last_reissued_at":"2026-05-18T02:02:44.265338Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:02:44.265338Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"TIMASSS: The IRAS16293-2422 Millimeter And Submillimeter Spectral Survey. I. Observations, calibration and analysis of the line kinematics","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Bacmann, A. Castets, A. Coutens, A.G.G.M. Tielens, A. Walters, B. Lefloch, B. Parise, C. Ceccarelli, C. Comito, C. Kahane, C. Vastel, E. Caux, E. van Dishoeck, F.P. Helmich, P. Schilke, S. Bisshop, S. Bottinelli, V. Wakelam","submitted_at":"2011-03-28T13:23:30Z","abstract_excerpt":"While unbiased surveys observable from ground-based telescopes have previously been obtained towards several high mass protostars, very little exists on low mass protostars. To fill up this gap, we carried out a complete spectral survey of the bands at 3, 2, 1 and 0.8 mm towards the solar type protostar IRAS16293-2422. The observations covered about 200\\,GHz and were obtained with the IRAM-30m and JCMT-15m telescopes. Particular attention was devoted to the inter-calibration of the obtained spectra with previous observations. All the lines detected with more than 3 sigma and free from obvious "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1103.5347","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":"1103.5347","created_at":"2026-05-18T02:02:44.265507+00:00"},{"alias_kind":"arxiv_version","alias_value":"1103.5347v1","created_at":"2026-05-18T02:02:44.265507+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1103.5347","created_at":"2026-05-18T02:02:44.265507+00:00"},{"alias_kind":"pith_short_12","alias_value":"DYQEYEM6E3KJ","created_at":"2026-05-18T12:26:26.731475+00:00"},{"alias_kind":"pith_short_16","alias_value":"DYQEYEM6E3KJ46TY","created_at":"2026-05-18T12:26:26.731475+00:00"},{"alias_kind":"pith_short_8","alias_value":"DYQEYEM6","created_at":"2026-05-18T12:26:26.731475+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.27184","citing_title":"Chemical Complexity in the Early Stages of Star Formation in the SKAO Era","ref_index":46,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/DYQEYEM6E3KJ46TY2UUF3JM6EA","json":"https://pith.science/pith/DYQEYEM6E3KJ46TY2UUF3JM6EA.json","graph_json":"https://pith.science/api/pith-number/DYQEYEM6E3KJ46TY2UUF3JM6EA/graph.json","events_json":"https://pith.science/api/pith-number/DYQEYEM6E3KJ46TY2UUF3JM6EA/events.json","paper":"https://pith.science/paper/DYQEYEM6"},"agent_actions":{"view_html":"https://pith.science/pith/DYQEYEM6E3KJ46TY2UUF3JM6EA","download_json":"https://pith.science/pith/DYQEYEM6E3KJ46TY2UUF3JM6EA.json","view_paper":"https://pith.science/paper/DYQEYEM6","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1103.5347&json=true","fetch_graph":"https://pith.science/api/pith-number/DYQEYEM6E3KJ46TY2UUF3JM6EA/graph.json","fetch_events":"https://pith.science/api/pith-number/DYQEYEM6E3KJ46TY2UUF3JM6EA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DYQEYEM6E3KJ46TY2UUF3JM6EA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DYQEYEM6E3KJ46TY2UUF3JM6EA/action/storage_attestation","attest_author":"https://pith.science/pith/DYQEYEM6E3KJ46TY2UUF3JM6EA/action/author_attestation","sign_citation":"https://pith.science/pith/DYQEYEM6E3KJ46TY2UUF3JM6EA/action/citation_signature","submit_replication":"https://pith.science/pith/DYQEYEM6E3KJ46TY2UUF3JM6EA/action/replication_record"}},"created_at":"2026-05-18T02:02:44.265507+00:00","updated_at":"2026-05-18T02:02:44.265507+00:00"}