{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:RTEOGKBAVHW57PPCDA7JFJMH4L","short_pith_number":"pith:RTEOGKBA","schema_version":"1.0","canonical_sha256":"8cc8e32820a9eddfbde2183e92a587e2ea6a3139c9fd7d034d4d35a404495428","source":{"kind":"arxiv","id":"1907.00731","version":1},"attestation_state":"computed","paper":{"title":"The molecular outflow in NGC253 at a resolution of two parsecs","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Adam K. Leroy, Alberto D. Bolatto, Axel Wei{\\ss}, David S. Meier, Elisabeth A.C. Mills, Fabian Walter, J\\\"urgen Ott, Laura K. Zschaechner, Mark Gorski, Nico Krieger, Rebecca C. Levy, Sylvain Veilleux","submitted_at":"2019-07-01T12:44:28Z","abstract_excerpt":"We present 0.15'' (~2.5pc) resolution ALMA CO(3-2) observations of the starbursting center in NGC253. Together with archival ALMA CO(1-0) and CO(2-1) data we decompose the emission into a disk and non-disk component. We find ~7-16% of the CO luminosity to be associated with the non-disk component ($1.2-4.2 \\times 10^7$ K km s$^{-1}$ pc$^2$). The total molecular gas mass in the center of NGC253 is $\\sim 3.6 \\times 10^8$ M$_\\odot$ with $\\sim 0.5 \\times 10^8$ M$_\\odot$ (~15%) in the non-disk component. These measurements are consistent across independent mass estimates through three CO transition"},"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":"1907.00731","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2019-07-01T12:44:28Z","cross_cats_sorted":[],"title_canon_sha256":"b439e058913d21f5fdba0780922afb462a7074d9d23bb023212d06e1a024b24b","abstract_canon_sha256":"2adb94b4369cce192b5d425ddd625b21df71f0878925420e727dae0aabcb3b2b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T23:58:27.863907Z","signature_b64":"sW7roCvx9V+mihZYMKhRM+Pavf33NxGcTZHeAH6McNfyMYTRNSGY7StevJiXyokFpc6LU3mhCPrNlbFRuuNuBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8cc8e32820a9eddfbde2183e92a587e2ea6a3139c9fd7d034d4d35a404495428","last_reissued_at":"2026-07-04T23:58:27.863449Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T23:58:27.863449Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The molecular outflow in NGC253 at a resolution of two parsecs","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Adam K. Leroy, Alberto D. Bolatto, Axel Wei{\\ss}, David S. Meier, Elisabeth A.C. Mills, Fabian Walter, J\\\"urgen Ott, Laura K. Zschaechner, Mark Gorski, Nico Krieger, Rebecca C. Levy, Sylvain Veilleux","submitted_at":"2019-07-01T12:44:28Z","abstract_excerpt":"We present 0.15'' (~2.5pc) resolution ALMA CO(3-2) observations of the starbursting center in NGC253. Together with archival ALMA CO(1-0) and CO(2-1) data we decompose the emission into a disk and non-disk component. We find ~7-16% of the CO luminosity to be associated with the non-disk component ($1.2-4.2 \\times 10^7$ K km s$^{-1}$ pc$^2$). The total molecular gas mass in the center of NGC253 is $\\sim 3.6 \\times 10^8$ M$_\\odot$ with $\\sim 0.5 \\times 10^8$ M$_\\odot$ (~15%) in the non-disk component. These measurements are consistent across independent mass estimates through three CO transition"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1907.00731","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/1907.00731/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":"1907.00731","created_at":"2026-07-04T23:58:27.863507+00:00"},{"alias_kind":"arxiv_version","alias_value":"1907.00731v1","created_at":"2026-07-04T23:58:27.863507+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1907.00731","created_at":"2026-07-04T23:58:27.863507+00:00"},{"alias_kind":"pith_short_12","alias_value":"RTEOGKBAVHW5","created_at":"2026-07-04T23:58:27.863507+00:00"},{"alias_kind":"pith_short_16","alias_value":"RTEOGKBAVHW57PPC","created_at":"2026-07-04T23:58:27.863507+00:00"},{"alias_kind":"pith_short_8","alias_value":"RTEOGKBA","created_at":"2026-07-04T23:58:27.863507+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1908.01775","citing_title":"Dusty Cloud Acceleration with Multiband Radiation","ref_index":23,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RTEOGKBAVHW57PPCDA7JFJMH4L","json":"https://pith.science/pith/RTEOGKBAVHW57PPCDA7JFJMH4L.json","graph_json":"https://pith.science/api/pith-number/RTEOGKBAVHW57PPCDA7JFJMH4L/graph.json","events_json":"https://pith.science/api/pith-number/RTEOGKBAVHW57PPCDA7JFJMH4L/events.json","paper":"https://pith.science/paper/RTEOGKBA"},"agent_actions":{"view_html":"https://pith.science/pith/RTEOGKBAVHW57PPCDA7JFJMH4L","download_json":"https://pith.science/pith/RTEOGKBAVHW57PPCDA7JFJMH4L.json","view_paper":"https://pith.science/paper/RTEOGKBA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1907.00731&json=true","fetch_graph":"https://pith.science/api/pith-number/RTEOGKBAVHW57PPCDA7JFJMH4L/graph.json","fetch_events":"https://pith.science/api/pith-number/RTEOGKBAVHW57PPCDA7JFJMH4L/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RTEOGKBAVHW57PPCDA7JFJMH4L/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RTEOGKBAVHW57PPCDA7JFJMH4L/action/storage_attestation","attest_author":"https://pith.science/pith/RTEOGKBAVHW57PPCDA7JFJMH4L/action/author_attestation","sign_citation":"https://pith.science/pith/RTEOGKBAVHW57PPCDA7JFJMH4L/action/citation_signature","submit_replication":"https://pith.science/pith/RTEOGKBAVHW57PPCDA7JFJMH4L/action/replication_record"}},"created_at":"2026-07-04T23:58:27.863507+00:00","updated_at":"2026-07-04T23:58:27.863507+00:00"}