{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:JI4OT2J55AT3KECOQJ4NTXBOOB","short_pith_number":"pith:JI4OT2J5","schema_version":"1.0","canonical_sha256":"4a38e9e93de827b5104e8278d9dc2e70614be9cf916334c43fdd687735a8a239","source":{"kind":"arxiv","id":"2409.06572","version":2},"attestation_state":"computed","paper":{"title":"The molecular gas content throughout the low-z merger sequence","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Saintonge, D. Cs. Moln\\'ar, G. Violino, J. M. Scudder, J. T. Mendel, Mark T. Sargent, S. L. Ellison, T. Schwandt","submitted_at":"2024-09-10T15:08:56Z","abstract_excerpt":"Exploiting IRAM 30m CO spectroscopy, we find that SDSS post-merger galaxies display gas fractions and depletion times enhanced by 25-50%, a mildly higher CO excitation, and standard molecular-to-atomic gas ratios, compared to non-interacting galaxies with similar redshift, stellar mass ($M_{\\star}$) and star-formation rate (SFR). To place these results in context, we compile further samples of interacting or starbursting galaxies, from pre-coalescence kinematic pairs to post-starbursts, carefully homogenising gas mass, $M_{\\star}$ and SFR measurements in the process. We explore systematics by "},"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":"2409.06572","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2024-09-10T15:08:56Z","cross_cats_sorted":[],"title_canon_sha256":"cdea25f7ecda7498591e65f16cba4a343e9d33b31002186ef526e2cda324bf49","abstract_canon_sha256":"e82046d85c04da3f8d1c4b434cd99b66830488b775c655adb81cbb00aa537c03"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:43:01.351271Z","signature_b64":"OpEwQp9EXkCZNiMqgoaPDfOb+XGXXMZNBHmt+lvAJMiOZlHK60rXHrZ3d05/jRjmMT5Tck9YDj3sY9mC6CckDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4a38e9e93de827b5104e8278d9dc2e70614be9cf916334c43fdd687735a8a239","last_reissued_at":"2026-07-05T10:43:01.350769Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:43:01.350769Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The molecular gas content throughout the low-z merger sequence","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Saintonge, D. Cs. Moln\\'ar, G. Violino, J. M. Scudder, J. T. Mendel, Mark T. Sargent, S. L. Ellison, T. Schwandt","submitted_at":"2024-09-10T15:08:56Z","abstract_excerpt":"Exploiting IRAM 30m CO spectroscopy, we find that SDSS post-merger galaxies display gas fractions and depletion times enhanced by 25-50%, a mildly higher CO excitation, and standard molecular-to-atomic gas ratios, compared to non-interacting galaxies with similar redshift, stellar mass ($M_{\\star}$) and star-formation rate (SFR). To place these results in context, we compile further samples of interacting or starbursting galaxies, from pre-coalescence kinematic pairs to post-starbursts, carefully homogenising gas mass, $M_{\\star}$ and SFR measurements in the process. We explore systematics by "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2409.06572","kind":"arxiv","version":2},"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/2409.06572/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":"2409.06572","created_at":"2026-07-05T10:43:01.350827+00:00"},{"alias_kind":"arxiv_version","alias_value":"2409.06572v2","created_at":"2026-07-05T10:43:01.350827+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2409.06572","created_at":"2026-07-05T10:43:01.350827+00:00"},{"alias_kind":"pith_short_12","alias_value":"JI4OT2J55AT3","created_at":"2026-07-05T10:43:01.350827+00:00"},{"alias_kind":"pith_short_16","alias_value":"JI4OT2J55AT3KECO","created_at":"2026-07-05T10:43:01.350827+00:00"},{"alias_kind":"pith_short_8","alias_value":"JI4OT2J5","created_at":"2026-07-05T10:43:01.350827+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2501.14031","citing_title":"Interacting galaxies in the IllustrisTNG simulations -- VIII: Pericentric star formation rate enhancements are driven both by increased fuelling and efficiency","ref_index":84,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JI4OT2J55AT3KECOQJ4NTXBOOB","json":"https://pith.science/pith/JI4OT2J55AT3KECOQJ4NTXBOOB.json","graph_json":"https://pith.science/api/pith-number/JI4OT2J55AT3KECOQJ4NTXBOOB/graph.json","events_json":"https://pith.science/api/pith-number/JI4OT2J55AT3KECOQJ4NTXBOOB/events.json","paper":"https://pith.science/paper/JI4OT2J5"},"agent_actions":{"view_html":"https://pith.science/pith/JI4OT2J55AT3KECOQJ4NTXBOOB","download_json":"https://pith.science/pith/JI4OT2J55AT3KECOQJ4NTXBOOB.json","view_paper":"https://pith.science/paper/JI4OT2J5","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2409.06572&json=true","fetch_graph":"https://pith.science/api/pith-number/JI4OT2J55AT3KECOQJ4NTXBOOB/graph.json","fetch_events":"https://pith.science/api/pith-number/JI4OT2J55AT3KECOQJ4NTXBOOB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JI4OT2J55AT3KECOQJ4NTXBOOB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JI4OT2J55AT3KECOQJ4NTXBOOB/action/storage_attestation","attest_author":"https://pith.science/pith/JI4OT2J55AT3KECOQJ4NTXBOOB/action/author_attestation","sign_citation":"https://pith.science/pith/JI4OT2J55AT3KECOQJ4NTXBOOB/action/citation_signature","submit_replication":"https://pith.science/pith/JI4OT2J55AT3KECOQJ4NTXBOOB/action/replication_record"}},"created_at":"2026-07-05T10:43:01.350827+00:00","updated_at":"2026-07-05T10:43:01.350827+00:00"}