{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:NTD5AT27ZQO6MCPSOJZHUQXMOL","short_pith_number":"pith:NTD5AT27","schema_version":"1.0","canonical_sha256":"6cc7d04f5fcc1de609f272727a42ec72e269a1d56326e3da441fe42306fa6e74","source":{"kind":"arxiv","id":"2503.05555","version":1},"attestation_state":"computed","paper":{"title":"ALMAGAL I. The ALMA evolutionary study of high-mass protocluster formation in the Galaxy. Presentation of the survey and early results","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"A. Ahmadi, A. Avison, A. Coletta, A.J. Rigby, A. Nucara, A. Sanchez-Monge, A. Traficante, B. Jones, B. Svoboda, B. Zimmermann, C. Battersby, C.L. Brogan, C. Mininni, C.Y. Law, D. Elia, D. Lis, D. Walker, E. Schisano, F. Amaral, F. De Angelis, F. Fontani, F. Nakamura, F. van der Tak, F. Wyrowski, G.A. Fuller, G. Stroud, H. Beuther, H. Zinnecker, J. Bally, J.D. Soler, J. Wallace, K.G. Johnston, K. Goh, K.L.J. Rygl, K.T. Kim, L. Bronfman, L. Maud, L. Moscadelli, L. Testi, M. Benedettini, M.G. Hoare, M. Merello, M.R.A. Wells, M.T. Beltran, N. Peretto, P.D. Klaassen, P. Hatchfield, P. Hennebelle, P. Koch, P. Sanhueza, P. Schilke, P.T.P. Ho, Q. Zhang, R. Cesaroni, R. Kuiper, R. Plume, R.S. Klessen, S.D. Clarke, S. Liu, S.L. Lumsden, S.-L. Qin, S. Molinari, S. Pezzuto, S. Pfalzner, S. Walch, S.-Y. Liu, T. Henning, T. Liu, T. Moeller, T.R. Hunter, T. Zhang, U. Lebreuilly, V.S. Veena, W.-J. Kim, Y.-N. Su, Y.-W. Tang","submitted_at":"2025-03-07T16:32:44Z","abstract_excerpt":"Fundamental questions about the physics responsible for fragmenting molecular parsec-scale clumps into cores of ~1000 au are still open, that only a statistically significant investigation with ALMA is able to address: what are the dominant agents that determine the core demographics, mass, and spatial distribution as a function of the physical properties of the hosting clumps, their evolutionary stage and the different Galactic environments in which they reside? To what extent extent is fragmentation driven by clumps dynamics or mass transport in filaments? With ALMAGAL we observed the 1.38 m"},"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":"2503.05555","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2025-03-07T16:32:44Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"2092ab20cbb4d87fa70a2c2c4177502390a0c60dc26cf00b05862153f9017945","abstract_canon_sha256":"72d85bea46cab7bdfbfcbbac35512cd16f4ddb5a56c00c70cb79b8e082687292"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:26:31.240805Z","signature_b64":"7S+WxpcG0/uP3eHEPN6/WtS5lzD6mK9Us7gXJfQWTswByTOoyiQnEFbO5ipW+/MfTmDBAE+eBu+O+nQ30J+0BQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6cc7d04f5fcc1de609f272727a42ec72e269a1d56326e3da441fe42306fa6e74","last_reissued_at":"2026-07-05T10:26:31.240110Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:26:31.240110Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"ALMAGAL I. The ALMA evolutionary study of high-mass protocluster formation in the Galaxy. Presentation of the survey and early results","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"A. Ahmadi, A. Avison, A. Coletta, A.J. Rigby, A. Nucara, A. Sanchez-Monge, A. Traficante, B. Jones, B. Svoboda, B. Zimmermann, C. Battersby, C.L. Brogan, C. Mininni, C.Y. Law, D. Elia, D. Lis, D. Walker, E. Schisano, F. Amaral, F. De Angelis, F. Fontani, F. Nakamura, F. van der Tak, F. Wyrowski, G.A. Fuller, G. Stroud, H. Beuther, H. Zinnecker, J. Bally, J.D. Soler, J. Wallace, K.G. Johnston, K. Goh, K.L.J. Rygl, K.T. Kim, L. Bronfman, L. Maud, L. Moscadelli, L. Testi, M. Benedettini, M.G. Hoare, M. Merello, M.R.A. Wells, M.T. Beltran, N. Peretto, P.D. Klaassen, P. Hatchfield, P. Hennebelle, P. Koch, P. Sanhueza, P. Schilke, P.T.P. Ho, Q. Zhang, R. Cesaroni, R. Kuiper, R. Plume, R.S. Klessen, S.D. Clarke, S. Liu, S.L. Lumsden, S.-L. Qin, S. Molinari, S. Pezzuto, S. Pfalzner, S. Walch, S.-Y. Liu, T. Henning, T. Liu, T. Moeller, T.R. Hunter, T. Zhang, U. Lebreuilly, V.S. Veena, W.-J. Kim, Y.-N. Su, Y.-W. Tang","submitted_at":"2025-03-07T16:32:44Z","abstract_excerpt":"Fundamental questions about the physics responsible for fragmenting molecular parsec-scale clumps into cores of ~1000 au are still open, that only a statistically significant investigation with ALMA is able to address: what are the dominant agents that determine the core demographics, mass, and spatial distribution as a function of the physical properties of the hosting clumps, their evolutionary stage and the different Galactic environments in which they reside? To what extent extent is fragmentation driven by clumps dynamics or mass transport in filaments? With ALMAGAL we observed the 1.38 m"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2503.05555","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/2503.05555/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":"2503.05555","created_at":"2026-07-05T10:26:31.240198+00:00"},{"alias_kind":"arxiv_version","alias_value":"2503.05555v1","created_at":"2026-07-05T10:26:31.240198+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2503.05555","created_at":"2026-07-05T10:26:31.240198+00:00"},{"alias_kind":"pith_short_12","alias_value":"NTD5AT27ZQO6","created_at":"2026-07-05T10:26:31.240198+00:00"},{"alias_kind":"pith_short_16","alias_value":"NTD5AT27ZQO6MCPS","created_at":"2026-07-05T10:26:31.240198+00:00"},{"alias_kind":"pith_short_8","alias_value":"NTD5AT27","created_at":"2026-07-05T10:26:31.240198+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07489","citing_title":"Chemical diversity of dense cores in Orion B: The role of the environment","ref_index":21,"is_internal_anchor":true},{"citing_arxiv_id":"2604.19878","citing_title":"The fragmentation properties of massive star-forming regions in 30Dor-10 at 2000 au resolution","ref_index":40,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NTD5AT27ZQO6MCPSOJZHUQXMOL","json":"https://pith.science/pith/NTD5AT27ZQO6MCPSOJZHUQXMOL.json","graph_json":"https://pith.science/api/pith-number/NTD5AT27ZQO6MCPSOJZHUQXMOL/graph.json","events_json":"https://pith.science/api/pith-number/NTD5AT27ZQO6MCPSOJZHUQXMOL/events.json","paper":"https://pith.science/paper/NTD5AT27"},"agent_actions":{"view_html":"https://pith.science/pith/NTD5AT27ZQO6MCPSOJZHUQXMOL","download_json":"https://pith.science/pith/NTD5AT27ZQO6MCPSOJZHUQXMOL.json","view_paper":"https://pith.science/paper/NTD5AT27","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2503.05555&json=true","fetch_graph":"https://pith.science/api/pith-number/NTD5AT27ZQO6MCPSOJZHUQXMOL/graph.json","fetch_events":"https://pith.science/api/pith-number/NTD5AT27ZQO6MCPSOJZHUQXMOL/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NTD5AT27ZQO6MCPSOJZHUQXMOL/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NTD5AT27ZQO6MCPSOJZHUQXMOL/action/storage_attestation","attest_author":"https://pith.science/pith/NTD5AT27ZQO6MCPSOJZHUQXMOL/action/author_attestation","sign_citation":"https://pith.science/pith/NTD5AT27ZQO6MCPSOJZHUQXMOL/action/citation_signature","submit_replication":"https://pith.science/pith/NTD5AT27ZQO6MCPSOJZHUQXMOL/action/replication_record"}},"created_at":"2026-07-05T10:26:31.240198+00:00","updated_at":"2026-07-05T10:26:31.240198+00:00"}