{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:CU37RBCMPEODNRCRFMJEXMEKTM","short_pith_number":"pith:CU37RBCM","schema_version":"1.0","canonical_sha256":"1537f8844c791c36c4512b124bb08a9b0dbad0e02721c24de643335de9fee883","source":{"kind":"arxiv","id":"2301.03144","version":1},"attestation_state":"computed","paper":{"title":"Evidence of high-mass star formation through multi-scale mass accretion in hub-filament-system clouds","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Amelia Stutz, Anandmayee Tej, Anindya Saha, Anxu Luo, Archana Soam, Chang Won Lee, Dongting Yang, Feng-Wei Xu, Guido Garay, Hong-Li Liu, Jianwen Zhou, Jinhua He, Kaho Morii, Ken\\'ichi Tatematsu, Ke Wang, Leonardo Bronfman, Lokesh Dewangan, L. Viktor Toth, Namitha Issac, Patricio Sanhueza, Paul F. Goldsmith, Qiu-Yi Luo, Shanghuo Li, Shengli Qin, Siju Zhang, Sirong Pan, Tapas Baug, Tie Liu, Xianjin Shen, Xun-Chuan Liu, Yong Zhang, Yue-Fang Wu, Zhiyuan Ren","submitted_at":"2023-01-09T01:59:14Z","abstract_excerpt":"We present a statistical study of a sample of 17 hub-filament-system (HFS) clouds of high-mass star formation using high-angular resolution ($\\sim$1-2 arcsecond) ALMA 1.3mm and 3mm continuum data. The sample includes 8 infrared (IR)-dark and 9 IR-bright types, which correspond to an evolutionary sequence from the IR-dark to IR-bright stage. The central massive clumps and their associated most massive cores are observed to follow a trend of increasing mass ($M$) and mass surface density ($\\Sigma$) with evolution from IR-dark to IR-bright stage. In addition, a mass-segregated cluster of young st"},"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":"2301.03144","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2023-01-09T01:59:14Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"91b8e0b1b388a0ae5fd09bd8f1f79062cebab54fd14927e1500cd7b9b741f97e","abstract_canon_sha256":"505290c940c92afb146765e0e6f94732d2e8f44d0fcc8cf05b5cae293888988c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:35:32.194060Z","signature_b64":"nqOnX8A1Iyq+7yqWXWALHscytDN8THYywSBVyfLF04SCg47HwMKnMQdmN1ghknJ5KI8DH0rDwO6OPnWxQzCUCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1537f8844c791c36c4512b124bb08a9b0dbad0e02721c24de643335de9fee883","last_reissued_at":"2026-07-05T05:35:32.193553Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:35:32.193553Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Evidence of high-mass star formation through multi-scale mass accretion in hub-filament-system clouds","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Amelia Stutz, Anandmayee Tej, Anindya Saha, Anxu Luo, Archana Soam, Chang Won Lee, Dongting Yang, Feng-Wei Xu, Guido Garay, Hong-Li Liu, Jianwen Zhou, Jinhua He, Kaho Morii, Ken\\'ichi Tatematsu, Ke Wang, Leonardo Bronfman, Lokesh Dewangan, L. Viktor Toth, Namitha Issac, Patricio Sanhueza, Paul F. Goldsmith, Qiu-Yi Luo, Shanghuo Li, Shengli Qin, Siju Zhang, Sirong Pan, Tapas Baug, Tie Liu, Xianjin Shen, Xun-Chuan Liu, Yong Zhang, Yue-Fang Wu, Zhiyuan Ren","submitted_at":"2023-01-09T01:59:14Z","abstract_excerpt":"We present a statistical study of a sample of 17 hub-filament-system (HFS) clouds of high-mass star formation using high-angular resolution ($\\sim$1-2 arcsecond) ALMA 1.3mm and 3mm continuum data. The sample includes 8 infrared (IR)-dark and 9 IR-bright types, which correspond to an evolutionary sequence from the IR-dark to IR-bright stage. The central massive clumps and their associated most massive cores are observed to follow a trend of increasing mass ($M$) and mass surface density ($\\Sigma$) with evolution from IR-dark to IR-bright stage. In addition, a mass-segregated cluster of young st"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2301.03144","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/2301.03144/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":"2301.03144","created_at":"2026-07-05T05:35:32.193616+00:00"},{"alias_kind":"arxiv_version","alias_value":"2301.03144v1","created_at":"2026-07-05T05:35:32.193616+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2301.03144","created_at":"2026-07-05T05:35:32.193616+00:00"},{"alias_kind":"pith_short_12","alias_value":"CU37RBCMPEOD","created_at":"2026-07-05T05:35:32.193616+00:00"},{"alias_kind":"pith_short_16","alias_value":"CU37RBCMPEODNRCR","created_at":"2026-07-05T05:35:32.193616+00:00"},{"alias_kind":"pith_short_8","alias_value":"CU37RBCM","created_at":"2026-07-05T05:35:32.193616+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/CU37RBCMPEODNRCRFMJEXMEKTM","json":"https://pith.science/pith/CU37RBCMPEODNRCRFMJEXMEKTM.json","graph_json":"https://pith.science/api/pith-number/CU37RBCMPEODNRCRFMJEXMEKTM/graph.json","events_json":"https://pith.science/api/pith-number/CU37RBCMPEODNRCRFMJEXMEKTM/events.json","paper":"https://pith.science/paper/CU37RBCM"},"agent_actions":{"view_html":"https://pith.science/pith/CU37RBCMPEODNRCRFMJEXMEKTM","download_json":"https://pith.science/pith/CU37RBCMPEODNRCRFMJEXMEKTM.json","view_paper":"https://pith.science/paper/CU37RBCM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2301.03144&json=true","fetch_graph":"https://pith.science/api/pith-number/CU37RBCMPEODNRCRFMJEXMEKTM/graph.json","fetch_events":"https://pith.science/api/pith-number/CU37RBCMPEODNRCRFMJEXMEKTM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CU37RBCMPEODNRCRFMJEXMEKTM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CU37RBCMPEODNRCRFMJEXMEKTM/action/storage_attestation","attest_author":"https://pith.science/pith/CU37RBCMPEODNRCRFMJEXMEKTM/action/author_attestation","sign_citation":"https://pith.science/pith/CU37RBCMPEODNRCRFMJEXMEKTM/action/citation_signature","submit_replication":"https://pith.science/pith/CU37RBCMPEODNRCRFMJEXMEKTM/action/replication_record"}},"created_at":"2026-07-05T05:35:32.193616+00:00","updated_at":"2026-07-05T05:35:32.193616+00:00"}