{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:XA2YTOEWCMGXQGSXJUAG7IE7EY","short_pith_number":"pith:XA2YTOEW","schema_version":"1.0","canonical_sha256":"b83589b896130d781a574d006fa09f2635ae59d4a5542ceb02c87abb8e2e8053","source":{"kind":"arxiv","id":"2211.05573","version":1},"attestation_state":"computed","paper":{"title":"The Star Formation Rate of the Milky Way as seen by Herschel","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Coletta, A. Noriega-Crespo, A. Traficante, A. Zavagno, C. Mininni, D. Elia, D. J. Eden, D. Russeil, E. Schisano, J. D. Soler, L. Olmi, M. Benedettini, M. Merello, M. Sormani, M. Veneziani, P. G. Martin, P. Hennebelle, R. Paladini, R. Plume, R. S. Klessen, S. J. Liu, S. Leurini, S. Molinari, S. Pezzuto, T. Colman, Y. Maruccia","submitted_at":"2022-11-10T13:47:53Z","abstract_excerpt":"We present a new derivation of the Milky Way's current star formation rate (SFR) based on the data of the Hi-GAL Galactic plane survey. We estimate the distribution of the SFR across the Galactic plane from the star-forming clumps identified in the Hi-GAL survey and calculate the total SFR from the sum of their contributions. The estimate of the global SFR amounts to $2.0 \\pm 0.7$~M$_{\\odot}$~yr$^{-1}$, of which $1.7 \\pm 0.6$~M$_{\\odot}$~yr$^{-1}$ coming from clumps with reliable heliocentric distance assignment. This value is in general agreement with estimates found in the literature of last"},"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":"2211.05573","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2022-11-10T13:47:53Z","cross_cats_sorted":[],"title_canon_sha256":"34c41e2182b70a9985b21c8da01483ec5c873dc7516a00f65d8506f44085b694","abstract_canon_sha256":"fde8a2cd0456cd04fba60414fd620ccb3de52b5a094a13c0b425c017e8e8d075"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:28:31.204535Z","signature_b64":"ehKu2c+doyz39v5b8+Tt5ZrUmr2Nf1dQogcxV4mlyO+MvCTQusiud4A4+op89EBVbggLzCIl3utlLRiBJjaOBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b83589b896130d781a574d006fa09f2635ae59d4a5542ceb02c87abb8e2e8053","last_reissued_at":"2026-07-05T05:28:31.204064Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:28:31.204064Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Star Formation Rate of the Milky Way as seen by Herschel","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Coletta, A. Noriega-Crespo, A. Traficante, A. Zavagno, C. Mininni, D. Elia, D. J. Eden, D. Russeil, E. Schisano, J. D. Soler, L. Olmi, M. Benedettini, M. Merello, M. Sormani, M. Veneziani, P. G. Martin, P. Hennebelle, R. Paladini, R. Plume, R. S. Klessen, S. J. Liu, S. Leurini, S. Molinari, S. Pezzuto, T. Colman, Y. Maruccia","submitted_at":"2022-11-10T13:47:53Z","abstract_excerpt":"We present a new derivation of the Milky Way's current star formation rate (SFR) based on the data of the Hi-GAL Galactic plane survey. We estimate the distribution of the SFR across the Galactic plane from the star-forming clumps identified in the Hi-GAL survey and calculate the total SFR from the sum of their contributions. The estimate of the global SFR amounts to $2.0 \\pm 0.7$~M$_{\\odot}$~yr$^{-1}$, of which $1.7 \\pm 0.6$~M$_{\\odot}$~yr$^{-1}$ coming from clumps with reliable heliocentric distance assignment. This value is in general agreement with estimates found in the literature of last"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2211.05573","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/2211.05573/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":"2211.05573","created_at":"2026-07-05T05:28:31.204118+00:00"},{"alias_kind":"arxiv_version","alias_value":"2211.05573v1","created_at":"2026-07-05T05:28:31.204118+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2211.05573","created_at":"2026-07-05T05:28:31.204118+00:00"},{"alias_kind":"pith_short_12","alias_value":"XA2YTOEWCMGX","created_at":"2026-07-05T05:28:31.204118+00:00"},{"alias_kind":"pith_short_16","alias_value":"XA2YTOEWCMGXQGSX","created_at":"2026-07-05T05:28:31.204118+00:00"},{"alias_kind":"pith_short_8","alias_value":"XA2YTOEW","created_at":"2026-07-05T05:28:31.204118+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.31362","citing_title":"Collective Winds of Massive Star Clusters as the Dominant PeVatrons for Galactic Cosmic Rays","ref_index":38,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XA2YTOEWCMGXQGSXJUAG7IE7EY","json":"https://pith.science/pith/XA2YTOEWCMGXQGSXJUAG7IE7EY.json","graph_json":"https://pith.science/api/pith-number/XA2YTOEWCMGXQGSXJUAG7IE7EY/graph.json","events_json":"https://pith.science/api/pith-number/XA2YTOEWCMGXQGSXJUAG7IE7EY/events.json","paper":"https://pith.science/paper/XA2YTOEW"},"agent_actions":{"view_html":"https://pith.science/pith/XA2YTOEWCMGXQGSXJUAG7IE7EY","download_json":"https://pith.science/pith/XA2YTOEWCMGXQGSXJUAG7IE7EY.json","view_paper":"https://pith.science/paper/XA2YTOEW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2211.05573&json=true","fetch_graph":"https://pith.science/api/pith-number/XA2YTOEWCMGXQGSXJUAG7IE7EY/graph.json","fetch_events":"https://pith.science/api/pith-number/XA2YTOEWCMGXQGSXJUAG7IE7EY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XA2YTOEWCMGXQGSXJUAG7IE7EY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XA2YTOEWCMGXQGSXJUAG7IE7EY/action/storage_attestation","attest_author":"https://pith.science/pith/XA2YTOEWCMGXQGSXJUAG7IE7EY/action/author_attestation","sign_citation":"https://pith.science/pith/XA2YTOEWCMGXQGSXJUAG7IE7EY/action/citation_signature","submit_replication":"https://pith.science/pith/XA2YTOEWCMGXQGSXJUAG7IE7EY/action/replication_record"}},"created_at":"2026-07-05T05:28:31.204118+00:00","updated_at":"2026-07-05T05:28:31.204118+00:00"}