{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:K25TBEJFBHCFGUP66O6LP52QRV","short_pith_number":"pith:K25TBEJF","schema_version":"1.0","canonical_sha256":"56bb30912509c45351fef3bcb7f7508d413835872762818aaaa317123e77feaa","source":{"kind":"arxiv","id":"2404.14797","version":1},"attestation_state":"computed","paper":{"title":"Isochrone Fitting of Galactic Globular Clusters -- VI. High-latitude Clusters NGC5024 (M53), NGC5053, NGC5272 (M3), NGC5466, and NGC7099 (M30)","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"A.A.Marchuk, A.A.Smirnov, A.V.Mosenkov, C.J.Bonatto, D.M.Poliakov, G.A.Gontcharov, M.Yu.Khovritchev, O.S.Ryutina, S.S.Savchenko, V.B.Il'in","submitted_at":"2024-04-23T07:22:52Z","abstract_excerpt":"We fit various colour-magnitude diagrams (CMDs) of the high-latitude Galactic globular clusters NGC\\,5024 (M53), NGC\\,5053, NGC\\,5272 (M3), NGC\\,5466, and NGC\\,7099 (M30) by isochrones from the Dartmouth Stellar Evolution Database and Bag of Stellar Tracks and Isochrones for $\\alpha$-enrichment [$\\alpha$/Fe]$=+0.4$. For the CMDs, we use data sets from {\\it Hubble Space Telescope}, {\\it Gaia}, and other sources utilizing, at least, 25 photometric filters for each cluster. We obtain the following characteristics with their statistic uncertainties for NGC\\,5024, NGC\\,5053, NGC\\,5272, NGC\\,5466, a"},"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":"2404.14797","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2024-04-23T07:22:52Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"2a49aa2d88529bc76eaf0990cdae9cee9a062e7c75f03f806c21f02b4c19958c","abstract_canon_sha256":"39bfb3706b95de19c7826e36acc6f288d021edc5080938196cd57c143d772d40"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:11:10.266676Z","signature_b64":"CY3oGTJ/P5VKx1lxq6XcGL6yULUtreD25l53tN3z4LajqhShYV/N0IdvZaEhPkNLh5HsFwF7ivLEPZqwPXBCCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"56bb30912509c45351fef3bcb7f7508d413835872762818aaaa317123e77feaa","last_reissued_at":"2026-07-05T08:11:10.266190Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:11:10.266190Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Isochrone Fitting of Galactic Globular Clusters -- VI. High-latitude Clusters NGC5024 (M53), NGC5053, NGC5272 (M3), NGC5466, and NGC7099 (M30)","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"A.A.Marchuk, A.A.Smirnov, A.V.Mosenkov, C.J.Bonatto, D.M.Poliakov, G.A.Gontcharov, M.Yu.Khovritchev, O.S.Ryutina, S.S.Savchenko, V.B.Il'in","submitted_at":"2024-04-23T07:22:52Z","abstract_excerpt":"We fit various colour-magnitude diagrams (CMDs) of the high-latitude Galactic globular clusters NGC\\,5024 (M53), NGC\\,5053, NGC\\,5272 (M3), NGC\\,5466, and NGC\\,7099 (M30) by isochrones from the Dartmouth Stellar Evolution Database and Bag of Stellar Tracks and Isochrones for $\\alpha$-enrichment [$\\alpha$/Fe]$=+0.4$. For the CMDs, we use data sets from {\\it Hubble Space Telescope}, {\\it Gaia}, and other sources utilizing, at least, 25 photometric filters for each cluster. We obtain the following characteristics with their statistic uncertainties for NGC\\,5024, NGC\\,5053, NGC\\,5272, NGC\\,5466, a"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2404.14797","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/2404.14797/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":"2404.14797","created_at":"2026-07-05T08:11:10.266258+00:00"},{"alias_kind":"arxiv_version","alias_value":"2404.14797v1","created_at":"2026-07-05T08:11:10.266258+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2404.14797","created_at":"2026-07-05T08:11:10.266258+00:00"},{"alias_kind":"pith_short_12","alias_value":"K25TBEJFBHCF","created_at":"2026-07-05T08:11:10.266258+00:00"},{"alias_kind":"pith_short_16","alias_value":"K25TBEJFBHCFGUP6","created_at":"2026-07-05T08:11:10.266258+00:00"},{"alias_kind":"pith_short_8","alias_value":"K25TBEJF","created_at":"2026-07-05T08:11:10.266258+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.04801","citing_title":"Isochrone fitting of Galactic globular clusters - IX. Tip of the red-giant branch for 27 clusters and constraints on new particle physics","ref_index":32,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/K25TBEJFBHCFGUP66O6LP52QRV","json":"https://pith.science/pith/K25TBEJFBHCFGUP66O6LP52QRV.json","graph_json":"https://pith.science/api/pith-number/K25TBEJFBHCFGUP66O6LP52QRV/graph.json","events_json":"https://pith.science/api/pith-number/K25TBEJFBHCFGUP66O6LP52QRV/events.json","paper":"https://pith.science/paper/K25TBEJF"},"agent_actions":{"view_html":"https://pith.science/pith/K25TBEJFBHCFGUP66O6LP52QRV","download_json":"https://pith.science/pith/K25TBEJFBHCFGUP66O6LP52QRV.json","view_paper":"https://pith.science/paper/K25TBEJF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2404.14797&json=true","fetch_graph":"https://pith.science/api/pith-number/K25TBEJFBHCFGUP66O6LP52QRV/graph.json","fetch_events":"https://pith.science/api/pith-number/K25TBEJFBHCFGUP66O6LP52QRV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/K25TBEJFBHCFGUP66O6LP52QRV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/K25TBEJFBHCFGUP66O6LP52QRV/action/storage_attestation","attest_author":"https://pith.science/pith/K25TBEJFBHCFGUP66O6LP52QRV/action/author_attestation","sign_citation":"https://pith.science/pith/K25TBEJFBHCFGUP66O6LP52QRV/action/citation_signature","submit_replication":"https://pith.science/pith/K25TBEJFBHCFGUP66O6LP52QRV/action/replication_record"}},"created_at":"2026-07-05T08:11:10.266258+00:00","updated_at":"2026-07-05T08:11:10.266258+00:00"}