{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:O43AYEUYXJM6PLNB23RC633IZ3","short_pith_number":"pith:O43AYEUY","schema_version":"1.0","canonical_sha256":"77360c1298ba59e7ada1d6e22f6f68cef71228c6c1a1e1688c4cef681a9b4e8f","source":{"kind":"arxiv","id":"1706.00017","version":1},"attestation_state":"computed","paper":{"title":"The Structure of the Young Star Cluster NGC 6231. I. Stellar Population","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"1, 1), 2), 2) ((1) Millenium Institute of Astrophysics, (2) Universidad de Valpara\\'iso, (3) Pennsylvania State University, (4) Warsaw University Astronomical Observatory), Eric D. Feigelson (3, Jordanka Borissova (1, Konstantin V. Getman (3), Mariusz Gromadzki (4, Michael A. Kuhn (1, Nicol\\'as Medina (1, Radostin Kurtev (1","submitted_at":"2017-05-31T18:00:02Z","abstract_excerpt":"NGC 6231 is a young cluster (age ~2-7 Myr) dominating the Sco OB1 association (distance ~1.59 kpc) with ~100 O and B stars and a large pre-main-sequence stellar population. We combine a reanalysis of archival Chandra X-ray data with multi-epoch NIR photometry from the VVV survey and published optical catalogs to obtain a catalog of 2148 probable cluster members. This catalog is 70% larger than previous censuses of probable cluster members in NGC 6231, and it includes many low-mass stars detected in the NIR but not in the optical and some B-stars without previously noted X-ray counterparts. In "},"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":"1706.00017","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2017-05-31T18:00:02Z","cross_cats_sorted":["astro-ph.HE","astro-ph.SR"],"title_canon_sha256":"f78b09d2784cdc98ab529ccb7c6535edcfd30699abda1032bc86e6d2dadf717a","abstract_canon_sha256":"5b66c0a9e319f5db2619c5007fbad1aae7f625cb0c891f8ecfbb83d3ad097aae"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:38:02.367643Z","signature_b64":"L7nH5ri5Mu99YdQXAeGWVH1MoI/nltN0Fz9npCh0ejBOH8oWPp+7s/FVvV63M5oJS9kJUYfbd0qhgcs247CFCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"77360c1298ba59e7ada1d6e22f6f68cef71228c6c1a1e1688c4cef681a9b4e8f","last_reissued_at":"2026-05-18T00:38:02.367081Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:38:02.367081Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Structure of the Young Star Cluster NGC 6231. I. Stellar Population","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"1, 1), 2), 2) ((1) Millenium Institute of Astrophysics, (2) Universidad de Valpara\\'iso, (3) Pennsylvania State University, (4) Warsaw University Astronomical Observatory), Eric D. Feigelson (3, Jordanka Borissova (1, Konstantin V. Getman (3), Mariusz Gromadzki (4, Michael A. Kuhn (1, Nicol\\'as Medina (1, Radostin Kurtev (1","submitted_at":"2017-05-31T18:00:02Z","abstract_excerpt":"NGC 6231 is a young cluster (age ~2-7 Myr) dominating the Sco OB1 association (distance ~1.59 kpc) with ~100 O and B stars and a large pre-main-sequence stellar population. We combine a reanalysis of archival Chandra X-ray data with multi-epoch NIR photometry from the VVV survey and published optical catalogs to obtain a catalog of 2148 probable cluster members. This catalog is 70% larger than previous censuses of probable cluster members in NGC 6231, and it includes many low-mass stars detected in the NIR but not in the optical and some B-stars without previously noted X-ray counterparts. In "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1706.00017","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":""},"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":"1706.00017","created_at":"2026-05-18T00:38:02.367170+00:00"},{"alias_kind":"arxiv_version","alias_value":"1706.00017v1","created_at":"2026-05-18T00:38:02.367170+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1706.00017","created_at":"2026-05-18T00:38:02.367170+00:00"},{"alias_kind":"pith_short_12","alias_value":"O43AYEUYXJM6","created_at":"2026-05-18T12:31:34.259226+00:00"},{"alias_kind":"pith_short_16","alias_value":"O43AYEUYXJM6PLNB","created_at":"2026-05-18T12:31:34.259226+00:00"},{"alias_kind":"pith_short_8","alias_value":"O43AYEUY","created_at":"2026-05-18T12:31:34.259226+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/O43AYEUYXJM6PLNB23RC633IZ3","json":"https://pith.science/pith/O43AYEUYXJM6PLNB23RC633IZ3.json","graph_json":"https://pith.science/api/pith-number/O43AYEUYXJM6PLNB23RC633IZ3/graph.json","events_json":"https://pith.science/api/pith-number/O43AYEUYXJM6PLNB23RC633IZ3/events.json","paper":"https://pith.science/paper/O43AYEUY"},"agent_actions":{"view_html":"https://pith.science/pith/O43AYEUYXJM6PLNB23RC633IZ3","download_json":"https://pith.science/pith/O43AYEUYXJM6PLNB23RC633IZ3.json","view_paper":"https://pith.science/paper/O43AYEUY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1706.00017&json=true","fetch_graph":"https://pith.science/api/pith-number/O43AYEUYXJM6PLNB23RC633IZ3/graph.json","fetch_events":"https://pith.science/api/pith-number/O43AYEUYXJM6PLNB23RC633IZ3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/O43AYEUYXJM6PLNB23RC633IZ3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/O43AYEUYXJM6PLNB23RC633IZ3/action/storage_attestation","attest_author":"https://pith.science/pith/O43AYEUYXJM6PLNB23RC633IZ3/action/author_attestation","sign_citation":"https://pith.science/pith/O43AYEUYXJM6PLNB23RC633IZ3/action/citation_signature","submit_replication":"https://pith.science/pith/O43AYEUYXJM6PLNB23RC633IZ3/action/replication_record"}},"created_at":"2026-05-18T00:38:02.367170+00:00","updated_at":"2026-05-18T00:38:02.367170+00:00"}