{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:JZRMDKPFLERGJKTRS7TF4FAHLZ","short_pith_number":"pith:JZRMDKPF","schema_version":"1.0","canonical_sha256":"4e62c1a9e5592264aa7197e65e14075e4ea8ce3d509f474e8b799848fa21bf27","source":{"kind":"arxiv","id":"2208.12112","version":1},"attestation_state":"computed","paper":{"title":"A Mass-Magnitude Relation for Low-mass Stars Based on Dynamical Measurements of Thousands of Binary Star Systems","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"Cullen H. Blake, Mark R. Giovinazzi","submitted_at":"2022-08-25T14:18:23Z","abstract_excerpt":"Stellar mass is a fundamental parameter that is key to our understanding of stellar formation and evolution, as well as the characterization of nearby exoplanet companions. Historically, stellar masses have been derived from long-term observations of visual or spectroscopic binary star systems. While advances in high-resolution imaging have enabled observations of systems with shorter orbital periods, stellar mass measurements remain challenging, and relatively few have been precisely measured. We present a new statistical approach to measuring masses for populations of stars. Using Gaia astro"},"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":"2208.12112","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2022-08-25T14:18:23Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"0f8503499624486d5962a037df5b5976255dd28ac3d768cf8a141dd9871b3da7","abstract_canon_sha256":"03a2ba6ce0c7f42e585c0684ab3a58eb0c9db48c70b084ba9714cfe74d263582"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:03:29.806477Z","signature_b64":"6DnS3K/NF96YbjWpDQHeZR1MeqgEvT+9L0cpGryCiSpHim6TGrYU924JYw0kfcAwm98QrIGho74nPDIkUur1Aw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4e62c1a9e5592264aa7197e65e14075e4ea8ce3d509f474e8b799848fa21bf27","last_reissued_at":"2026-07-05T05:03:29.805984Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:03:29.805984Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Mass-Magnitude Relation for Low-mass Stars Based on Dynamical Measurements of Thousands of Binary Star Systems","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"Cullen H. Blake, Mark R. Giovinazzi","submitted_at":"2022-08-25T14:18:23Z","abstract_excerpt":"Stellar mass is a fundamental parameter that is key to our understanding of stellar formation and evolution, as well as the characterization of nearby exoplanet companions. Historically, stellar masses have been derived from long-term observations of visual or spectroscopic binary star systems. While advances in high-resolution imaging have enabled observations of systems with shorter orbital periods, stellar mass measurements remain challenging, and relatively few have been precisely measured. We present a new statistical approach to measuring masses for populations of stars. Using Gaia astro"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2208.12112","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/2208.12112/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":"2208.12112","created_at":"2026-07-05T05:03:29.806041+00:00"},{"alias_kind":"arxiv_version","alias_value":"2208.12112v1","created_at":"2026-07-05T05:03:29.806041+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2208.12112","created_at":"2026-07-05T05:03:29.806041+00:00"},{"alias_kind":"pith_short_12","alias_value":"JZRMDKPFLERG","created_at":"2026-07-05T05:03:29.806041+00:00"},{"alias_kind":"pith_short_16","alias_value":"JZRMDKPFLERGJKTR","created_at":"2026-07-05T05:03:29.806041+00:00"},{"alias_kind":"pith_short_8","alias_value":"JZRMDKPF","created_at":"2026-07-05T05:03:29.806041+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2505.12563","citing_title":"The NEID Earth Twin Survey. II. Dynamical Masses in Seven High-acceleration Star Systems","ref_index":62,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JZRMDKPFLERGJKTRS7TF4FAHLZ","json":"https://pith.science/pith/JZRMDKPFLERGJKTRS7TF4FAHLZ.json","graph_json":"https://pith.science/api/pith-number/JZRMDKPFLERGJKTRS7TF4FAHLZ/graph.json","events_json":"https://pith.science/api/pith-number/JZRMDKPFLERGJKTRS7TF4FAHLZ/events.json","paper":"https://pith.science/paper/JZRMDKPF"},"agent_actions":{"view_html":"https://pith.science/pith/JZRMDKPFLERGJKTRS7TF4FAHLZ","download_json":"https://pith.science/pith/JZRMDKPFLERGJKTRS7TF4FAHLZ.json","view_paper":"https://pith.science/paper/JZRMDKPF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2208.12112&json=true","fetch_graph":"https://pith.science/api/pith-number/JZRMDKPFLERGJKTRS7TF4FAHLZ/graph.json","fetch_events":"https://pith.science/api/pith-number/JZRMDKPFLERGJKTRS7TF4FAHLZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JZRMDKPFLERGJKTRS7TF4FAHLZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JZRMDKPFLERGJKTRS7TF4FAHLZ/action/storage_attestation","attest_author":"https://pith.science/pith/JZRMDKPFLERGJKTRS7TF4FAHLZ/action/author_attestation","sign_citation":"https://pith.science/pith/JZRMDKPFLERGJKTRS7TF4FAHLZ/action/citation_signature","submit_replication":"https://pith.science/pith/JZRMDKPFLERGJKTRS7TF4FAHLZ/action/replication_record"}},"created_at":"2026-07-05T05:03:29.806041+00:00","updated_at":"2026-07-05T05:03:29.806041+00:00"}