{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:LNJ4BTG5DL2KHVSPN7HVBG7WBT","short_pith_number":"pith:LNJ4BTG5","schema_version":"1.0","canonical_sha256":"5b53c0ccdd1af4a3d64f6fcf509bf60cccf746f77eef0990f2f679b42bdf2dc3","source":{"kind":"arxiv","id":"2401.08289","version":1},"attestation_state":"computed","paper":{"title":"The hidden companion in J1527: a 0.69 solar-mass white dwarf?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Hao-Bin Liu, Mouyuan Sun, Tuan Yi, Wei-Min Gu, Zhi-Xiang Zhang","submitted_at":"2024-01-16T11:34:58Z","abstract_excerpt":"Finding nearby neutron stars can probe the supernova and metal-enrichment histories near our Solar system. Recently, Lin et al. 2023 reported an exciting neutron star candidate, 2MASS J15274848+3536572 (hereafter J1527), with a small Gaia distance of 118 parsecs. They claim that J1527 harbors an unseen neutron star candidate with an unusually low mass of $0.98\\pm0.03\\,M_{\\odot}$. In this work, we use the Canada-France-Hawaii Telescope high-resolution spectrum to measure J1527's orbital inclination independently. Our spectral fitting suggests an orbital inclination of $63\\pm2$ degrees. Instead,"},"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":"2401.08289","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2024-01-16T11:34:58Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"348e90524680885bf952337c42be5836f2658e03982e54b91d75d843b8f84c68","abstract_canon_sha256":"055a49cfee91f6f2572733e3499a43b62a38a8a340384a003dcbdfde1e24d9e8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:34:10.087970Z","signature_b64":"2VlHUq/1XdK9XcZMldip0025G2ZD2JkdOVFaePtpAaV9H/nW3k+NF6QshUttWMarDleOOQXQPTFYlrvChm2nBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5b53c0ccdd1af4a3d64f6fcf509bf60cccf746f77eef0990f2f679b42bdf2dc3","last_reissued_at":"2026-07-05T07:34:10.087498Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:34:10.087498Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The hidden companion in J1527: a 0.69 solar-mass white dwarf?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Hao-Bin Liu, Mouyuan Sun, Tuan Yi, Wei-Min Gu, Zhi-Xiang Zhang","submitted_at":"2024-01-16T11:34:58Z","abstract_excerpt":"Finding nearby neutron stars can probe the supernova and metal-enrichment histories near our Solar system. Recently, Lin et al. 2023 reported an exciting neutron star candidate, 2MASS J15274848+3536572 (hereafter J1527), with a small Gaia distance of 118 parsecs. They claim that J1527 harbors an unseen neutron star candidate with an unusually low mass of $0.98\\pm0.03\\,M_{\\odot}$. In this work, we use the Canada-France-Hawaii Telescope high-resolution spectrum to measure J1527's orbital inclination independently. Our spectral fitting suggests an orbital inclination of $63\\pm2$ degrees. Instead,"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2401.08289","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/2401.08289/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":"2401.08289","created_at":"2026-07-05T07:34:10.087558+00:00"},{"alias_kind":"arxiv_version","alias_value":"2401.08289v1","created_at":"2026-07-05T07:34:10.087558+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2401.08289","created_at":"2026-07-05T07:34:10.087558+00:00"},{"alias_kind":"pith_short_12","alias_value":"LNJ4BTG5DL2K","created_at":"2026-07-05T07:34:10.087558+00:00"},{"alias_kind":"pith_short_16","alias_value":"LNJ4BTG5DL2KHVSP","created_at":"2026-07-05T07:34:10.087558+00:00"},{"alias_kind":"pith_short_8","alias_value":"LNJ4BTG5","created_at":"2026-07-05T07:34:10.087558+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2509.03001","citing_title":"Low-frequency observations of low-mass binary systems with neutron star candidates","ref_index":79,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LNJ4BTG5DL2KHVSPN7HVBG7WBT","json":"https://pith.science/pith/LNJ4BTG5DL2KHVSPN7HVBG7WBT.json","graph_json":"https://pith.science/api/pith-number/LNJ4BTG5DL2KHVSPN7HVBG7WBT/graph.json","events_json":"https://pith.science/api/pith-number/LNJ4BTG5DL2KHVSPN7HVBG7WBT/events.json","paper":"https://pith.science/paper/LNJ4BTG5"},"agent_actions":{"view_html":"https://pith.science/pith/LNJ4BTG5DL2KHVSPN7HVBG7WBT","download_json":"https://pith.science/pith/LNJ4BTG5DL2KHVSPN7HVBG7WBT.json","view_paper":"https://pith.science/paper/LNJ4BTG5","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2401.08289&json=true","fetch_graph":"https://pith.science/api/pith-number/LNJ4BTG5DL2KHVSPN7HVBG7WBT/graph.json","fetch_events":"https://pith.science/api/pith-number/LNJ4BTG5DL2KHVSPN7HVBG7WBT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LNJ4BTG5DL2KHVSPN7HVBG7WBT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LNJ4BTG5DL2KHVSPN7HVBG7WBT/action/storage_attestation","attest_author":"https://pith.science/pith/LNJ4BTG5DL2KHVSPN7HVBG7WBT/action/author_attestation","sign_citation":"https://pith.science/pith/LNJ4BTG5DL2KHVSPN7HVBG7WBT/action/citation_signature","submit_replication":"https://pith.science/pith/LNJ4BTG5DL2KHVSPN7HVBG7WBT/action/replication_record"}},"created_at":"2026-07-05T07:34:10.087558+00:00","updated_at":"2026-07-05T07:34:10.087558+00:00"}