{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:JL5UIZ6JU254CCD7TGDO5M7AKD","short_pith_number":"pith:JL5UIZ6J","schema_version":"1.0","canonical_sha256":"4afb4467c9a6bbc1087f9986eeb3e050e7cb72f5d1ddbdf330d41265fe092436","source":{"kind":"arxiv","id":"2112.10256","version":3},"attestation_state":"computed","paper":{"title":"The redshift dependence of black hole mass distribution: Is it reliable for standard sirens cosmology?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Suvodip Mukherjee","submitted_at":"2021-12-19T20:50:01Z","abstract_excerpt":"An upper limit on the mass of a black hole set by the pair-instability supernovae (PISN) process can be useful in inferring the redshift of the gravitational wave (GW) sources by lifting the degeneracy between mass and redshift. However, for this technique to work, it is essential that the PISN mass-scale is redshift independent or at least has a predictable redshift dependence. We show that the observed PISN mass-scale can get smeared and the position of the PISN mass-scale is likely to exhibit a strong redshift dependence due to a combined effect from the non-zero value of the delay time bet"},"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":"2112.10256","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2021-12-19T20:50:01Z","cross_cats_sorted":["astro-ph.HE","gr-qc"],"title_canon_sha256":"70107903ef4acb6c18c7b6a057f6ac8001313d1874032d74e8588b797e4f4b34","abstract_canon_sha256":"4de636126faa4597d98c9352667d015aa0aefd87603f46181f807a4a5c1b44e0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:06:29.153778Z","signature_b64":"T5F2g8ipcoiGVgkV3FskebLjot6ket5WarRpsp1rtP5EI358NN7c9rEPPQ0wx1CjgVPLvKZv7Yl+MZ5U/bjqBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4afb4467c9a6bbc1087f9986eeb3e050e7cb72f5d1ddbdf330d41265fe092436","last_reissued_at":"2026-07-05T05:06:29.153272Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:06:29.153272Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The redshift dependence of black hole mass distribution: Is it reliable for standard sirens cosmology?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Suvodip Mukherjee","submitted_at":"2021-12-19T20:50:01Z","abstract_excerpt":"An upper limit on the mass of a black hole set by the pair-instability supernovae (PISN) process can be useful in inferring the redshift of the gravitational wave (GW) sources by lifting the degeneracy between mass and redshift. However, for this technique to work, it is essential that the PISN mass-scale is redshift independent or at least has a predictable redshift dependence. We show that the observed PISN mass-scale can get smeared and the position of the PISN mass-scale is likely to exhibit a strong redshift dependence due to a combined effect from the non-zero value of the delay time bet"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2112.10256","kind":"arxiv","version":3},"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/2112.10256/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":"2112.10256","created_at":"2026-07-05T05:06:29.153337+00:00"},{"alias_kind":"arxiv_version","alias_value":"2112.10256v3","created_at":"2026-07-05T05:06:29.153337+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2112.10256","created_at":"2026-07-05T05:06:29.153337+00:00"},{"alias_kind":"pith_short_12","alias_value":"JL5UIZ6JU254","created_at":"2026-07-05T05:06:29.153337+00:00"},{"alias_kind":"pith_short_16","alias_value":"JL5UIZ6JU254CCD7","created_at":"2026-07-05T05:06:29.153337+00:00"},{"alias_kind":"pith_short_8","alias_value":"JL5UIZ6J","created_at":"2026-07-05T05:06:29.153337+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.28299","citing_title":"The impact of stellar binaries and star cluster dynamics on pair-instability supernovae","ref_index":266,"is_internal_anchor":false},{"citing_arxiv_id":"2605.20112","citing_title":"Gravitational-wave constraints on $H_0$ are robust to (putative) redshift evolution in the binary black hole mass spectrum at current sensitivity","ref_index":29,"is_internal_anchor":false},{"citing_arxiv_id":"2510.16955","citing_title":"On the use of the Derivative Approximation for Likelihoods for Gravitational Wave Inference","ref_index":49,"is_internal_anchor":false},{"citing_arxiv_id":"2604.14290","citing_title":"Emergent structure in the binary black hole mass distribution and implications for population-based cosmology","ref_index":97,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JL5UIZ6JU254CCD7TGDO5M7AKD","json":"https://pith.science/pith/JL5UIZ6JU254CCD7TGDO5M7AKD.json","graph_json":"https://pith.science/api/pith-number/JL5UIZ6JU254CCD7TGDO5M7AKD/graph.json","events_json":"https://pith.science/api/pith-number/JL5UIZ6JU254CCD7TGDO5M7AKD/events.json","paper":"https://pith.science/paper/JL5UIZ6J"},"agent_actions":{"view_html":"https://pith.science/pith/JL5UIZ6JU254CCD7TGDO5M7AKD","download_json":"https://pith.science/pith/JL5UIZ6JU254CCD7TGDO5M7AKD.json","view_paper":"https://pith.science/paper/JL5UIZ6J","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2112.10256&json=true","fetch_graph":"https://pith.science/api/pith-number/JL5UIZ6JU254CCD7TGDO5M7AKD/graph.json","fetch_events":"https://pith.science/api/pith-number/JL5UIZ6JU254CCD7TGDO5M7AKD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JL5UIZ6JU254CCD7TGDO5M7AKD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JL5UIZ6JU254CCD7TGDO5M7AKD/action/storage_attestation","attest_author":"https://pith.science/pith/JL5UIZ6JU254CCD7TGDO5M7AKD/action/author_attestation","sign_citation":"https://pith.science/pith/JL5UIZ6JU254CCD7TGDO5M7AKD/action/citation_signature","submit_replication":"https://pith.science/pith/JL5UIZ6JU254CCD7TGDO5M7AKD/action/replication_record"}},"created_at":"2026-07-05T05:06:29.153337+00:00","updated_at":"2026-07-05T05:06:29.153337+00:00"}