{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:XWKPBNK3JSRHIN53ROQKQCA6DU","short_pith_number":"pith:XWKPBNK3","schema_version":"1.0","canonical_sha256":"bd94f0b55b4ca27437bb8ba0a8081e1d3279f07c878f0efebc79d17c357a2b58","source":{"kind":"arxiv","id":"2204.03614","version":2},"attestation_state":"computed","paper":{"title":"Impact of calibration uncertainties on Hubble constant measurements from gravitational-wave sources","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Carl-Johan Haster, Hsin-Yu Chen, Jeffrey S. Kissel, Ling Sun, Salvatore Vitale, Yiwen Huang","submitted_at":"2022-04-07T17:37:55Z","abstract_excerpt":"Gravitational-wave (GW) detections of electromagnetically bright compact binary coalescences can provide an independent measurement of the Hubble constant $H_0$. In order to obtain a measurement that could help arbitrate the existing tension on $H_0$, one needs to fully understand any source of systematic biases for this approach. In this study, we aim to understand the impact of instrumental calibration errors (CEs) on the measurements of the luminosity distance, $D_L$, and the inferred $H_0$ value. We simulate binary neutron star mergers (BNSs), as detected by a network of Advanced LIGO and "},"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":"2204.03614","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2022-04-07T17:37:55Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"89ff29f68bce7161f542cd9edb208f7bec2e0e0c6b9e073868c2b4f6008fec2a","abstract_canon_sha256":"77d31bba98697c4d244b8f63e61a9fd5a4784b4d9b2898ce0480655d65e94371"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:29:59.652602Z","signature_b64":"iarxEmcYte2R5Go+aQ8aqdluDEy/GYzmRgHektth9vbxJEYgvNWzdN52GXBhBXV3f452MLZp3n8JskjJNQYtDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bd94f0b55b4ca27437bb8ba0a8081e1d3279f07c878f0efebc79d17c357a2b58","last_reissued_at":"2026-07-05T10:29:59.652065Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:29:59.652065Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Impact of calibration uncertainties on Hubble constant measurements from gravitational-wave sources","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Carl-Johan Haster, Hsin-Yu Chen, Jeffrey S. Kissel, Ling Sun, Salvatore Vitale, Yiwen Huang","submitted_at":"2022-04-07T17:37:55Z","abstract_excerpt":"Gravitational-wave (GW) detections of electromagnetically bright compact binary coalescences can provide an independent measurement of the Hubble constant $H_0$. In order to obtain a measurement that could help arbitrate the existing tension on $H_0$, one needs to fully understand any source of systematic biases for this approach. In this study, we aim to understand the impact of instrumental calibration errors (CEs) on the measurements of the luminosity distance, $D_L$, and the inferred $H_0$ value. We simulate binary neutron star mergers (BNSs), as detected by a network of Advanced LIGO and "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2204.03614","kind":"arxiv","version":2},"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/2204.03614/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":"2204.03614","created_at":"2026-07-05T10:29:59.652131+00:00"},{"alias_kind":"arxiv_version","alias_value":"2204.03614v2","created_at":"2026-07-05T10:29:59.652131+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2204.03614","created_at":"2026-07-05T10:29:59.652131+00:00"},{"alias_kind":"pith_short_12","alias_value":"XWKPBNK3JSRH","created_at":"2026-07-05T10:29:59.652131+00:00"},{"alias_kind":"pith_short_16","alias_value":"XWKPBNK3JSRHIN53","created_at":"2026-07-05T10:29:59.652131+00:00"},{"alias_kind":"pith_short_8","alias_value":"XWKPBNK3","created_at":"2026-07-05T10:29:59.652131+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.11703","citing_title":"GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors","ref_index":22,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XWKPBNK3JSRHIN53ROQKQCA6DU","json":"https://pith.science/pith/XWKPBNK3JSRHIN53ROQKQCA6DU.json","graph_json":"https://pith.science/api/pith-number/XWKPBNK3JSRHIN53ROQKQCA6DU/graph.json","events_json":"https://pith.science/api/pith-number/XWKPBNK3JSRHIN53ROQKQCA6DU/events.json","paper":"https://pith.science/paper/XWKPBNK3"},"agent_actions":{"view_html":"https://pith.science/pith/XWKPBNK3JSRHIN53ROQKQCA6DU","download_json":"https://pith.science/pith/XWKPBNK3JSRHIN53ROQKQCA6DU.json","view_paper":"https://pith.science/paper/XWKPBNK3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2204.03614&json=true","fetch_graph":"https://pith.science/api/pith-number/XWKPBNK3JSRHIN53ROQKQCA6DU/graph.json","fetch_events":"https://pith.science/api/pith-number/XWKPBNK3JSRHIN53ROQKQCA6DU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XWKPBNK3JSRHIN53ROQKQCA6DU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XWKPBNK3JSRHIN53ROQKQCA6DU/action/storage_attestation","attest_author":"https://pith.science/pith/XWKPBNK3JSRHIN53ROQKQCA6DU/action/author_attestation","sign_citation":"https://pith.science/pith/XWKPBNK3JSRHIN53ROQKQCA6DU/action/citation_signature","submit_replication":"https://pith.science/pith/XWKPBNK3JSRHIN53ROQKQCA6DU/action/replication_record"}},"created_at":"2026-07-05T10:29:59.652131+00:00","updated_at":"2026-07-05T10:29:59.652131+00:00"}