{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:MJ5IAXHZ4FA3NILZH72JJRYTOZ","short_pith_number":"pith:MJ5IAXHZ","schema_version":"1.0","canonical_sha256":"627a805cf9e141b6a1793ff494c71376509511bfd00578800262d6c945f0ac3c","source":{"kind":"arxiv","id":"2306.12468","version":2},"attestation_state":"computed","paper":{"title":"Measuring the Hubble constant with kilonovae using the Expanding Photosphere Method","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"Albert Sneppen, Andreas Bauswein, Darach Watson, Dovi Poznanski, Oliver Just, Rados{\\l}aw Wojtak","submitted_at":"2023-06-21T18:00:00Z","abstract_excerpt":"While gravitational wave (GW) standard sirens from neutron star (NS) mergers have been proposed to offer good measurements of the Hubble constant, we show in this paper how a variation of the expanding photosphere method (EPM) or spectral-fitting expanding atmosphere method, applied to the kilonovae (KNe) associated with the mergers, can provide an independent distance measurement to individual mergers that is potentially accurate to within a few percent. There are four reasons why the KN-EPM overcomes the major uncertainties commonly associated with this method in supernovae: 1) the early con"},"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":"2306.12468","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2023-06-21T18:00:00Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"8e9f1f96cb81f8fe6f5fe0e818965f19a746d1b49c60e14a85c45714da749137","abstract_canon_sha256":"6a36402655bf06b89d229267b45b88f82cde6617153319eb8569b81a2afa89b6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:56:34.823724Z","signature_b64":"B+SqONu1jLvpb4LZEX1g4L+mzZKnup/99FwVULujrc+bz29EZ8mlac5XDCfbEjrMTFndrc+SWcXaGaWuRxEpBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"627a805cf9e141b6a1793ff494c71376509511bfd00578800262d6c945f0ac3c","last_reissued_at":"2026-07-05T06:56:34.823246Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:56:34.823246Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Measuring the Hubble constant with kilonovae using the Expanding Photosphere Method","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"Albert Sneppen, Andreas Bauswein, Darach Watson, Dovi Poznanski, Oliver Just, Rados{\\l}aw Wojtak","submitted_at":"2023-06-21T18:00:00Z","abstract_excerpt":"While gravitational wave (GW) standard sirens from neutron star (NS) mergers have been proposed to offer good measurements of the Hubble constant, we show in this paper how a variation of the expanding photosphere method (EPM) or spectral-fitting expanding atmosphere method, applied to the kilonovae (KNe) associated with the mergers, can provide an independent distance measurement to individual mergers that is potentially accurate to within a few percent. There are four reasons why the KN-EPM overcomes the major uncertainties commonly associated with this method in supernovae: 1) the early con"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2306.12468","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/2306.12468/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":"2306.12468","created_at":"2026-07-05T06:56:34.823302+00:00"},{"alias_kind":"arxiv_version","alias_value":"2306.12468v2","created_at":"2026-07-05T06:56:34.823302+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2306.12468","created_at":"2026-07-05T06:56:34.823302+00:00"},{"alias_kind":"pith_short_12","alias_value":"MJ5IAXHZ4FA3","created_at":"2026-07-05T06:56:34.823302+00:00"},{"alias_kind":"pith_short_16","alias_value":"MJ5IAXHZ4FA3NILZ","created_at":"2026-07-05T06:56:34.823302+00:00"},{"alias_kind":"pith_short_8","alias_value":"MJ5IAXHZ","created_at":"2026-07-05T06:56:34.823302+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2505.08856","citing_title":"Expanding Ejecta Method: II. Framework for Cosmological Distance Measurements via Intensity Interferometry","ref_index":48,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MJ5IAXHZ4FA3NILZH72JJRYTOZ","json":"https://pith.science/pith/MJ5IAXHZ4FA3NILZH72JJRYTOZ.json","graph_json":"https://pith.science/api/pith-number/MJ5IAXHZ4FA3NILZH72JJRYTOZ/graph.json","events_json":"https://pith.science/api/pith-number/MJ5IAXHZ4FA3NILZH72JJRYTOZ/events.json","paper":"https://pith.science/paper/MJ5IAXHZ"},"agent_actions":{"view_html":"https://pith.science/pith/MJ5IAXHZ4FA3NILZH72JJRYTOZ","download_json":"https://pith.science/pith/MJ5IAXHZ4FA3NILZH72JJRYTOZ.json","view_paper":"https://pith.science/paper/MJ5IAXHZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2306.12468&json=true","fetch_graph":"https://pith.science/api/pith-number/MJ5IAXHZ4FA3NILZH72JJRYTOZ/graph.json","fetch_events":"https://pith.science/api/pith-number/MJ5IAXHZ4FA3NILZH72JJRYTOZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MJ5IAXHZ4FA3NILZH72JJRYTOZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MJ5IAXHZ4FA3NILZH72JJRYTOZ/action/storage_attestation","attest_author":"https://pith.science/pith/MJ5IAXHZ4FA3NILZH72JJRYTOZ/action/author_attestation","sign_citation":"https://pith.science/pith/MJ5IAXHZ4FA3NILZH72JJRYTOZ/action/citation_signature","submit_replication":"https://pith.science/pith/MJ5IAXHZ4FA3NILZH72JJRYTOZ/action/replication_record"}},"created_at":"2026-07-05T06:56:34.823302+00:00","updated_at":"2026-07-05T06:56:34.823302+00:00"}