{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:PPNZ7F2K7OTP6MXHCNTF4JDE6F","short_pith_number":"pith:PPNZ7F2K","schema_version":"1.0","canonical_sha256":"7bdb9f974afba6ff32e713665e2464f1638dd0cea053ee5994b7ddfb1c131e4d","source":{"kind":"arxiv","id":"2111.15450","version":4},"attestation_state":"computed","paper":{"title":"Measuring the sound horizon and absolute magnitude of SNIa by maximizing the consistency between low-redshift data sets","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Adri\\`a G\\'omez-Valent","submitted_at":"2021-11-30T14:47:34Z","abstract_excerpt":"The comoving sound horizon at the baryon drag epoch, $r_{d}$, encapsulates very important physical information about the pre-recombination era and serves as a cosmic standard ruler. On the other hand, the absolute magnitude of supernovae of Type Ia (SNIa), $M$, is pivotal to infer the distances to these standard candles. Having access to (at least) one of these two quantities is crucial to measure the Hubble parameter $H_0$ from BAO/SNIa data. In this work we present a new method to measure how long is the cosmic ruler and how bright are the standard candles independently from the main drivers"},"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":"2111.15450","kind":"arxiv","version":4},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2021-11-30T14:47:34Z","cross_cats_sorted":[],"title_canon_sha256":"0b810f9191406d129b314e2096b1e421dceaef8df134aa33073bd650692651b6","abstract_canon_sha256":"a3c7f7d3c69ced6b75bdbaf90f8f96e0ea99503aeaaf7539147a6eea9e53b766"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:02:59.625371Z","signature_b64":"2EYuXLc2O4vrLGmIM0D5NlMuTMN+vazyWKLGSNgZAlmXZJTYhujkCyqVFaYltE3Y7t2Kj7XuFpmvMRCOLcDeDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7bdb9f974afba6ff32e713665e2464f1638dd0cea053ee5994b7ddfb1c131e4d","last_reissued_at":"2026-07-05T04:02:59.624804Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:02:59.624804Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Measuring the sound horizon and absolute magnitude of SNIa by maximizing the consistency between low-redshift data sets","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Adri\\`a G\\'omez-Valent","submitted_at":"2021-11-30T14:47:34Z","abstract_excerpt":"The comoving sound horizon at the baryon drag epoch, $r_{d}$, encapsulates very important physical information about the pre-recombination era and serves as a cosmic standard ruler. On the other hand, the absolute magnitude of supernovae of Type Ia (SNIa), $M$, is pivotal to infer the distances to these standard candles. Having access to (at least) one of these two quantities is crucial to measure the Hubble parameter $H_0$ from BAO/SNIa data. In this work we present a new method to measure how long is the cosmic ruler and how bright are the standard candles independently from the main drivers"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2111.15450","kind":"arxiv","version":4},"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/2111.15450/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":"2111.15450","created_at":"2026-07-05T04:02:59.624881+00:00"},{"alias_kind":"arxiv_version","alias_value":"2111.15450v4","created_at":"2026-07-05T04:02:59.624881+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2111.15450","created_at":"2026-07-05T04:02:59.624881+00:00"},{"alias_kind":"pith_short_12","alias_value":"PPNZ7F2K7OTP","created_at":"2026-07-05T04:02:59.624881+00:00"},{"alias_kind":"pith_short_16","alias_value":"PPNZ7F2K7OTP6MXH","created_at":"2026-07-05T04:02:59.624881+00:00"},{"alias_kind":"pith_short_8","alias_value":"PPNZ7F2K","created_at":"2026-07-05T04:02:59.624881+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.06959","citing_title":"KAN-LSTM-Transformer Neural Networks, MFV and Cosmological Parameters","ref_index":93,"is_internal_anchor":true},{"citing_arxiv_id":"2411.03773","citing_title":"Model-independent calibration of Gamma-Ray Bursts with neural networks","ref_index":90,"is_internal_anchor":false},{"citing_arxiv_id":"2510.04179","citing_title":"Crosschecking Cosmic Distances from DESI BAO and DES SNe","ref_index":50,"is_internal_anchor":false},{"citing_arxiv_id":"2603.26560","citing_title":"Exploring the interplay of late-time dynamical dark energy and new physics before recombination","ref_index":149,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PPNZ7F2K7OTP6MXHCNTF4JDE6F","json":"https://pith.science/pith/PPNZ7F2K7OTP6MXHCNTF4JDE6F.json","graph_json":"https://pith.science/api/pith-number/PPNZ7F2K7OTP6MXHCNTF4JDE6F/graph.json","events_json":"https://pith.science/api/pith-number/PPNZ7F2K7OTP6MXHCNTF4JDE6F/events.json","paper":"https://pith.science/paper/PPNZ7F2K"},"agent_actions":{"view_html":"https://pith.science/pith/PPNZ7F2K7OTP6MXHCNTF4JDE6F","download_json":"https://pith.science/pith/PPNZ7F2K7OTP6MXHCNTF4JDE6F.json","view_paper":"https://pith.science/paper/PPNZ7F2K","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2111.15450&json=true","fetch_graph":"https://pith.science/api/pith-number/PPNZ7F2K7OTP6MXHCNTF4JDE6F/graph.json","fetch_events":"https://pith.science/api/pith-number/PPNZ7F2K7OTP6MXHCNTF4JDE6F/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PPNZ7F2K7OTP6MXHCNTF4JDE6F/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PPNZ7F2K7OTP6MXHCNTF4JDE6F/action/storage_attestation","attest_author":"https://pith.science/pith/PPNZ7F2K7OTP6MXHCNTF4JDE6F/action/author_attestation","sign_citation":"https://pith.science/pith/PPNZ7F2K7OTP6MXHCNTF4JDE6F/action/citation_signature","submit_replication":"https://pith.science/pith/PPNZ7F2K7OTP6MXHCNTF4JDE6F/action/replication_record"}},"created_at":"2026-07-05T04:02:59.624881+00:00","updated_at":"2026-07-05T04:02:59.624881+00:00"}