{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:FWNNFHMS73OSR2DDAI6MOLTBB6","short_pith_number":"pith:FWNNFHMS","schema_version":"1.0","canonical_sha256":"2d9ad29d92fedd28e863023cc72e610f84bbce5c9e22c02511db9aa58e473704","source":{"kind":"arxiv","id":"2309.10841","version":2},"attestation_state":"computed","paper":{"title":"Cosmological Collider Signatures of Higgs-$R^2$ Inflation","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"hep-ph","authors_text":"Sarunas Verner, Yohei Ema","submitted_at":"2023-09-19T18:00:01Z","abstract_excerpt":"We study the cosmological collider signatures in the Higgs-$R^2$ inflation model. We consider two distinct types of signals: one originating from the inflaton coupling to Standard Model fermions and gauge bosons, and another arising from the isocurvature mode interaction with the inflaton. In the former case, we determine that the signal magnitude is likely too small for detection by upcoming probes, primarily due to suppression by both the Planck scale and slow-roll parameters. However, we provide a detailed computation of the signal which could be potentially applicable to various Higgs infl"},"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":"2309.10841","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"hep-ph","submitted_at":"2023-09-19T18:00:01Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"51a5d87b8d1cc7789eab1caa16f0c04f19f3ccec9f751dd64fe338f3871139c3","abstract_canon_sha256":"2082bde72d1a5a758e68d608e6d886f5189c54a889b023d1b45709ddbbdb140f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:49:14.646860Z","signature_b64":"4UYzdtu9C4ZbufI0XfF85AltC0TZ8/zQCgF6TfFqBNkzH/sqQ7jOa07RZTxGjpPNzdjJL/uLEzPIY8gF+BF7BA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2d9ad29d92fedd28e863023cc72e610f84bbce5c9e22c02511db9aa58e473704","last_reissued_at":"2026-07-05T07:49:14.646393Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:49:14.646393Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Cosmological Collider Signatures of Higgs-$R^2$ Inflation","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"hep-ph","authors_text":"Sarunas Verner, Yohei Ema","submitted_at":"2023-09-19T18:00:01Z","abstract_excerpt":"We study the cosmological collider signatures in the Higgs-$R^2$ inflation model. We consider two distinct types of signals: one originating from the inflaton coupling to Standard Model fermions and gauge bosons, and another arising from the isocurvature mode interaction with the inflaton. In the former case, we determine that the signal magnitude is likely too small for detection by upcoming probes, primarily due to suppression by both the Planck scale and slow-roll parameters. However, we provide a detailed computation of the signal which could be potentially applicable to various Higgs infl"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2309.10841","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/2309.10841/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":"2309.10841","created_at":"2026-07-05T07:49:14.646457+00:00"},{"alias_kind":"arxiv_version","alias_value":"2309.10841v2","created_at":"2026-07-05T07:49:14.646457+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2309.10841","created_at":"2026-07-05T07:49:14.646457+00:00"},{"alias_kind":"pith_short_12","alias_value":"FWNNFHMS73OS","created_at":"2026-07-05T07:49:14.646457+00:00"},{"alias_kind":"pith_short_16","alias_value":"FWNNFHMS73OSR2DD","created_at":"2026-07-05T07:49:14.646457+00:00"},{"alias_kind":"pith_short_8","alias_value":"FWNNFHMS","created_at":"2026-07-05T07:49:14.646457+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.28054","citing_title":"Fermionic Bubble Loop in Cosmological Collider Revisited: Exact signals from spectral and Mellin-Barnes methods","ref_index":27,"is_internal_anchor":false},{"citing_arxiv_id":"2509.21148","citing_title":"Scalaron dark matter dynamics: effects of Higgs non-minimal coupling to gravity","ref_index":27,"is_internal_anchor":false},{"citing_arxiv_id":"2604.05548","citing_title":"Cosmological collider signals of modular spontaneous CP breaking","ref_index":33,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FWNNFHMS73OSR2DDAI6MOLTBB6","json":"https://pith.science/pith/FWNNFHMS73OSR2DDAI6MOLTBB6.json","graph_json":"https://pith.science/api/pith-number/FWNNFHMS73OSR2DDAI6MOLTBB6/graph.json","events_json":"https://pith.science/api/pith-number/FWNNFHMS73OSR2DDAI6MOLTBB6/events.json","paper":"https://pith.science/paper/FWNNFHMS"},"agent_actions":{"view_html":"https://pith.science/pith/FWNNFHMS73OSR2DDAI6MOLTBB6","download_json":"https://pith.science/pith/FWNNFHMS73OSR2DDAI6MOLTBB6.json","view_paper":"https://pith.science/paper/FWNNFHMS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2309.10841&json=true","fetch_graph":"https://pith.science/api/pith-number/FWNNFHMS73OSR2DDAI6MOLTBB6/graph.json","fetch_events":"https://pith.science/api/pith-number/FWNNFHMS73OSR2DDAI6MOLTBB6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FWNNFHMS73OSR2DDAI6MOLTBB6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FWNNFHMS73OSR2DDAI6MOLTBB6/action/storage_attestation","attest_author":"https://pith.science/pith/FWNNFHMS73OSR2DDAI6MOLTBB6/action/author_attestation","sign_citation":"https://pith.science/pith/FWNNFHMS73OSR2DDAI6MOLTBB6/action/citation_signature","submit_replication":"https://pith.science/pith/FWNNFHMS73OSR2DDAI6MOLTBB6/action/replication_record"}},"created_at":"2026-07-05T07:49:14.646457+00:00","updated_at":"2026-07-05T07:49:14.646457+00:00"}