{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2003:DMX4CX5ZA52PAXC5XHD3G4TR53","short_pith_number":"pith:DMX4CX5Z","schema_version":"1.0","canonical_sha256":"1b2fc15fb90774f05c5db9c7b37271eecd67ee2daaa9ee354c72bf76db53af51","source":{"kind":"arxiv","id":"hep-th/0305161","version":2},"attestation_state":"computed","paper":{"title":"On the Dependence of the Spectra of Fluctuations in Inflationary Cosmology on Trans-Planckian Physics","license":"","headline":"","cross_cats":["astro-ph","gr-qc","hep-ph"],"primary_cat":"hep-th","authors_text":"Jerome Martin, R. H. Brandenberger","submitted_at":"2003-05-19T16:39:14Z","abstract_excerpt":"We calculate the power spectrum of metric fluctuations in inflationary cosmology starting with initial conditions which are imposed mode by mode when the wavelength equals some critical length $\\ell_{_{\\rm C}}$ corresponding to a new energy scale $M_{_{\\rm C}}$ at which trans-Planckian physics becomes important. In this case, the power spectrum can differ from what is calculated in the usual framework (which amounts to choosing the adiabatic vacuum state). The fractional difference in the results depends on the ratio $\\sigma_0$ between the Hubble expansion rate $H_{\\rm inf}$ during inflation a"},"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":"hep-th/0305161","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"hep-th","submitted_at":"2003-05-19T16:39:14Z","cross_cats_sorted":["astro-ph","gr-qc","hep-ph"],"title_canon_sha256":"947a1812c766a525d61b250a287317a5845213f44125e97390c9c7300a757c60","abstract_canon_sha256":"d8e9c457a67598d19403e158a3dd1d58c949de9a2e1155e8a78b8431b6bd348f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:41:16.292822Z","signature_b64":"2o1t2TpZ4NapT+ICiXZe7mUy1pL9DGOU5Hw+n254JdqqCHIX+AQ+VD53y0J2ILSS6TAnUmlp/po6IqL88ptiDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1b2fc15fb90774f05c5db9c7b37271eecd67ee2daaa9ee354c72bf76db53af51","last_reissued_at":"2026-07-04T16:41:16.292497Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:41:16.292497Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"On the Dependence of the Spectra of Fluctuations in Inflationary Cosmology on Trans-Planckian Physics","license":"","headline":"","cross_cats":["astro-ph","gr-qc","hep-ph"],"primary_cat":"hep-th","authors_text":"Jerome Martin, R. H. Brandenberger","submitted_at":"2003-05-19T16:39:14Z","abstract_excerpt":"We calculate the power spectrum of metric fluctuations in inflationary cosmology starting with initial conditions which are imposed mode by mode when the wavelength equals some critical length $\\ell_{_{\\rm C}}$ corresponding to a new energy scale $M_{_{\\rm C}}$ at which trans-Planckian physics becomes important. In this case, the power spectrum can differ from what is calculated in the usual framework (which amounts to choosing the adiabatic vacuum state). The fractional difference in the results depends on the ratio $\\sigma_0$ between the Hubble expansion rate $H_{\\rm inf}$ during inflation a"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"hep-th/0305161","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/hep-th/0305161/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":"hep-th/0305161","created_at":"2026-07-04T16:41:16.292549+00:00"},{"alias_kind":"arxiv_version","alias_value":"hep-th/0305161v2","created_at":"2026-07-04T16:41:16.292549+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.hep-th/0305161","created_at":"2026-07-04T16:41:16.292549+00:00"},{"alias_kind":"pith_short_12","alias_value":"DMX4CX5ZA52P","created_at":"2026-07-04T16:41:16.292549+00:00"},{"alias_kind":"pith_short_16","alias_value":"DMX4CX5ZA52PAXC5","created_at":"2026-07-04T16:41:16.292549+00:00"},{"alias_kind":"pith_short_8","alias_value":"DMX4CX5Z","created_at":"2026-07-04T16:41:16.292549+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2606.28310","citing_title":"Constraining primordial oscillations and inflationary particle production with Planck, ACT DR6, and DESI DR2","ref_index":21,"is_internal_anchor":true},{"citing_arxiv_id":"2605.18615","citing_title":"Primordial power spectrum reconstructions from BOSS + eBOSS","ref_index":14,"is_internal_anchor":true},{"citing_arxiv_id":"2605.19336","citing_title":"Recombination Thickness as an Uncertainty in Inflationary Observables","ref_index":26,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/DMX4CX5ZA52PAXC5XHD3G4TR53","json":"https://pith.science/pith/DMX4CX5ZA52PAXC5XHD3G4TR53.json","graph_json":"https://pith.science/api/pith-number/DMX4CX5ZA52PAXC5XHD3G4TR53/graph.json","events_json":"https://pith.science/api/pith-number/DMX4CX5ZA52PAXC5XHD3G4TR53/events.json","paper":"https://pith.science/paper/DMX4CX5Z"},"agent_actions":{"view_html":"https://pith.science/pith/DMX4CX5ZA52PAXC5XHD3G4TR53","download_json":"https://pith.science/pith/DMX4CX5ZA52PAXC5XHD3G4TR53.json","view_paper":"https://pith.science/paper/DMX4CX5Z","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=hep-th/0305161&json=true","fetch_graph":"https://pith.science/api/pith-number/DMX4CX5ZA52PAXC5XHD3G4TR53/graph.json","fetch_events":"https://pith.science/api/pith-number/DMX4CX5ZA52PAXC5XHD3G4TR53/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DMX4CX5ZA52PAXC5XHD3G4TR53/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DMX4CX5ZA52PAXC5XHD3G4TR53/action/storage_attestation","attest_author":"https://pith.science/pith/DMX4CX5ZA52PAXC5XHD3G4TR53/action/author_attestation","sign_citation":"https://pith.science/pith/DMX4CX5ZA52PAXC5XHD3G4TR53/action/citation_signature","submit_replication":"https://pith.science/pith/DMX4CX5ZA52PAXC5XHD3G4TR53/action/replication_record"}},"created_at":"2026-07-04T16:41:16.292549+00:00","updated_at":"2026-07-04T16:41:16.292549+00:00"}