{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:IHRMLHLQTWKXVTGAS7NVVSTNRM","short_pith_number":"pith:IHRMLHLQ","schema_version":"1.0","canonical_sha256":"41e2c59d709d957accc097db5aca6d8b3a6ad0cae2e696f6dccd574f850f30fa","source":{"kind":"arxiv","id":"0904.2518","version":2},"attestation_state":"computed","paper":{"title":"The tensor-to-scalar ratio in punctuated inflation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Allahabad), L. Sriramkumar (HRI, Pravabati Chingangbam (KIAS, Pune), Rajeev Kumar Jain (HRI, Seoul), Tarun Souradeep (IUCAA","submitted_at":"2009-04-16T15:20:09Z","abstract_excerpt":"Recently, we have shown that scalar spectra with lower power on large scales and certain other features naturally occur in {\\it punctuated inflation}, i.e. the scenario wherein a brief period of rapid roll is sandwiched between two stages of slow roll inflation. Such spectra gain importance due to the fact that they can lead to a better fit of the observed Cosmic Microwave Background (CMB) anisotropies, when compared to the conventional, featureless, power law spectrum. In this paper, with examples from the canonical scalar field as well as the tachyonic models, we illustrate that, in punctuat"},"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":"0904.2518","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-04-16T15:20:09Z","cross_cats_sorted":["gr-qc","hep-th"],"title_canon_sha256":"ecd7341af8182512e26a17341c21851a39f1dbba8fbeb34e31173c00a71890b0","abstract_canon_sha256":"bcbb1be49c9d4aecb1d31762a2bd2f898947132cfb997239330a6996bc0627ab"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:34:59.695940Z","signature_b64":"3IPx6N2Tkn75bBKbhDNSEYlZuMV1bwHpSixoRisHVve4GOf5yKUiyadLHMI1689ymnLG9oY01p3CRgNX98r4Cw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"41e2c59d709d957accc097db5aca6d8b3a6ad0cae2e696f6dccd574f850f30fa","last_reissued_at":"2026-05-18T02:34:59.695571Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:34:59.695571Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The tensor-to-scalar ratio in punctuated inflation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Allahabad), L. Sriramkumar (HRI, Pravabati Chingangbam (KIAS, Pune), Rajeev Kumar Jain (HRI, Seoul), Tarun Souradeep (IUCAA","submitted_at":"2009-04-16T15:20:09Z","abstract_excerpt":"Recently, we have shown that scalar spectra with lower power on large scales and certain other features naturally occur in {\\it punctuated inflation}, i.e. the scenario wherein a brief period of rapid roll is sandwiched between two stages of slow roll inflation. Such spectra gain importance due to the fact that they can lead to a better fit of the observed Cosmic Microwave Background (CMB) anisotropies, when compared to the conventional, featureless, power law spectrum. In this paper, with examples from the canonical scalar field as well as the tachyonic models, we illustrate that, in punctuat"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0904.2518","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":""},"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":"0904.2518","created_at":"2026-05-18T02:34:59.695628+00:00"},{"alias_kind":"arxiv_version","alias_value":"0904.2518v2","created_at":"2026-05-18T02:34:59.695628+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0904.2518","created_at":"2026-05-18T02:34:59.695628+00:00"},{"alias_kind":"pith_short_12","alias_value":"IHRMLHLQTWKX","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_16","alias_value":"IHRMLHLQTWKXVTGA","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_8","alias_value":"IHRMLHLQ","created_at":"2026-05-18T12:26:00.592388+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2505.10534","citing_title":"ACT-ing on inflation: Implications of non Bunch-Davies initial condition and reheating on single-field slow roll models","ref_index":55,"is_internal_anchor":true},{"citing_arxiv_id":"2604.13547","citing_title":"Reconstructing inflationary features on large scales using genetic algorithm","ref_index":33,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/IHRMLHLQTWKXVTGAS7NVVSTNRM","json":"https://pith.science/pith/IHRMLHLQTWKXVTGAS7NVVSTNRM.json","graph_json":"https://pith.science/api/pith-number/IHRMLHLQTWKXVTGAS7NVVSTNRM/graph.json","events_json":"https://pith.science/api/pith-number/IHRMLHLQTWKXVTGAS7NVVSTNRM/events.json","paper":"https://pith.science/paper/IHRMLHLQ"},"agent_actions":{"view_html":"https://pith.science/pith/IHRMLHLQTWKXVTGAS7NVVSTNRM","download_json":"https://pith.science/pith/IHRMLHLQTWKXVTGAS7NVVSTNRM.json","view_paper":"https://pith.science/paper/IHRMLHLQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0904.2518&json=true","fetch_graph":"https://pith.science/api/pith-number/IHRMLHLQTWKXVTGAS7NVVSTNRM/graph.json","fetch_events":"https://pith.science/api/pith-number/IHRMLHLQTWKXVTGAS7NVVSTNRM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/IHRMLHLQTWKXVTGAS7NVVSTNRM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/IHRMLHLQTWKXVTGAS7NVVSTNRM/action/storage_attestation","attest_author":"https://pith.science/pith/IHRMLHLQTWKXVTGAS7NVVSTNRM/action/author_attestation","sign_citation":"https://pith.science/pith/IHRMLHLQTWKXVTGAS7NVVSTNRM/action/citation_signature","submit_replication":"https://pith.science/pith/IHRMLHLQTWKXVTGAS7NVVSTNRM/action/replication_record"}},"created_at":"2026-05-18T02:34:59.695628+00:00","updated_at":"2026-05-18T02:34:59.695628+00:00"}