{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:S2XDUYHQ7X4KWFFUX2TYPYFRUZ","short_pith_number":"pith:S2XDUYHQ","schema_version":"1.0","canonical_sha256":"96ae3a60f0fdf8ab14b4bea787e0b1a65a9e1428e30b1f68e20c07b12c9474e3","source":{"kind":"arxiv","id":"2407.18976","version":3},"attestation_state":"computed","paper":{"title":"Obviating PBH overproduction for SIGWs generated by Pulsar Timing Arrays in loop corrected EFT of bounce","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Pranjal Tiwari, Sayantan Choudhury, Siddhant Ganguly, Soumitra SenGupta, Sudhakar Panda","submitted_at":"2024-07-22T14:06:25Z","abstract_excerpt":"In order to unravel the present situation of the PBH overproduction problem, our study emphasizes the critical role played by the equation of state (EoS) parameter $w$ within the framework of effective field theory (EFT) of non-singular bounce. Our analysis focuses on a wide range of EoS parameter values that are still optimal for explaining the latest data from the pulsar timing array (PTA). As a result of our study, the most advantageous window, $0.31 \\leq w \\leq 1/3$, is identified as the location of a substantial PBH abundance, $f_{\\rm PBH} \\in (10^{-3},1)$ with large mass PBHs, $M_{\\rm PB"},"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":"2407.18976","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2024-07-22T14:06:25Z","cross_cats_sorted":["gr-qc","hep-ph","hep-th"],"title_canon_sha256":"9b24923ed368954e717d8e4159c3eb7e478314a90b370d797cfcb2751dc0d484","abstract_canon_sha256":"44bcb25d5a8d0fcb639dcffc985c6b37f7244b9bc6a3be81beaa9c565efabf3f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:03:01.707756Z","signature_b64":"XMyeofLxpiXsUHb6+6m5Utqw4wX+oumR2mIj3uEnJiQzSRjiBTYYCLuveOTsmcPbc1PZ+4fsNKVpx8UagE8JAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"96ae3a60f0fdf8ab14b4bea787e0b1a65a9e1428e30b1f68e20c07b12c9474e3","last_reissued_at":"2026-07-05T09:03:01.707189Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:03:01.707189Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Obviating PBH overproduction for SIGWs generated by Pulsar Timing Arrays in loop corrected EFT of bounce","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Pranjal Tiwari, Sayantan Choudhury, Siddhant Ganguly, Soumitra SenGupta, Sudhakar Panda","submitted_at":"2024-07-22T14:06:25Z","abstract_excerpt":"In order to unravel the present situation of the PBH overproduction problem, our study emphasizes the critical role played by the equation of state (EoS) parameter $w$ within the framework of effective field theory (EFT) of non-singular bounce. Our analysis focuses on a wide range of EoS parameter values that are still optimal for explaining the latest data from the pulsar timing array (PTA). As a result of our study, the most advantageous window, $0.31 \\leq w \\leq 1/3$, is identified as the location of a substantial PBH abundance, $f_{\\rm PBH} \\in (10^{-3},1)$ with large mass PBHs, $M_{\\rm PB"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2407.18976","kind":"arxiv","version":3},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2407.18976/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"2407.18976","created_at":"2026-07-05T09:03:01.707260+00:00"},{"alias_kind":"arxiv_version","alias_value":"2407.18976v3","created_at":"2026-07-05T09:03:01.707260+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2407.18976","created_at":"2026-07-05T09:03:01.707260+00:00"},{"alias_kind":"pith_short_12","alias_value":"S2XDUYHQ7X4K","created_at":"2026-07-05T09:03:01.707260+00:00"},{"alias_kind":"pith_short_16","alias_value":"S2XDUYHQ7X4KWFFU","created_at":"2026-07-05T09:03:01.707260+00:00"},{"alias_kind":"pith_short_8","alias_value":"S2XDUYHQ","created_at":"2026-07-05T09:03:01.707260+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.06355","citing_title":"$\\tt BlackHawk$ $\\tt v3.0$: Hawking Radiation from Regular Black Holes","ref_index":176,"is_internal_anchor":false},{"citing_arxiv_id":"2505.16820","citing_title":"Isotropy, anisotropies and non-Gaussianity in the scalar-induced gravitational-wave background: diagrammatic approach for primordial non-Gaussianity up to arbitrary order","ref_index":294,"is_internal_anchor":false},{"citing_arxiv_id":"2604.20063","citing_title":"Purely quadratic non-Gaussianity from tachyonic instability: Primordial black holes and scalar-induced gravitational waves","ref_index":113,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/S2XDUYHQ7X4KWFFUX2TYPYFRUZ","json":"https://pith.science/pith/S2XDUYHQ7X4KWFFUX2TYPYFRUZ.json","graph_json":"https://pith.science/api/pith-number/S2XDUYHQ7X4KWFFUX2TYPYFRUZ/graph.json","events_json":"https://pith.science/api/pith-number/S2XDUYHQ7X4KWFFUX2TYPYFRUZ/events.json","paper":"https://pith.science/paper/S2XDUYHQ"},"agent_actions":{"view_html":"https://pith.science/pith/S2XDUYHQ7X4KWFFUX2TYPYFRUZ","download_json":"https://pith.science/pith/S2XDUYHQ7X4KWFFUX2TYPYFRUZ.json","view_paper":"https://pith.science/paper/S2XDUYHQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2407.18976&json=true","fetch_graph":"https://pith.science/api/pith-number/S2XDUYHQ7X4KWFFUX2TYPYFRUZ/graph.json","fetch_events":"https://pith.science/api/pith-number/S2XDUYHQ7X4KWFFUX2TYPYFRUZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/S2XDUYHQ7X4KWFFUX2TYPYFRUZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/S2XDUYHQ7X4KWFFUX2TYPYFRUZ/action/storage_attestation","attest_author":"https://pith.science/pith/S2XDUYHQ7X4KWFFUX2TYPYFRUZ/action/author_attestation","sign_citation":"https://pith.science/pith/S2XDUYHQ7X4KWFFUX2TYPYFRUZ/action/citation_signature","submit_replication":"https://pith.science/pith/S2XDUYHQ7X4KWFFUX2TYPYFRUZ/action/replication_record"}},"created_at":"2026-07-05T09:03:01.707260+00:00","updated_at":"2026-07-05T09:03:01.707260+00:00"}