{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:XULHXBAHBBAVV3VM7CW427YVTO","short_pith_number":"pith:XULHXBAH","schema_version":"1.0","canonical_sha256":"bd167b840708415aeeacf8adcd7f159b9fb196036119afa174cb6f8d658a2038","source":{"kind":"arxiv","id":"2307.12144","version":1},"attestation_state":"computed","paper":{"title":"Ideal E/IMRI vs Real E/IMRI system : Observable signature in LISA","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Prasad Basu, Sangita Chatterjee, Soumen Mondal","submitted_at":"2023-07-22T18:59:15Z","abstract_excerpt":"Real extreme/intermediate mass ratio inspiral(E/IMRI) systems are likely to contain large accretion disks which could be as massive as the central supermassive black hole. Therefore, contrary to its ideal model, a real E/IMRI system contains a third important component: the accretion disk. We study the influence of these disks on the emitted GW profile and its detectability through proposed LISA observation. We use a semi-relativistic formalism in the Kerr background (Gair & Glampedakis 2006; Barausse & Rezzolla 2008) for the case of transonic accretion flow which is a potential candidate to d"},"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":"2307.12144","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2023-07-22T18:59:15Z","cross_cats_sorted":[],"title_canon_sha256":"ef60f66a81915c7ac40a64b9ec9fb848ecac69d523788e4eb3efbe7ce5557f75","abstract_canon_sha256":"c13679a3e1b4868e698eb66fa8f140e34d9ebc2d0de2b595d49e8a0e0928bc8b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:33:50.274950Z","signature_b64":"MzokJ2d1G56vaSz84+AA7XIAXp07uzddfuG+hgkgdl2ILqlpgYPGR6ToYCgSN5rKxYHiHZoiASO6STWRwObcDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bd167b840708415aeeacf8adcd7f159b9fb196036119afa174cb6f8d658a2038","last_reissued_at":"2026-07-05T06:33:50.274407Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:33:50.274407Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Ideal E/IMRI vs Real E/IMRI system : Observable signature in LISA","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Prasad Basu, Sangita Chatterjee, Soumen Mondal","submitted_at":"2023-07-22T18:59:15Z","abstract_excerpt":"Real extreme/intermediate mass ratio inspiral(E/IMRI) systems are likely to contain large accretion disks which could be as massive as the central supermassive black hole. Therefore, contrary to its ideal model, a real E/IMRI system contains a third important component: the accretion disk. We study the influence of these disks on the emitted GW profile and its detectability through proposed LISA observation. We use a semi-relativistic formalism in the Kerr background (Gair & Glampedakis 2006; Barausse & Rezzolla 2008) for the case of transonic accretion flow which is a potential candidate to d"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2307.12144","kind":"arxiv","version":1},"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/2307.12144/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":"2307.12144","created_at":"2026-07-05T06:33:50.274489+00:00"},{"alias_kind":"arxiv_version","alias_value":"2307.12144v1","created_at":"2026-07-05T06:33:50.274489+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2307.12144","created_at":"2026-07-05T06:33:50.274489+00:00"},{"alias_kind":"pith_short_12","alias_value":"XULHXBAHBBAV","created_at":"2026-07-05T06:33:50.274489+00:00"},{"alias_kind":"pith_short_16","alias_value":"XULHXBAHBBAVV3VM","created_at":"2026-07-05T06:33:50.274489+00:00"},{"alias_kind":"pith_short_8","alias_value":"XULHXBAH","created_at":"2026-07-05T06:33:50.274489+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.10942","citing_title":"Probing Active Galactic Nuclei and Measuring the Hubble constant with Extreme-Mass-Ratio Inspirals","ref_index":19,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XULHXBAHBBAVV3VM7CW427YVTO","json":"https://pith.science/pith/XULHXBAHBBAVV3VM7CW427YVTO.json","graph_json":"https://pith.science/api/pith-number/XULHXBAHBBAVV3VM7CW427YVTO/graph.json","events_json":"https://pith.science/api/pith-number/XULHXBAHBBAVV3VM7CW427YVTO/events.json","paper":"https://pith.science/paper/XULHXBAH"},"agent_actions":{"view_html":"https://pith.science/pith/XULHXBAHBBAVV3VM7CW427YVTO","download_json":"https://pith.science/pith/XULHXBAHBBAVV3VM7CW427YVTO.json","view_paper":"https://pith.science/paper/XULHXBAH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2307.12144&json=true","fetch_graph":"https://pith.science/api/pith-number/XULHXBAHBBAVV3VM7CW427YVTO/graph.json","fetch_events":"https://pith.science/api/pith-number/XULHXBAHBBAVV3VM7CW427YVTO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XULHXBAHBBAVV3VM7CW427YVTO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XULHXBAHBBAVV3VM7CW427YVTO/action/storage_attestation","attest_author":"https://pith.science/pith/XULHXBAHBBAVV3VM7CW427YVTO/action/author_attestation","sign_citation":"https://pith.science/pith/XULHXBAHBBAVV3VM7CW427YVTO/action/citation_signature","submit_replication":"https://pith.science/pith/XULHXBAHBBAVV3VM7CW427YVTO/action/replication_record"}},"created_at":"2026-07-05T06:33:50.274489+00:00","updated_at":"2026-07-05T06:33:50.274489+00:00"}