{"as_of":"2026-08-11T17:27:00Z","caps":{"database_statements":6,"inbound":100,"outbound":100},"context_digest":"sha256:50a208af9ef760c24c7f4829f173dd933306861d41b2b8cfbe13d3ba28b21c3a","coverage":[{"denominator":0,"lane":"reference_resolution","note":"Typed states for the displayed outbound observations.","records_observed":0,"source":"paper_references, paper_reference_links","source_observed_at":null,"state":"measured"},{"denominator":11,"lane":"standing_notices","note":"One-hop event checks from named stored sources.","records_observed":11,"source":"scholarly_work_events, retraction_status_cache","source_observed_at":"2026-08-11T06:34:44.6726+00:00","state":"measured"},{"denominator":11,"lane":"inbound_itemization","note":"Pith citing papers itemized under the disclosed page cap.","records_observed":11,"source":"paper_references, paper_reference_links","source_observed_at":"2026-08-10T13:27:10.489491Z","state":"measured"},{"denominator":1,"lane":"external_citation_measurements","note":"A source-named dated measurement, never combined with another source.","records_observed":0,"source":"arxiv_reference","source_observed_at":"2026-07-04T11:59:51.914279Z","state":"measured"}],"external_citation_measurements":[],"inbound":[{"citation":{"cited_paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","version":2},"cited_work":{"arxiv_id":null,"doi":null,"metadata_source":null,"pith_arxiv_id":"2403.09767","snapshot_observed_at":"2026-08-10T13:27:10.489491Z","title":"Nonlinear quasinormal mode detectabil- ity with next-generation gravitational wave detectors,","venue":null,"work_id":null,"year":2024},"citing_paper":{"arxiv_id":"2501.16422","last_updated":"2025-03-26T13:39:24Z","snapshot_observed_at":"2026-08-11T02:35:26.695721Z","submitted_at":"2025-01-27T19:00:01Z","title":"Gravitational wave inference of star cluster properties from intermediate-mass black hole mergers","version":2},"reference_index":78,"source":"pdf_text","source_observed_at":"2026-08-10T13:27:10.489491Z"},"links":{"cited_paper":"/paper/2403.09767","citing_paper":"/paper/2501.16422"},"observation_digest":"sha256:94cd271d05bd67ce642812e9ab810a95f87f4c9b0b6c9260fb91c63a5d8e44d5","observation_id":"670b5a0b-d863-4899-90d8-a39acb764ecd","resolution":{"observed_at":"2026-08-10T13:27:10.489491Z","resolver_source":null,"status":"unresolved"},"standing_notice":{"events":[],"reason":"canonical_work_link_unavailable","source_receipts":[],"state":"unavailable"}},{"citation":{"cited_paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","version":2},"cited_work":{"arxiv_id":"2403.09767","doi":null,"metadata_source":"arxiv_reference","pith_arxiv_id":"2403.09767","snapshot_observed_at":"2026-07-04T11:59:51.914279Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","venue":null,"work_id":"5e6a86cf-049c-4890-aafe-cd41e5ad6c89","year":2024},"citing_paper":{"arxiv_id":"2501.16433","last_updated":"2026-05-13T15:28:20Z","snapshot_observed_at":"2026-08-02T14:23:16.098022Z","submitted_at":"2025-01-27T19:00:06Z","title":"Greybody factors, reflectionless scattering modes, and echoes of ultracompact horizonless objects","version":3},"reference_index":89,"source":"pdf_text","source_observed_at":"2026-05-23T04:43:04.006726Z"},"links":{"cited_paper":"/paper/2403.09767","citing_paper":"/paper/2501.16433"},"observation_digest":"sha256:82339280249ca6474a2e914c437d43d494c560f2210e14d1aab23e6105d5b767","observation_id":"fd123e7a-ec20-4881-bee7-c611f517a6a5","resolution":{"observed_at":"2026-05-23T04:45:25.190157Z","resolver_source":"arxiv_id","status":"verified_exact"},"standing_notice":{"events":[],"observation":"No event found in the named queried sources as of 2026-08-11T06:34:44.6726+00:00.","reason":null,"source_receipts":[{"observed_at":"2026-08-11T06:34:44.6726+00:00","source":"crossref"},{"observed_at":"2026-08-11T06:34:36.301508+00:00","source":"retraction_watch"}],"state":"measured"}},{"citation":{"cited_paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","version":2},"cited_work":{"arxiv_id":null,"doi":null,"metadata_source":null,"pith_arxiv_id":"2403.09767","snapshot_observed_at":"2026-08-04T19:41:18.997206Z","title":null,"venue":null,"work_id":null,"year":2024},"citing_paper":{"arxiv_id":"2509.09165","last_updated":"2025-09-11T05:48:16Z","snapshot_observed_at":"2026-08-06T05:34:14.678824Z","submitted_at":"2025-09-11T05:48:16Z","title":"Probing Direct Waves in Black Hole Ringdowns","version":1},"reference_index":28,"source":"pdf_text","source_observed_at":"2026-08-04T19:41:18.997206Z"},"links":{"cited_paper":"/paper/2403.09767","citing_paper":"/paper/2509.09165"},"observation_digest":"sha256:afe8d05e797069bc2756e2127a1f497592ddd13eb089948d86aa0a6004f179b2","observation_id":"63b338fb-68c1-4cce-88ab-ad3ed29bd102","resolution":{"observed_at":"2026-08-04T19:41:18.997206Z","resolver_source":null,"status":"unresolved"},"standing_notice":{"events":[],"reason":"canonical_work_link_unavailable","source_receipts":[],"state":"unavailable"}},{"citation":{"cited_paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","version":2},"cited_work":{"arxiv_id":"2403.09767","doi":null,"metadata_source":"arxiv_reference","pith_arxiv_id":"2403.09767","snapshot_observed_at":"2026-07-04T11:59:51.914279Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","venue":null,"work_id":"5e6a86cf-049c-4890-aafe-cd41e5ad6c89","year":2024},"citing_paper":{"arxiv_id":"2510.17954","last_updated":"2026-05-05T18:22:42Z","snapshot_observed_at":"2026-07-06T22:33:39.148066Z","submitted_at":"2025-10-20T18:00:00Z","title":"Green function of the P\\\"{o}schl-Teller potential","version":2},"reference_index":13,"source":"pdf_text","source_observed_at":"2026-05-18T05:53:55.681550Z"},"links":{"cited_paper":"/paper/2403.09767","citing_paper":"/paper/2510.17954"},"observation_digest":"sha256:c2cb78dcdf46b4e90887738181717bfcfb1b8a0cb6a77762a5250206faeb386d","observation_id":"d7d1c3bb-ce9a-4dec-abff-9062768d48e5","resolution":{"observed_at":"2026-05-18T05:55:56.734233Z","resolver_source":"arxiv_id","status":"verified_exact"},"standing_notice":{"events":[],"observation":"No event found in the named queried sources as of 2026-08-11T06:34:44.6726+00:00.","reason":null,"source_receipts":[{"observed_at":"2026-08-11T06:34:44.6726+00:00","source":"crossref"},{"observed_at":"2026-08-11T06:34:36.301508+00:00","source":"retraction_watch"}],"state":"measured"}},{"citation":{"cited_paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","version":2},"cited_work":{"arxiv_id":"2403.09767","doi":null,"metadata_source":"arxiv_reference","pith_arxiv_id":"2403.09767","snapshot_observed_at":"2026-07-04T11:59:51.914279Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","venue":null,"work_id":"5e6a86cf-049c-4890-aafe-cd41e5ad6c89","year":2024},"citing_paper":{"arxiv_id":"2511.08692","last_updated":"2026-05-13T14:11:56Z","snapshot_observed_at":"2026-07-06T22:35:31.750339Z","submitted_at":"2025-11-11T19:00:08Z","title":"Excitation factors for horizonless compact objects: long-lived modes, echoes, and greybody factors","version":2},"reference_index":86,"source":"pdf_text","source_observed_at":"2026-05-17T23:20:36.030481Z"},"links":{"cited_paper":"/paper/2403.09767","citing_paper":"/paper/2511.08692"},"observation_digest":"sha256:502dc164514babd184e0bd9cfa20aa2bab9e7f5fc9d0edafb49a9004680cba66","observation_id":"9613af77-9497-456a-98b3-8842d5fa8409","resolution":{"observed_at":"2026-05-17T23:22:13.130171Z","resolver_source":"arxiv_id","status":"verified_exact"},"standing_notice":{"events":[],"observation":"No event found in the named queried sources as of 2026-08-11T06:34:44.6726+00:00.","reason":null,"source_receipts":[{"observed_at":"2026-08-11T06:34:44.6726+00:00","source":"crossref"},{"observed_at":"2026-08-11T06:34:36.301508+00:00","source":"retraction_watch"}],"state":"measured"}},{"citation":{"cited_paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","version":2},"cited_work":{"arxiv_id":"2403.09767","doi":null,"metadata_source":"arxiv_reference","pith_arxiv_id":"2403.09767","snapshot_observed_at":"2026-07-04T11:59:51.914279Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","venue":null,"work_id":"5e6a86cf-049c-4890-aafe-cd41e5ad6c89","year":2024},"citing_paper":{"arxiv_id":"2603.23634","last_updated":"2026-04-29T08:42:54Z","snapshot_observed_at":"2026-08-11T00:52:47.122746Z","submitted_at":"2026-03-24T18:20:49Z","title":"Testing Dark Energy with Black Hole Ringdown","version":2},"reference_index":98,"source":"pdf_text","source_observed_at":"2026-05-15T00:29:02.526419Z"},"links":{"cited_paper":"/paper/2403.09767","citing_paper":"/paper/2603.23634"},"observation_digest":"sha256:7fc3db712236ec9b09441f19d9859a66600fab1d709916420d10cfb08ba4a011","observation_id":"af3d1e01-e8d4-4155-95ed-4657147b439c","resolution":{"observed_at":"2026-05-15T00:29:35.599839Z","resolver_source":"arxiv_id","status":"verified_exact"},"standing_notice":{"events":[],"observation":"No event found in the named queried sources as of 2026-08-11T06:34:44.6726+00:00.","reason":null,"source_receipts":[{"observed_at":"2026-08-11T06:34:44.6726+00:00","source":"crossref"},{"observed_at":"2026-08-11T06:34:36.301508+00:00","source":"retraction_watch"}],"state":"measured"}},{"citation":{"cited_paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","version":2},"cited_work":{"arxiv_id":"2403.09767","doi":null,"metadata_source":"arxiv_reference","pith_arxiv_id":"2403.09767","snapshot_observed_at":"2026-07-04T11:59:51.914279Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","venue":null,"work_id":"5e6a86cf-049c-4890-aafe-cd41e5ad6c89","year":2024},"citing_paper":{"arxiv_id":"2604.08680","last_updated":"2026-04-09T18:12:06Z","snapshot_observed_at":"2026-08-11T04:34:00.594362Z","submitted_at":"2026-04-09T18:12:06Z","title":"Prompt Response from Plunging Sources in Schwarzschild Spacetime","version":1},"reference_index":36,"source":"pdf_text","source_observed_at":"2026-05-10T17:11:15.686360Z"},"links":{"cited_paper":"/paper/2403.09767","citing_paper":"/paper/2604.08680"},"observation_digest":"sha256:27692ab33ae078c3d6a7e8c081c538efac6c5ea5b8ce90c2052b8c583d67e036","observation_id":"a39c98fe-7319-4e17-b7ac-bfec1ffe15a4","resolution":{"observed_at":"2026-05-11T07:26:01.844083Z","resolver_source":"arxiv_id","status":"verified_exact"},"standing_notice":{"events":[],"observation":"No event found in the named queried sources as of 2026-08-11T06:34:44.6726+00:00.","reason":null,"source_receipts":[{"observed_at":"2026-08-11T06:34:44.6726+00:00","source":"crossref"},{"observed_at":"2026-08-11T06:34:36.301508+00:00","source":"retraction_watch"}],"state":"measured"}},{"citation":{"cited_paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","version":2},"cited_work":{"arxiv_id":"2403.09767","doi":null,"metadata_source":"arxiv_reference","pith_arxiv_id":"2403.09767","snapshot_observed_at":"2026-07-04T11:59:51.914279Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","venue":null,"work_id":"5e6a86cf-049c-4890-aafe-cd41e5ad6c89","year":2024},"citing_paper":{"arxiv_id":"2605.04147","last_updated":"2026-05-05T18:00:02Z","snapshot_observed_at":"2026-07-06T23:16:59.568304Z","submitted_at":"2026-05-05T18:00:02Z","title":"Unifying the Regge-Wheeler-Zerilli and Bardeen-Press-Teukolsky formalisms on spherical backgrounds","version":1},"reference_index":69,"source":"pdf_text","source_observed_at":"2026-05-08T18:56:09.664711Z"},"links":{"cited_paper":"/paper/2403.09767","citing_paper":"/paper/2605.04147"},"observation_digest":"sha256:7e7f1fca947110a2e38daaa20c60069ee0cf19c04b8dc4ee3a2f37868ae89cb6","observation_id":"3d3a7ee3-82c3-449f-9112-3c2efa7369a1","resolution":{"observed_at":"2026-05-09T06:05:35.824790Z","resolver_source":"arxiv_id","status":"verified_exact"},"standing_notice":{"events":[],"observation":"No event found in the named queried sources as of 2026-08-11T06:34:44.6726+00:00.","reason":null,"source_receipts":[{"observed_at":"2026-08-11T06:34:44.6726+00:00","source":"crossref"},{"observed_at":"2026-08-11T06:34:36.301508+00:00","source":"retraction_watch"}],"state":"measured"}},{"citation":{"cited_paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","version":2},"cited_work":{"arxiv_id":"2403.09767","doi":null,"metadata_source":"arxiv_reference","pith_arxiv_id":"2403.09767","snapshot_observed_at":"2026-07-04T11:59:51.914279Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","venue":null,"work_id":"5e6a86cf-049c-4890-aafe-cd41e5ad6c89","year":2024},"citing_paper":{"arxiv_id":"2605.18595","last_updated":"2026-05-18T16:07:29Z","snapshot_observed_at":"2026-08-02T05:34:30.048120Z","submitted_at":"2026-05-18T16:07:29Z","title":"Impact of sky localization uncertainty on ringdown inference","version":1},"reference_index":27,"source":"pdf_text","source_observed_at":"2026-05-20T08:54:00.288180Z"},"links":{"cited_paper":"/paper/2403.09767","citing_paper":"/paper/2605.18595"},"observation_digest":"sha256:fc8c5e62d3fe9802f1363c765b5c7ff623c023357bdad09e5dd086f3b4c9eb8f","observation_id":"a004b3ed-aff1-4d19-aa33-2760364aaa76","resolution":{"observed_at":"2026-05-20T08:58:10.372088Z","resolver_source":"arxiv_id","status":"verified_exact"},"standing_notice":{"events":[],"observation":"No event found in the named queried sources as of 2026-08-11T06:34:44.6726+00:00.","reason":null,"source_receipts":[{"observed_at":"2026-08-11T06:34:44.6726+00:00","source":"crossref"},{"observed_at":"2026-08-11T06:34:36.301508+00:00","source":"retraction_watch"}],"state":"measured"}},{"citation":{"cited_paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","version":2},"cited_work":{"arxiv_id":"2403.09767","doi":null,"metadata_source":"arxiv_reference","pith_arxiv_id":"2403.09767","snapshot_observed_at":"2026-07-04T11:59:51.914279Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","venue":null,"work_id":"5e6a86cf-049c-4890-aafe-cd41e5ad6c89","year":2024},"citing_paper":{"arxiv_id":"2606.23804","last_updated":"2026-06-22T18:00:06Z","snapshot_observed_at":"2026-07-06T02:11:23.670680Z","submitted_at":"2026-06-22T18:00:06Z","title":"Black Hole Ringdown Nonlinearities in the Large-D Limit","version":1},"reference_index":9,"source":"pdf_text","source_observed_at":"2026-06-26T07:18:12.945787Z"},"links":{"cited_paper":"/paper/2403.09767","citing_paper":"/paper/2606.23804"},"observation_digest":"sha256:70c043ad76efaa364e71dd202e6b057fae0b9cf165175ae8581a610c17ac4492","observation_id":"f019dd0d-1eaf-4e85-8a73-e2beec099e7f","resolution":{"observed_at":"2026-07-04T11:59:51.916515Z","resolver_source":"arxiv_id","status":"verified_exact"},"standing_notice":{"events":[],"observation":"No event found in the named queried sources as of 2026-08-11T06:34:44.6726+00:00.","reason":null,"source_receipts":[{"observed_at":"2026-08-11T06:34:44.6726+00:00","source":"crossref"},{"observed_at":"2026-08-11T06:34:36.301508+00:00","source":"retraction_watch"}],"state":"measured"}},{"citation":{"cited_paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors","version":2},"cited_work":{"arxiv_id":null,"doi":null,"metadata_source":null,"pith_arxiv_id":"2403.09767","snapshot_observed_at":"2026-07-14T13:34:21.455038Z","title":null,"venue":null,"work_id":null,"year":2024},"citing_paper":{"arxiv_id":"2607.10199","last_updated":"2026-07-11T08:25:20Z","snapshot_observed_at":"2026-08-08T07:47:26.456201Z","submitted_at":"2026-07-11T08:25:20Z","title":"Quasinormal modes of Bonanno-Reuter black holes via the Spectral Method","version":1},"reference_index":71,"source":"pdf_text","source_observed_at":"2026-07-14T13:34:21.455038Z"},"links":{"cited_paper":"/paper/2403.09767","citing_paper":"/paper/2607.10199"},"observation_digest":"sha256:87d9828c87d2a25436b08347de081297a0bc0d7d2949da5ee65877ca83387e33","observation_id":"74215cf1-1f18-4793-ae1b-b680dbf6899d","resolution":{"observed_at":"2026-07-14T13:34:21.455038Z","resolver_source":null,"status":"unresolved"},"standing_notice":{"events":[],"reason":"canonical_work_link_unavailable","source_receipts":[],"state":"unavailable"}}],"links":{"evidence":"/evidence","html":"/paper/2403.09767/citation-record","integrity":"/paper/2403.09767/integrity","json":"/paper/2403.09767/citation-record.json","paper":"/paper/2403.09767"},"outbound":[],"paper":{"arxiv_id":"2403.09767","last_updated":"2024-06-17T14:01:04Z","latest_version":2,"primary_category":"gr-qc","snapshot_observed_at":"2026-08-11T04:47:50.705497Z","submitted_at":"2024-03-14T18:00:00Z","title":"Nonlinear quasinormal mode detectability with next-generation gravitational wave detectors"},"reference_resolution":{"displayed":0,"state_counts":{"malformed_identifier":0,"metadata_mismatch":0,"parse_uncertain":0,"unresolved":0,"verified_exact":0,"verified_fuzzy":0},"total_outbound_references":0},"refusal":"A citation records a reference. It does not transfer a finding from one paper to another.","schema":"pith.paper-citation-record.v1","standing_sources":[{"observed_at":"2026-08-11T06:34:44.6726+00:00","source":"crossref"},{"observed_at":"2026-08-11T06:34:36.301508+00:00","source":"retraction_watch"}],"thesis":"As of 11 August 2026, this Paper Citation Record lists 0 of 0 outbound references and 11 inbound Pith citation observations for arXiv:2403.09767."}