{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:OWPCXFEVJFRYIMP736WSN5G5K6","short_pith_number":"pith:OWPCXFEV","schema_version":"1.0","canonical_sha256":"759e2b949549638431ffdfad26f4dd57befa09f723be9bc8688214ca4b16fff4","source":{"kind":"arxiv","id":"1909.06296","version":4},"attestation_state":"computed","paper":{"title":"Bayesian parameter estimation using conditional variational autoencoders for gravitational-wave astronomy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["cs.LG","gr-qc"],"primary_cat":"astro-ph.IM","authors_text":"Chris Messenger, Francesco Tonolini, Hunter Gabbard, Ik Siong Heng, Roderick Murray-Smith","submitted_at":"2019-09-13T15:41:33Z","abstract_excerpt":"Gravitational wave (GW) detection is now commonplace and as the sensitivity of the global network of GW detectors improves, we will observe $\\mathcal{O}(100)$s of transient GW events per year. The current methods used to estimate their source parameters employ optimally sensitive but computationally costly Bayesian inference approaches where typical analyses have taken between 6 hours and 5 days. For binary neutron star and neutron star black hole systems prompt counterpart electromagnetic (EM) signatures are expected on timescales of 1 second -- 1 minute and the current fastest method for ale"},"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":"1909.06296","kind":"arxiv","version":4},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.IM","submitted_at":"2019-09-13T15:41:33Z","cross_cats_sorted":["cs.LG","gr-qc"],"title_canon_sha256":"a3b42fedcc4dedc4fc0245ba7f800ffa66a7c73ba02d86ae43971229fdbdf280","abstract_canon_sha256":"973d2489396a478de982d854c3fb282692c8d84a8b1c2ef852a273913434d405"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:49:57.768464Z","signature_b64":"nyGEAE8elmFKOfg6B1bkVaFvf49wW2hLXIrblI2Lbb59FK5A1aeHmTlblpTKzJz3T60zs3hKlWAeZhM6V14MCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"759e2b949549638431ffdfad26f4dd57befa09f723be9bc8688214ca4b16fff4","last_reissued_at":"2026-07-05T03:49:57.768049Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:49:57.768049Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Bayesian parameter estimation using conditional variational autoencoders for gravitational-wave astronomy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["cs.LG","gr-qc"],"primary_cat":"astro-ph.IM","authors_text":"Chris Messenger, Francesco Tonolini, Hunter Gabbard, Ik Siong Heng, Roderick Murray-Smith","submitted_at":"2019-09-13T15:41:33Z","abstract_excerpt":"Gravitational wave (GW) detection is now commonplace and as the sensitivity of the global network of GW detectors improves, we will observe $\\mathcal{O}(100)$s of transient GW events per year. The current methods used to estimate their source parameters employ optimally sensitive but computationally costly Bayesian inference approaches where typical analyses have taken between 6 hours and 5 days. For binary neutron star and neutron star black hole systems prompt counterpart electromagnetic (EM) signatures are expected on timescales of 1 second -- 1 minute and the current fastest method for ale"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1909.06296","kind":"arxiv","version":4},"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/1909.06296/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":"1909.06296","created_at":"2026-07-05T03:49:57.768109+00:00"},{"alias_kind":"arxiv_version","alias_value":"1909.06296v4","created_at":"2026-07-05T03:49:57.768109+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1909.06296","created_at":"2026-07-05T03:49:57.768109+00:00"},{"alias_kind":"pith_short_12","alias_value":"OWPCXFEVJFRY","created_at":"2026-07-05T03:49:57.768109+00:00"},{"alias_kind":"pith_short_16","alias_value":"OWPCXFEVJFRYIMP7","created_at":"2026-07-05T03:49:57.768109+00:00"},{"alias_kind":"pith_short_8","alias_value":"OWPCXFEV","created_at":"2026-07-05T03:49:57.768109+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2404.14286","citing_title":"Evidence for eccentricity in the population of binary black holes observed by LIGO-Virgo-KAGRA","ref_index":165,"is_internal_anchor":false},{"citing_arxiv_id":"2505.20996","citing_title":"Parameter inference of millilensed gravitational waves using neural spline flows","ref_index":55,"is_internal_anchor":false},{"citing_arxiv_id":"2006.00714","citing_title":"Bayesian inference for compact binary coalescences with BILBY: Validation and application to the first LIGO--Virgo gravitational-wave transient catalogue","ref_index":86,"is_internal_anchor":false},{"citing_arxiv_id":"2511.12642","citing_title":"Auto-encoder model for faster generation of effective one-body gravitational waveform approximations","ref_index":41,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OWPCXFEVJFRYIMP736WSN5G5K6","json":"https://pith.science/pith/OWPCXFEVJFRYIMP736WSN5G5K6.json","graph_json":"https://pith.science/api/pith-number/OWPCXFEVJFRYIMP736WSN5G5K6/graph.json","events_json":"https://pith.science/api/pith-number/OWPCXFEVJFRYIMP736WSN5G5K6/events.json","paper":"https://pith.science/paper/OWPCXFEV"},"agent_actions":{"view_html":"https://pith.science/pith/OWPCXFEVJFRYIMP736WSN5G5K6","download_json":"https://pith.science/pith/OWPCXFEVJFRYIMP736WSN5G5K6.json","view_paper":"https://pith.science/paper/OWPCXFEV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1909.06296&json=true","fetch_graph":"https://pith.science/api/pith-number/OWPCXFEVJFRYIMP736WSN5G5K6/graph.json","fetch_events":"https://pith.science/api/pith-number/OWPCXFEVJFRYIMP736WSN5G5K6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OWPCXFEVJFRYIMP736WSN5G5K6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OWPCXFEVJFRYIMP736WSN5G5K6/action/storage_attestation","attest_author":"https://pith.science/pith/OWPCXFEVJFRYIMP736WSN5G5K6/action/author_attestation","sign_citation":"https://pith.science/pith/OWPCXFEVJFRYIMP736WSN5G5K6/action/citation_signature","submit_replication":"https://pith.science/pith/OWPCXFEVJFRYIMP736WSN5G5K6/action/replication_record"}},"created_at":"2026-07-05T03:49:57.768109+00:00","updated_at":"2026-07-05T03:49:57.768109+00:00"}