{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:HTYRVNFZIF7W6M3DYZK2NLU6FJ","short_pith_number":"pith:HTYRVNFZ","schema_version":"1.0","canonical_sha256":"3cf11ab4b9417f6f3363c655a6ae9e2a6890f4093b861316942fd02fe2dcd8d1","source":{"kind":"arxiv","id":"1603.07333","version":4},"attestation_state":"computed","paper":{"title":"Going the Distance: Mapping Host Galaxies of LIGO and Virgo Sources in Three Dimensions Using Local Cosmography and Targeted Follow-up","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Alex L. Urban, B. Farr, C. P. L. Berry, D. E. Holz, H.-Y. Chen, I. Mandel, J. Cannizzo, J. Veitch, L. P. Singer, L. R. Price, M. Coughlin, M. M. Kasliwal, N. Gehrels, P. Graff, S. B. Cenko, S. Mohapatra, S. Nissanke, S. Vitale, V. Raymond, W. M. Farr","submitted_at":"2016-03-23T20:00:02Z","abstract_excerpt":"The Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) discovered gravitational waves (GWs) from a binary black hole merger in 2015 September and may soon observe signals from neutron star mergers. There is considerable interest in searching for their faint and rapidly fading electromagnetic (EM) counterparts, though GW position uncertainties are as coarse as hundreds of square degrees. Because LIGO's sensitivity to binary neutron stars is limited to the local universe, the area on the sky that must be searched could be reduced by weighting positions by mass, luminosity, or st"},"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":"1603.07333","kind":"arxiv","version":4},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2016-03-23T20:00:02Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"6fda62db15094fe646f882e187cfe3e93a132f81cb414791f8b215ab04daf965","abstract_canon_sha256":"d3fdd3d741f07d1f9b24c53ff48223868aeb041c541b1a4ce9584b41f78f09de"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:03:40.737007Z","signature_b64":"rByLFrnmy29BBTmAzX6D6KzRmZ+eR9Ix9a8LUJ+S4UryxnJD2PSGMMFtPKixRzLGxwB6OpBBQ9ORS9qHQEkyDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3cf11ab4b9417f6f3363c655a6ae9e2a6890f4093b861316942fd02fe2dcd8d1","last_reissued_at":"2026-05-18T01:03:40.736620Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:03:40.736620Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Going the Distance: Mapping Host Galaxies of LIGO and Virgo Sources in Three Dimensions Using Local Cosmography and Targeted Follow-up","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Alex L. Urban, B. Farr, C. P. L. Berry, D. E. Holz, H.-Y. Chen, I. Mandel, J. Cannizzo, J. Veitch, L. P. Singer, L. R. Price, M. Coughlin, M. M. Kasliwal, N. Gehrels, P. Graff, S. B. Cenko, S. Mohapatra, S. Nissanke, S. Vitale, V. Raymond, W. M. Farr","submitted_at":"2016-03-23T20:00:02Z","abstract_excerpt":"The Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) discovered gravitational waves (GWs) from a binary black hole merger in 2015 September and may soon observe signals from neutron star mergers. There is considerable interest in searching for their faint and rapidly fading electromagnetic (EM) counterparts, though GW position uncertainties are as coarse as hundreds of square degrees. Because LIGO's sensitivity to binary neutron stars is limited to the local universe, the area on the sky that must be searched could be reduced by weighting positions by mass, luminosity, or st"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1603.07333","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":""},"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":"1603.07333","created_at":"2026-05-18T01:03:40.736683+00:00"},{"alias_kind":"arxiv_version","alias_value":"1603.07333v4","created_at":"2026-05-18T01:03:40.736683+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1603.07333","created_at":"2026-05-18T01:03:40.736683+00:00"},{"alias_kind":"pith_short_12","alias_value":"HTYRVNFZIF7W","created_at":"2026-05-18T12:30:22.444734+00:00"},{"alias_kind":"pith_short_16","alias_value":"HTYRVNFZIF7W6M3D","created_at":"2026-05-18T12:30:22.444734+00:00"},{"alias_kind":"pith_short_8","alias_value":"HTYRVNFZ","created_at":"2026-05-18T12:30:22.444734+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2108.01045","citing_title":"GWTC-2.1: Deep Extended Catalog of Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run","ref_index":290,"is_internal_anchor":true},{"citing_arxiv_id":"2605.11703","citing_title":"GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors","ref_index":65,"is_internal_anchor":false},{"citing_arxiv_id":"2604.11871","citing_title":"Not too close! Evaluating the impact of the baseline on the localization of binary black holes by next-generation gravitational-wave detectors","ref_index":88,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HTYRVNFZIF7W6M3DYZK2NLU6FJ","json":"https://pith.science/pith/HTYRVNFZIF7W6M3DYZK2NLU6FJ.json","graph_json":"https://pith.science/api/pith-number/HTYRVNFZIF7W6M3DYZK2NLU6FJ/graph.json","events_json":"https://pith.science/api/pith-number/HTYRVNFZIF7W6M3DYZK2NLU6FJ/events.json","paper":"https://pith.science/paper/HTYRVNFZ"},"agent_actions":{"view_html":"https://pith.science/pith/HTYRVNFZIF7W6M3DYZK2NLU6FJ","download_json":"https://pith.science/pith/HTYRVNFZIF7W6M3DYZK2NLU6FJ.json","view_paper":"https://pith.science/paper/HTYRVNFZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1603.07333&json=true","fetch_graph":"https://pith.science/api/pith-number/HTYRVNFZIF7W6M3DYZK2NLU6FJ/graph.json","fetch_events":"https://pith.science/api/pith-number/HTYRVNFZIF7W6M3DYZK2NLU6FJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HTYRVNFZIF7W6M3DYZK2NLU6FJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HTYRVNFZIF7W6M3DYZK2NLU6FJ/action/storage_attestation","attest_author":"https://pith.science/pith/HTYRVNFZIF7W6M3DYZK2NLU6FJ/action/author_attestation","sign_citation":"https://pith.science/pith/HTYRVNFZIF7W6M3DYZK2NLU6FJ/action/citation_signature","submit_replication":"https://pith.science/pith/HTYRVNFZIF7W6M3DYZK2NLU6FJ/action/replication_record"}},"created_at":"2026-05-18T01:03:40.736683+00:00","updated_at":"2026-05-18T01:03:40.736683+00:00"}