{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:5MEYWJG36HBCN6OXDIS3ZKN4YJ","short_pith_number":"pith:5MEYWJG3","schema_version":"1.0","canonical_sha256":"eb098b24dbf1c226f9d71a25bca9bcc270cbc5e34cac07bb6fdd87c30de3049f","source":{"kind":"arxiv","id":"2312.12435","version":2},"attestation_state":"computed","paper":{"title":"Velocity reconstruction in the era of DESI and Rubin (part I): Exploring spectroscopic, photometric & hybrid samples","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Bernardita Ried Guachalla, Boryana Hadzhiyska, Emmanuel Schaan, Simone Ferraro","submitted_at":"2023-12-19T18:59:19Z","abstract_excerpt":"Peculiar velocities of galaxies and halos can be reconstructed from their spatial distribution alone. This technique is analogous to the baryon acoustic oscillations (BAO) reconstruction, using the continuity equation to connect density and velocity fields. The resulting reconstructed velocities can be used to measure imprints of galaxy velocities on the cosmic microwave background (CMB) like the kinematic Sunyaev-Zel'dovich (kSZ) effect or the moving lens effect. As the precision of these measurements increases, characterizing the performance of the velocity reconstruction becomes crucial to "},"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":"2312.12435","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2023-12-19T18:59:19Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"01d7d10d1ed0ddea3f2b2018354f2f1326c90adf64db340e79adaa5f8b376685","abstract_canon_sha256":"eb9e801683562bff5d8ee0db3cae2f3a3cac7301f8cd8b17d486e1ea3b56a88b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:21:46.093789Z","signature_b64":"jQjiBiyCdyjbf7VTvBB2kx5dLWkXs6dwh/TFfSARN3PZy1iHL1mTj7qmNhS1//VvhbLvN2O9vqXrYdW6PjlDBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"eb098b24dbf1c226f9d71a25bca9bcc270cbc5e34cac07bb6fdd87c30de3049f","last_reissued_at":"2026-07-05T08:21:46.093292Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:21:46.093292Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Velocity reconstruction in the era of DESI and Rubin (part I): Exploring spectroscopic, photometric & hybrid samples","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Bernardita Ried Guachalla, Boryana Hadzhiyska, Emmanuel Schaan, Simone Ferraro","submitted_at":"2023-12-19T18:59:19Z","abstract_excerpt":"Peculiar velocities of galaxies and halos can be reconstructed from their spatial distribution alone. This technique is analogous to the baryon acoustic oscillations (BAO) reconstruction, using the continuity equation to connect density and velocity fields. The resulting reconstructed velocities can be used to measure imprints of galaxy velocities on the cosmic microwave background (CMB) like the kinematic Sunyaev-Zel'dovich (kSZ) effect or the moving lens effect. As the precision of these measurements increases, characterizing the performance of the velocity reconstruction becomes crucial to "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2312.12435","kind":"arxiv","version":2},"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/2312.12435/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":"2312.12435","created_at":"2026-07-05T08:21:46.093360+00:00"},{"alias_kind":"arxiv_version","alias_value":"2312.12435v2","created_at":"2026-07-05T08:21:46.093360+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2312.12435","created_at":"2026-07-05T08:21:46.093360+00:00"},{"alias_kind":"pith_short_12","alias_value":"5MEYWJG36HBC","created_at":"2026-07-05T08:21:46.093360+00:00"},{"alias_kind":"pith_short_16","alias_value":"5MEYWJG36HBCN6OX","created_at":"2026-07-05T08:21:46.093360+00:00"},{"alias_kind":"pith_short_8","alias_value":"5MEYWJG3","created_at":"2026-07-05T08:21:46.093360+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.05047","citing_title":"Full Nonlinear Velocity Reconstruction With Transformer and Ensemble Tree Machine Learning","ref_index":37,"is_internal_anchor":false},{"citing_arxiv_id":"2606.26237","citing_title":"First full-shape joint analysis of the two- and three-point correlation functions on real data: $\\Lambda$CDM cosmological constraints from BOSS DR12","ref_index":262,"is_internal_anchor":false},{"citing_arxiv_id":"2605.18938","citing_title":"First detection of the moving lens effect with ACT and DESI LS","ref_index":24,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5MEYWJG36HBCN6OXDIS3ZKN4YJ","json":"https://pith.science/pith/5MEYWJG36HBCN6OXDIS3ZKN4YJ.json","graph_json":"https://pith.science/api/pith-number/5MEYWJG36HBCN6OXDIS3ZKN4YJ/graph.json","events_json":"https://pith.science/api/pith-number/5MEYWJG36HBCN6OXDIS3ZKN4YJ/events.json","paper":"https://pith.science/paper/5MEYWJG3"},"agent_actions":{"view_html":"https://pith.science/pith/5MEYWJG36HBCN6OXDIS3ZKN4YJ","download_json":"https://pith.science/pith/5MEYWJG36HBCN6OXDIS3ZKN4YJ.json","view_paper":"https://pith.science/paper/5MEYWJG3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2312.12435&json=true","fetch_graph":"https://pith.science/api/pith-number/5MEYWJG36HBCN6OXDIS3ZKN4YJ/graph.json","fetch_events":"https://pith.science/api/pith-number/5MEYWJG36HBCN6OXDIS3ZKN4YJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5MEYWJG36HBCN6OXDIS3ZKN4YJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5MEYWJG36HBCN6OXDIS3ZKN4YJ/action/storage_attestation","attest_author":"https://pith.science/pith/5MEYWJG36HBCN6OXDIS3ZKN4YJ/action/author_attestation","sign_citation":"https://pith.science/pith/5MEYWJG36HBCN6OXDIS3ZKN4YJ/action/citation_signature","submit_replication":"https://pith.science/pith/5MEYWJG36HBCN6OXDIS3ZKN4YJ/action/replication_record"}},"created_at":"2026-07-05T08:21:46.093360+00:00","updated_at":"2026-07-05T08:21:46.093360+00:00"}