{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:QEHKWQ3WEFWAIHLUISLPPCGH3N","short_pith_number":"pith:QEHKWQ3W","schema_version":"1.0","canonical_sha256":"810eab4376216c041d744496f788c7db6cebc525d708d65d2234edd114c835d8","source":{"kind":"arxiv","id":"1606.01716","version":2},"attestation_state":"computed","paper":{"title":"Towards a first design of a Newtonian-noise cancellation system for Advanced LIGO","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"gr-qc","authors_text":"Jan Harms, Jenne Driggers, Michael Coughlin, Nikhil Mukund, Rana Adhikari, Sanjit Mitra","submitted_at":"2016-06-06T12:40:55Z","abstract_excerpt":"Newtonian gravitational noise from seismic fields is predicted to be a limiting noise source at low frequency for second generation gravitational-wave detectors. Mitigation of this noise will be achieved by Wiener filtering using arrays of seismometers deployed in the vicinity of all test masses. In this work, we present optimized configurations of seismometer arrays using a variety of simplified models of the seismic field based on seismic observations at LIGO Hanford. The model that best fits the seismic measurements leads to noise reduction limited predominantly by seismometer self-noise. A"},"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":"1606.01716","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2016-06-06T12:40:55Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"0c51cdb73919d8afd8c72bc0eec8951425d0b993e9af2a1337831ed4e640fcfe","abstract_canon_sha256":"0498096863ef616b16c28614406b941b162a5d5fc2762da44e0bd7fdf2e92d13"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:54:15.585663Z","signature_b64":"LhSYqoXMQDPwbLjxVQCupC9swkvc3UQz65JUwuSj53VsUfbpjQCFAHjjNI6BJc3m2wxOWrZkb4pOGOTaco94DA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"810eab4376216c041d744496f788c7db6cebc525d708d65d2234edd114c835d8","last_reissued_at":"2026-05-18T00:54:15.585124Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:54:15.585124Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Towards a first design of a Newtonian-noise cancellation system for Advanced LIGO","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"gr-qc","authors_text":"Jan Harms, Jenne Driggers, Michael Coughlin, Nikhil Mukund, Rana Adhikari, Sanjit Mitra","submitted_at":"2016-06-06T12:40:55Z","abstract_excerpt":"Newtonian gravitational noise from seismic fields is predicted to be a limiting noise source at low frequency for second generation gravitational-wave detectors. Mitigation of this noise will be achieved by Wiener filtering using arrays of seismometers deployed in the vicinity of all test masses. In this work, we present optimized configurations of seismometer arrays using a variety of simplified models of the seismic field based on seismic observations at LIGO Hanford. The model that best fits the seismic measurements leads to noise reduction limited predominantly by seismometer self-noise. A"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1606.01716","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":""},"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":"1606.01716","created_at":"2026-05-18T00:54:15.585186+00:00"},{"alias_kind":"arxiv_version","alias_value":"1606.01716v2","created_at":"2026-05-18T00:54:15.585186+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1606.01716","created_at":"2026-05-18T00:54:15.585186+00:00"},{"alias_kind":"pith_short_12","alias_value":"QEHKWQ3WEFWA","created_at":"2026-05-18T12:30:39.010887+00:00"},{"alias_kind":"pith_short_16","alias_value":"QEHKWQ3WEFWAIHLU","created_at":"2026-05-18T12:30:39.010887+00:00"},{"alias_kind":"pith_short_8","alias_value":"QEHKWQ3W","created_at":"2026-05-18T12:30:39.010887+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2408.14341","citing_title":"True and apparent motion of optomechanical resonators, with applications to feedback cooling of gravitational wave detector test masses","ref_index":57,"is_internal_anchor":true},{"citing_arxiv_id":"2604.24866","citing_title":"Seismic background mitigation with the Lunar Gravitational-wave Antenna","ref_index":30,"is_internal_anchor":false},{"citing_arxiv_id":"2604.15759","citing_title":"Mechanical Long Baseline Differential Gradiometers as Low Frequency Gravitational Wave Detectors","ref_index":33,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QEHKWQ3WEFWAIHLUISLPPCGH3N","json":"https://pith.science/pith/QEHKWQ3WEFWAIHLUISLPPCGH3N.json","graph_json":"https://pith.science/api/pith-number/QEHKWQ3WEFWAIHLUISLPPCGH3N/graph.json","events_json":"https://pith.science/api/pith-number/QEHKWQ3WEFWAIHLUISLPPCGH3N/events.json","paper":"https://pith.science/paper/QEHKWQ3W"},"agent_actions":{"view_html":"https://pith.science/pith/QEHKWQ3WEFWAIHLUISLPPCGH3N","download_json":"https://pith.science/pith/QEHKWQ3WEFWAIHLUISLPPCGH3N.json","view_paper":"https://pith.science/paper/QEHKWQ3W","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1606.01716&json=true","fetch_graph":"https://pith.science/api/pith-number/QEHKWQ3WEFWAIHLUISLPPCGH3N/graph.json","fetch_events":"https://pith.science/api/pith-number/QEHKWQ3WEFWAIHLUISLPPCGH3N/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QEHKWQ3WEFWAIHLUISLPPCGH3N/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QEHKWQ3WEFWAIHLUISLPPCGH3N/action/storage_attestation","attest_author":"https://pith.science/pith/QEHKWQ3WEFWAIHLUISLPPCGH3N/action/author_attestation","sign_citation":"https://pith.science/pith/QEHKWQ3WEFWAIHLUISLPPCGH3N/action/citation_signature","submit_replication":"https://pith.science/pith/QEHKWQ3WEFWAIHLUISLPPCGH3N/action/replication_record"}},"created_at":"2026-05-18T00:54:15.585186+00:00","updated_at":"2026-05-18T00:54:15.585186+00:00"}