{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:EOEIPAVLO6OCCG7CL5QDWPWZ4B","short_pith_number":"pith:EOEIPAVL","schema_version":"1.0","canonical_sha256":"23888782ab779c211be25f603b3ed9e078ac63802590b018262a002c7a61a121","source":{"kind":"arxiv","id":"1211.5042","version":2},"attestation_state":"computed","paper":{"title":"Projected constraints on the cosmic (super)string tension with future gravitational wave detection experiments","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Benjamin W. Stappers, Richard A. Battye, Sotirios A. Sanidas","submitted_at":"2012-11-21T14:26:06Z","abstract_excerpt":"We present projected constraints on the cosmic string tension, $G\\mu/c^2$, that could be achieved by future gravitational wave detection experiments and express our results as semi-analytic relations of the form $G\\mu(\\Omega_{\\rm gw}h^2)/c^2$, to allow for direct computation of the tension constraints for future experiments. These results can be applied to new constraints on $\\ogwh$ as they are imposed. Experiments operating in different frequency bands probe different parts of the gravitational wave spectrum of a cosmic string network and are sensitive to different uncertainties in the underl"},"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":"1211.5042","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-11-21T14:26:06Z","cross_cats_sorted":[],"title_canon_sha256":"cfd85459f1944d5c9f7a46ec41eac5c812834315809bd0ca34de887948f2b130","abstract_canon_sha256":"62ca0ddbd3a8d49b80fccfa46b208ce793eef08349da861f41f60e6dc5d60ad2"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:53:01.971724Z","signature_b64":"maFEPUcKSr8bIo2piXOqUzPiZXTMjMlMV1Pps63NIkaJ3ICp/AUdr/5M+ZpnKz1FW2Ho/ywTUEI7LjF1Z8JVBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"23888782ab779c211be25f603b3ed9e078ac63802590b018262a002c7a61a121","last_reissued_at":"2026-05-18T01:53:01.971179Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:53:01.971179Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Projected constraints on the cosmic (super)string tension with future gravitational wave detection experiments","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Benjamin W. Stappers, Richard A. Battye, Sotirios A. Sanidas","submitted_at":"2012-11-21T14:26:06Z","abstract_excerpt":"We present projected constraints on the cosmic string tension, $G\\mu/c^2$, that could be achieved by future gravitational wave detection experiments and express our results as semi-analytic relations of the form $G\\mu(\\Omega_{\\rm gw}h^2)/c^2$, to allow for direct computation of the tension constraints for future experiments. These results can be applied to new constraints on $\\ogwh$ as they are imposed. Experiments operating in different frequency bands probe different parts of the gravitational wave spectrum of a cosmic string network and are sensitive to different uncertainties in the underl"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1211.5042","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":"1211.5042","created_at":"2026-05-18T01:53:01.971260+00:00"},{"alias_kind":"arxiv_version","alias_value":"1211.5042v2","created_at":"2026-05-18T01:53:01.971260+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1211.5042","created_at":"2026-05-18T01:53:01.971260+00:00"},{"alias_kind":"pith_short_12","alias_value":"EOEIPAVLO6OC","created_at":"2026-05-18T12:27:04.183437+00:00"},{"alias_kind":"pith_short_16","alias_value":"EOEIPAVLO6OCCG7C","created_at":"2026-05-18T12:27:04.183437+00:00"},{"alias_kind":"pith_short_8","alias_value":"EOEIPAVL","created_at":"2026-05-18T12:27:04.183437+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2311.01300","citing_title":"Waveform Modelling for the Laser Interferometer Space Antenna","ref_index":256,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EOEIPAVLO6OCCG7CL5QDWPWZ4B","json":"https://pith.science/pith/EOEIPAVLO6OCCG7CL5QDWPWZ4B.json","graph_json":"https://pith.science/api/pith-number/EOEIPAVLO6OCCG7CL5QDWPWZ4B/graph.json","events_json":"https://pith.science/api/pith-number/EOEIPAVLO6OCCG7CL5QDWPWZ4B/events.json","paper":"https://pith.science/paper/EOEIPAVL"},"agent_actions":{"view_html":"https://pith.science/pith/EOEIPAVLO6OCCG7CL5QDWPWZ4B","download_json":"https://pith.science/pith/EOEIPAVLO6OCCG7CL5QDWPWZ4B.json","view_paper":"https://pith.science/paper/EOEIPAVL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1211.5042&json=true","fetch_graph":"https://pith.science/api/pith-number/EOEIPAVLO6OCCG7CL5QDWPWZ4B/graph.json","fetch_events":"https://pith.science/api/pith-number/EOEIPAVLO6OCCG7CL5QDWPWZ4B/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EOEIPAVLO6OCCG7CL5QDWPWZ4B/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EOEIPAVLO6OCCG7CL5QDWPWZ4B/action/storage_attestation","attest_author":"https://pith.science/pith/EOEIPAVLO6OCCG7CL5QDWPWZ4B/action/author_attestation","sign_citation":"https://pith.science/pith/EOEIPAVLO6OCCG7CL5QDWPWZ4B/action/citation_signature","submit_replication":"https://pith.science/pith/EOEIPAVLO6OCCG7CL5QDWPWZ4B/action/replication_record"}},"created_at":"2026-05-18T01:53:01.971260+00:00","updated_at":"2026-05-18T01:53:01.971260+00:00"}