{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:6XPMDC3M2O32W2K6H7J25SSAXZ","short_pith_number":"pith:6XPMDC3M","schema_version":"1.0","canonical_sha256":"f5dec18b6cd3b7ab695e3fd3aeca40be7090d0d2992799fa6cd3f5f824cdc2fb","source":{"kind":"arxiv","id":"1101.5971","version":3},"attestation_state":"computed","paper":{"title":"Prospects for accurate distance measurements of pulsars with the SKA: enabling fundamental physics","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.IM","authors_text":"B. Stappers, M. Kramer, N. Wex, R. Smits, S.J. Tingay","submitted_at":"2011-01-31T14:01:13Z","abstract_excerpt":"Parallax measurements of pulsars allow for accurate measurements of the interstellar electron density and contribute to accurate tests of general relativity using binary systems. The Square Kilometre Array (SKA) will be an ideal instrument for measuring the parallax of pulsars, because it has a very high sensitivity, as well as baselines extending up to several thousands of kilometres. We performed simulations to estimate the number of pulsars for which the parallax can be measured with the SKA and the distance to which a parallax can be measured. We compare two different methods. The first me"},"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":"1101.5971","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.IM","submitted_at":"2011-01-31T14:01:13Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"951502011c535190e73527d11d69bebe4dcfcfc7f2b6a2a02dca435e9fc64333","abstract_canon_sha256":"55bf920169fd53dc7569471b17e1839231403979eefe4a99354d04324e98852f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:03:20.008287Z","signature_b64":"bhcFrRZncl6Mv2b/XYLxviq7ZceREEGoTmDPZXiF2guwkHkqS5dwA1t+fHpfEjdeHXSfx9A2pYESGo1tNlEmAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f5dec18b6cd3b7ab695e3fd3aeca40be7090d0d2992799fa6cd3f5f824cdc2fb","last_reissued_at":"2026-05-18T02:03:20.007578Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:03:20.007578Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Prospects for accurate distance measurements of pulsars with the SKA: enabling fundamental physics","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.IM","authors_text":"B. Stappers, M. Kramer, N. Wex, R. Smits, S.J. Tingay","submitted_at":"2011-01-31T14:01:13Z","abstract_excerpt":"Parallax measurements of pulsars allow for accurate measurements of the interstellar electron density and contribute to accurate tests of general relativity using binary systems. The Square Kilometre Array (SKA) will be an ideal instrument for measuring the parallax of pulsars, because it has a very high sensitivity, as well as baselines extending up to several thousands of kilometres. We performed simulations to estimate the number of pulsars for which the parallax can be measured with the SKA and the distance to which a parallax can be measured. We compare two different methods. The first me"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1101.5971","kind":"arxiv","version":3},"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":"1101.5971","created_at":"2026-05-18T02:03:20.007667+00:00"},{"alias_kind":"arxiv_version","alias_value":"1101.5971v3","created_at":"2026-05-18T02:03:20.007667+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1101.5971","created_at":"2026-05-18T02:03:20.007667+00:00"},{"alias_kind":"pith_short_12","alias_value":"6XPMDC3M2O32","created_at":"2026-05-18T12:26:22.705136+00:00"},{"alias_kind":"pith_short_16","alias_value":"6XPMDC3M2O32W2K6","created_at":"2026-05-18T12:26:22.705136+00:00"},{"alias_kind":"pith_short_8","alias_value":"6XPMDC3M","created_at":"2026-05-18T12:26:22.705136+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2406.13043","citing_title":"Inferring neutron star properties through gravitational waves from r-modes and their relativistic counterparts","ref_index":43,"is_internal_anchor":true},{"citing_arxiv_id":"2512.10795","citing_title":"Reaching diffraction-limited localization with coherent PTAs","ref_index":30,"is_internal_anchor":true},{"citing_arxiv_id":"2604.20975","citing_title":"Probing Supermassive Black Hole Mergers with Pulsar Timing Arrays","ref_index":63,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/6XPMDC3M2O32W2K6H7J25SSAXZ","json":"https://pith.science/pith/6XPMDC3M2O32W2K6H7J25SSAXZ.json","graph_json":"https://pith.science/api/pith-number/6XPMDC3M2O32W2K6H7J25SSAXZ/graph.json","events_json":"https://pith.science/api/pith-number/6XPMDC3M2O32W2K6H7J25SSAXZ/events.json","paper":"https://pith.science/paper/6XPMDC3M"},"agent_actions":{"view_html":"https://pith.science/pith/6XPMDC3M2O32W2K6H7J25SSAXZ","download_json":"https://pith.science/pith/6XPMDC3M2O32W2K6H7J25SSAXZ.json","view_paper":"https://pith.science/paper/6XPMDC3M","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1101.5971&json=true","fetch_graph":"https://pith.science/api/pith-number/6XPMDC3M2O32W2K6H7J25SSAXZ/graph.json","fetch_events":"https://pith.science/api/pith-number/6XPMDC3M2O32W2K6H7J25SSAXZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6XPMDC3M2O32W2K6H7J25SSAXZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6XPMDC3M2O32W2K6H7J25SSAXZ/action/storage_attestation","attest_author":"https://pith.science/pith/6XPMDC3M2O32W2K6H7J25SSAXZ/action/author_attestation","sign_citation":"https://pith.science/pith/6XPMDC3M2O32W2K6H7J25SSAXZ/action/citation_signature","submit_replication":"https://pith.science/pith/6XPMDC3M2O32W2K6H7J25SSAXZ/action/replication_record"}},"created_at":"2026-05-18T02:03:20.007667+00:00","updated_at":"2026-05-18T02:03:20.007667+00:00"}