{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:USWEN2LBVXVWYD4RFQRYINTV5W","short_pith_number":"pith:USWEN2LB","schema_version":"1.0","canonical_sha256":"a4ac46e961adeb6c0f912c23843675edb8b6cf449fa3f587d34f2cc3884cf33f","source":{"kind":"arxiv","id":"2103.15160","version":2},"attestation_state":"computed","paper":{"title":"Characterization of the AARTFAAC-12 aperture array: radio source counts at 42 and 61 MHz","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.IM","authors_text":"A. Shulevski, B. K. Gehlot, M. Kuiack, R. A. M. J. Wijers, T. M. O. Franzen, T. Vernstrom, W. L. Williams","submitted_at":"2021-03-28T16:03:51Z","abstract_excerpt":"Dense aperture arrays provide key benefits in modern astrophysical research. They are flexible, employing cheap receivers, while relying on the ever more sophisticated compute back-end to deal with the complexities of signal processing required for optimal use. Their advantage is that they offer very large fields of view and are readily scalable to any size, all other things being equal. Since they represent \"software telescopes\", the science cases these arrays can be applied to are quite broad. Here, we describe the calibration and performance of the AARTFAAC-12 instrument, which is composed "},"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":"2103.15160","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.IM","submitted_at":"2021-03-28T16:03:51Z","cross_cats_sorted":[],"title_canon_sha256":"2ce2f1fe9a414f0ac1d302036036dc5adaca7f1aaf43c4ed6d66a2c8c7f7ed9d","abstract_canon_sha256":"c54d983863c453b01747a77517e8711d4d9f38421ba64284c370b2713f16b15d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:11:44.768325Z","signature_b64":"K7UYHdpvZs8ct/sXAYIdV++2aD5tFnXRAGeyr1G6Eo//3rVLyziuYQMJsAThZA9FDqzENkeWI2KXl1XO00kkAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a4ac46e961adeb6c0f912c23843675edb8b6cf449fa3f587d34f2cc3884cf33f","last_reissued_at":"2026-07-05T04:11:44.767904Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:11:44.767904Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Characterization of the AARTFAAC-12 aperture array: radio source counts at 42 and 61 MHz","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.IM","authors_text":"A. Shulevski, B. K. Gehlot, M. Kuiack, R. A. M. J. Wijers, T. M. O. Franzen, T. Vernstrom, W. L. Williams","submitted_at":"2021-03-28T16:03:51Z","abstract_excerpt":"Dense aperture arrays provide key benefits in modern astrophysical research. They are flexible, employing cheap receivers, while relying on the ever more sophisticated compute back-end to deal with the complexities of signal processing required for optimal use. Their advantage is that they offer very large fields of view and are readily scalable to any size, all other things being equal. Since they represent \"software telescopes\", the science cases these arrays can be applied to are quite broad. Here, we describe the calibration and performance of the AARTFAAC-12 instrument, which is composed "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2103.15160","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/2103.15160/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":"2103.15160","created_at":"2026-07-05T04:11:44.767955+00:00"},{"alias_kind":"arxiv_version","alias_value":"2103.15160v2","created_at":"2026-07-05T04:11:44.767955+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2103.15160","created_at":"2026-07-05T04:11:44.767955+00:00"},{"alias_kind":"pith_short_12","alias_value":"USWEN2LBVXVW","created_at":"2026-07-05T04:11:44.767955+00:00"},{"alias_kind":"pith_short_16","alias_value":"USWEN2LBVXVWYD4R","created_at":"2026-07-05T04:11:44.767955+00:00"},{"alias_kind":"pith_short_8","alias_value":"USWEN2LB","created_at":"2026-07-05T04:11:44.767955+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.03024","citing_title":"Rapid Response Triggering for Radio Transients with the SKA Observatory","ref_index":292,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/USWEN2LBVXVWYD4RFQRYINTV5W","json":"https://pith.science/pith/USWEN2LBVXVWYD4RFQRYINTV5W.json","graph_json":"https://pith.science/api/pith-number/USWEN2LBVXVWYD4RFQRYINTV5W/graph.json","events_json":"https://pith.science/api/pith-number/USWEN2LBVXVWYD4RFQRYINTV5W/events.json","paper":"https://pith.science/paper/USWEN2LB"},"agent_actions":{"view_html":"https://pith.science/pith/USWEN2LBVXVWYD4RFQRYINTV5W","download_json":"https://pith.science/pith/USWEN2LBVXVWYD4RFQRYINTV5W.json","view_paper":"https://pith.science/paper/USWEN2LB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2103.15160&json=true","fetch_graph":"https://pith.science/api/pith-number/USWEN2LBVXVWYD4RFQRYINTV5W/graph.json","fetch_events":"https://pith.science/api/pith-number/USWEN2LBVXVWYD4RFQRYINTV5W/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/USWEN2LBVXVWYD4RFQRYINTV5W/action/timestamp_anchor","attest_storage":"https://pith.science/pith/USWEN2LBVXVWYD4RFQRYINTV5W/action/storage_attestation","attest_author":"https://pith.science/pith/USWEN2LBVXVWYD4RFQRYINTV5W/action/author_attestation","sign_citation":"https://pith.science/pith/USWEN2LBVXVWYD4RFQRYINTV5W/action/citation_signature","submit_replication":"https://pith.science/pith/USWEN2LBVXVWYD4RFQRYINTV5W/action/replication_record"}},"created_at":"2026-07-05T04:11:44.767955+00:00","updated_at":"2026-07-05T04:11:44.767955+00:00"}