{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:2E54ZAY3DLGAAHOW5UHNRJCETR","short_pith_number":"pith:2E54ZAY3","schema_version":"1.0","canonical_sha256":"d13bcc831b1acc001dd6ed0ed8a4449c651dffefdf684cd02df8fb250abb55ff","source":{"kind":"arxiv","id":"2501.06301","version":1},"attestation_state":"computed","paper":{"title":"Deep radio interferometric search for decametre radio emission from the exoplanet Tau Bo\\\"otis b","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.EP","authors_text":"C.M. Cordun, F.F.S. van der Tak, H.K. Vedantham, M.A. Brentjens","submitted_at":"2025-01-10T19:00:10Z","abstract_excerpt":"Detection of electron cyclotron maser (ECM) emission from exoplanets in the 10-40 MHz radio band is likely the only way to measure an exoplanet's magnetic field directly. However, no definitive detection of exoplanetary ECM emission has been made to date. A detection of the hot Jupiter Tau Bo\\\"otis b was reported but with an observing mode that is not immune to confusion from off-axis interference, making the detection tentative. We searched for radio emissions from Tau Bo\\\"otis b using the Low Frequency Array (LOFAR) in interferometric mode, which employs direction-of-arrival information to d"},"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":"2501.06301","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"astro-ph.EP","submitted_at":"2025-01-10T19:00:10Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"2a9830ce50b39d76611bf4f19f591fee86e7a31447c6d76353b024624de4d419","abstract_canon_sha256":"7485db9061c7ef24fe1cf5ba9ad3ea66d608d130ba15d747888930dbd80b9d0c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:00:00.892892Z","signature_b64":"cA/T4hERSqDKliDNgt4CMGu3ZFWkKQqyDs7g8lyTqtIbD9dcMyWaqCD4Sa/+Z4zU6Y5g0Bkcf53ADGHfG8ILAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d13bcc831b1acc001dd6ed0ed8a4449c651dffefdf684cd02df8fb250abb55ff","last_reissued_at":"2026-07-05T10:00:00.892477Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:00:00.892477Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Deep radio interferometric search for decametre radio emission from the exoplanet Tau Bo\\\"otis b","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.EP","authors_text":"C.M. Cordun, F.F.S. van der Tak, H.K. Vedantham, M.A. Brentjens","submitted_at":"2025-01-10T19:00:10Z","abstract_excerpt":"Detection of electron cyclotron maser (ECM) emission from exoplanets in the 10-40 MHz radio band is likely the only way to measure an exoplanet's magnetic field directly. However, no definitive detection of exoplanetary ECM emission has been made to date. A detection of the hot Jupiter Tau Bo\\\"otis b was reported but with an observing mode that is not immune to confusion from off-axis interference, making the detection tentative. We searched for radio emissions from Tau Bo\\\"otis b using the Low Frequency Array (LOFAR) in interferometric mode, which employs direction-of-arrival information to d"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2501.06301","kind":"arxiv","version":1},"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/2501.06301/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":"2501.06301","created_at":"2026-07-05T10:00:00.892535+00:00"},{"alias_kind":"arxiv_version","alias_value":"2501.06301v1","created_at":"2026-07-05T10:00:00.892535+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2501.06301","created_at":"2026-07-05T10:00:00.892535+00:00"},{"alias_kind":"pith_short_12","alias_value":"2E54ZAY3DLGA","created_at":"2026-07-05T10:00:00.892535+00:00"},{"alias_kind":"pith_short_16","alias_value":"2E54ZAY3DLGAAHOW","created_at":"2026-07-05T10:00:00.892535+00:00"},{"alias_kind":"pith_short_8","alias_value":"2E54ZAY3","created_at":"2026-07-05T10:00:00.892535+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.03133","citing_title":"Radio emission from star-planet interactions","ref_index":66,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2E54ZAY3DLGAAHOW5UHNRJCETR","json":"https://pith.science/pith/2E54ZAY3DLGAAHOW5UHNRJCETR.json","graph_json":"https://pith.science/api/pith-number/2E54ZAY3DLGAAHOW5UHNRJCETR/graph.json","events_json":"https://pith.science/api/pith-number/2E54ZAY3DLGAAHOW5UHNRJCETR/events.json","paper":"https://pith.science/paper/2E54ZAY3"},"agent_actions":{"view_html":"https://pith.science/pith/2E54ZAY3DLGAAHOW5UHNRJCETR","download_json":"https://pith.science/pith/2E54ZAY3DLGAAHOW5UHNRJCETR.json","view_paper":"https://pith.science/paper/2E54ZAY3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2501.06301&json=true","fetch_graph":"https://pith.science/api/pith-number/2E54ZAY3DLGAAHOW5UHNRJCETR/graph.json","fetch_events":"https://pith.science/api/pith-number/2E54ZAY3DLGAAHOW5UHNRJCETR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2E54ZAY3DLGAAHOW5UHNRJCETR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2E54ZAY3DLGAAHOW5UHNRJCETR/action/storage_attestation","attest_author":"https://pith.science/pith/2E54ZAY3DLGAAHOW5UHNRJCETR/action/author_attestation","sign_citation":"https://pith.science/pith/2E54ZAY3DLGAAHOW5UHNRJCETR/action/citation_signature","submit_replication":"https://pith.science/pith/2E54ZAY3DLGAAHOW5UHNRJCETR/action/replication_record"}},"created_at":"2026-07-05T10:00:00.892535+00:00","updated_at":"2026-07-05T10:00:00.892535+00:00"}