{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:MP3ZMRKOXK7XLM5FYVAEVPSCHM","short_pith_number":"pith:MP3ZMRKO","schema_version":"1.0","canonical_sha256":"63f796454ebabf75b3a5c5404abe423b3bb6c6805b7ffe3ca896ed24d789b63b","source":{"kind":"arxiv","id":"1707.07521","version":1},"attestation_state":"computed","paper":{"title":"The EBLM Project IV. Spectroscopic orbits of over 100 eclipsing M dwarfs masquerading as transiting hot-Jupiters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"Amaury H.M.J. Triaud, Andrew Collier Cameron, Barry Smalley, Coel Hellier, Damien S\\'egransan, David R. Anderson, David V. Martin, Didier Queloz, Don Pollacco, Fran\\c{c}ois Bouchy, Francesca Faedi, Francesco Pepe, Leslie Hebb, Maxime Marmier, Pierre F.L. Maxted, Richard West, St\\'ephane Udry, Yilen G\\'omez Maqueo Chew","submitted_at":"2017-07-24T12:41:08Z","abstract_excerpt":"We present 2271 radial velocity measurements taken on 118 single-line binary stars, taken over eight years with the CORALIE spectrograph. The binaries consist of F/G/K primaries and M-dwarf secondaries. They were initially discovered photometrically by the WASP planet survey, as their shallow eclipses mimic a hot-Jupiter transit. The observations we present permit a precise characterisation of the binary orbital elements and mass function. With modelling of the primary star this mass function is converted to a mass of the secondary star. In the future, this spectroscopic work will be combined "},"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":"1707.07521","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2017-07-24T12:41:08Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"3cad19a9c7a8777d4f324fc2f0f4e85f5a05fd81b546c689f31bcbe5b97cdbeb","abstract_canon_sha256":"01051b0b84dfda73e5f62f74fb427972716b46f775e3b16e4293bee56e971ece"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:27:46.205874Z","signature_b64":"o+uvGc5hCMiXSvKzHxHssEp+dzG9L/YMZtwFyCDnvXiqo5j8vPTQTimG4d3SvXB5XpVBJ/2i+C9vqIm6+JzSAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"63f796454ebabf75b3a5c5404abe423b3bb6c6805b7ffe3ca896ed24d789b63b","last_reissued_at":"2026-05-18T00:27:46.205292Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:27:46.205292Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The EBLM Project IV. Spectroscopic orbits of over 100 eclipsing M dwarfs masquerading as transiting hot-Jupiters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"Amaury H.M.J. Triaud, Andrew Collier Cameron, Barry Smalley, Coel Hellier, Damien S\\'egransan, David R. Anderson, David V. Martin, Didier Queloz, Don Pollacco, Fran\\c{c}ois Bouchy, Francesca Faedi, Francesco Pepe, Leslie Hebb, Maxime Marmier, Pierre F.L. Maxted, Richard West, St\\'ephane Udry, Yilen G\\'omez Maqueo Chew","submitted_at":"2017-07-24T12:41:08Z","abstract_excerpt":"We present 2271 radial velocity measurements taken on 118 single-line binary stars, taken over eight years with the CORALIE spectrograph. The binaries consist of F/G/K primaries and M-dwarf secondaries. They were initially discovered photometrically by the WASP planet survey, as their shallow eclipses mimic a hot-Jupiter transit. The observations we present permit a precise characterisation of the binary orbital elements and mass function. With modelling of the primary star this mass function is converted to a mass of the secondary star. In the future, this spectroscopic work will be combined "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1707.07521","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":""},"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":"1707.07521","created_at":"2026-05-18T00:27:46.205451+00:00"},{"alias_kind":"arxiv_version","alias_value":"1707.07521v1","created_at":"2026-05-18T00:27:46.205451+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1707.07521","created_at":"2026-05-18T00:27:46.205451+00:00"},{"alias_kind":"pith_short_12","alias_value":"MP3ZMRKOXK7X","created_at":"2026-05-18T12:31:31.346846+00:00"},{"alias_kind":"pith_short_16","alias_value":"MP3ZMRKOXK7XLM5F","created_at":"2026-05-18T12:31:31.346846+00:00"},{"alias_kind":"pith_short_8","alias_value":"MP3ZMRKO","created_at":"2026-05-18T12:31:31.346846+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MP3ZMRKOXK7XLM5FYVAEVPSCHM","json":"https://pith.science/pith/MP3ZMRKOXK7XLM5FYVAEVPSCHM.json","graph_json":"https://pith.science/api/pith-number/MP3ZMRKOXK7XLM5FYVAEVPSCHM/graph.json","events_json":"https://pith.science/api/pith-number/MP3ZMRKOXK7XLM5FYVAEVPSCHM/events.json","paper":"https://pith.science/paper/MP3ZMRKO"},"agent_actions":{"view_html":"https://pith.science/pith/MP3ZMRKOXK7XLM5FYVAEVPSCHM","download_json":"https://pith.science/pith/MP3ZMRKOXK7XLM5FYVAEVPSCHM.json","view_paper":"https://pith.science/paper/MP3ZMRKO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1707.07521&json=true","fetch_graph":"https://pith.science/api/pith-number/MP3ZMRKOXK7XLM5FYVAEVPSCHM/graph.json","fetch_events":"https://pith.science/api/pith-number/MP3ZMRKOXK7XLM5FYVAEVPSCHM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MP3ZMRKOXK7XLM5FYVAEVPSCHM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MP3ZMRKOXK7XLM5FYVAEVPSCHM/action/storage_attestation","attest_author":"https://pith.science/pith/MP3ZMRKOXK7XLM5FYVAEVPSCHM/action/author_attestation","sign_citation":"https://pith.science/pith/MP3ZMRKOXK7XLM5FYVAEVPSCHM/action/citation_signature","submit_replication":"https://pith.science/pith/MP3ZMRKOXK7XLM5FYVAEVPSCHM/action/replication_record"}},"created_at":"2026-05-18T00:27:46.205451+00:00","updated_at":"2026-05-18T00:27:46.205451+00:00"}