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Our modeling results in a parallax, $\\pi_{abs} = 21.96\\pm0.12$ milliseconds of arc, a mass for HD 202206 B of M$_B = 0.089^{ +0.007}_{-0.006}$ Msun, and a mass for HD 202206 c of M$_c = 17.9 ^{ +2.9}_{-1.8}$ MJup. HD 202206 is a nearly face-on G+M binary orbited by a brown dwarf. The system architecture we determine supports past assertions that stability requires a 5:1 mean motion resonance (we find a period ratio, $P_c/P_B = 4.92\\pm0.04$)"},"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":"1705.00659","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2017-05-01T18:47:06Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"f8c74496e0b1992ebaf476398e6be04a0d5a3b84063ea5dbf658eb1793f1795b","abstract_canon_sha256":"66691a3414e4cb411ec9b28e521b5fce749b1a1c524b5dde08e0e6428faac566"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:43:25.277324Z","signature_b64":"LKSTcJo7iGsB4QQ/euzCF4DzIjwqL+Jsm41MXbyBrQHbs6eZ/G5N6IsiSgRXChrspGcHsEGF4Y854UuS4O/hBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1c9dd9f81c3a4916b5e551ccb6a06398b9295baa4c0bc2e49eef6cd95b4bbdb7","last_reissued_at":"2026-05-18T00:43:25.276685Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:43:25.276685Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"HD 202206 : A Circumbinary Brown Dwarf System","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"G. Fritz Benedict, Thomas E. Harrison","submitted_at":"2017-05-01T18:47:06Z","abstract_excerpt":"With Hubble Space Telescope Fine Guidance Sensor astrometry and previously published radial velocity measures we explore the exoplanetary system HD 202206. Our modeling results in a parallax, $\\pi_{abs} = 21.96\\pm0.12$ milliseconds of arc, a mass for HD 202206 B of M$_B = 0.089^{ +0.007}_{-0.006}$ Msun, and a mass for HD 202206 c of M$_c = 17.9 ^{ +2.9}_{-1.8}$ MJup. HD 202206 is a nearly face-on G+M binary orbited by a brown dwarf. 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