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This binary may serve as a benchmark for metallicity measurement calibrations and as a test-bed for atmospheric and evolutionary models for esdM objects.\n  We determine abundances primarily using high resolution optical spectra of the primary. Other parameters were determined from the fits of synthetic spectra computed with these abundances to the observed spectra from 0.4 to 2.5 microns for both components.\n  We determine \\Tef =4625 $\\pm$ 100 K, \\l"},"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":"1507.07740","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2015-07-28T12:34:12Z","cross_cats_sorted":[],"title_canon_sha256":"8a5c4a3f5ee43374b22848e8d0bad9ea448d7009eaa3b4edcf4de866eefddcb5","abstract_canon_sha256":"8a1326a4f1cc412060c8a2f93206168b8e469b4f2b34fc44301fda4c82d7c352"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:29:45.242737Z","signature_b64":"eFvLsyX2/SW7rx7UxARIJC3TwRK9cmc8Hi+BbXT8jCDu/z7WnlAI01feUNID/lNutewyXNlXpdQp6DxLqjEUDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"148de30568995f4c1e879d6cb2781859384349166ae23a981575e4d850e35ea3","last_reissued_at":"2026-05-18T01:29:45.242277Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:29:45.242277Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Probing M subdwarf metallicity with an esdK5+esdM5.5 binary","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"H.R.A. Jones (UH), I.O. Kushniruk (UKyiv), MAO), M.C. G\\'alvez-Ortiz (CSIC-INTA, UH), UL), Ya.V. Pavlenko (UH, Z.H. Zhang (IAC","submitted_at":"2015-07-28T12:34:12Z","abstract_excerpt":"We present a spectral analysis of the binary G 224-58 AB that consists of the coolest M extreme subdwarf (esdM5.5) and a brighter primary (esdK5). This binary may serve as a benchmark for metallicity measurement calibrations and as a test-bed for atmospheric and evolutionary models for esdM objects.\n  We determine abundances primarily using high resolution optical spectra of the primary. 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