{"paper":{"title":"Spitzer as Microlens Parallax Satellite: Mass Measurement for the OGLE-2014-BLG-0124L Planet and its Host Star","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"A. Gould, A. Udalski, C. Han, G. Pietrzy\\'nski, I. Soszy\\'nski, J.C. Yee, J. Skowron, K. Ulaczyk, {\\L}. Wyrzykowski, M.K. Szyma\\'nski, P. Mr\\'oz, P. Pietrukowicz, R. Poleski, R.W. Pogge, S. Calchi Novati, S. Carey, S. Koz{\\l}owski, W. Zhu","submitted_at":"2014-10-15T20:28:15Z","abstract_excerpt":"We combine Spitzer and ground-based observations to measure the microlens parallax vector ${\\mathbf \\pi}_{\\rm E}$, and so the mass and distance of OGLE-2014-BLG-0124L, making it the first microlensing planetary system with a space-based parallax measurement. The planet and star have masses $m \\sim 0.5\\,M_{\\rm jup}$ and $M\\sim 0.7\\,M_\\odot$ and are separated by $a_\\perp\\sim 3.1$ AU in projection. The main source of uncertainty in all these numbers (approximately 30%, 30%, and 20%) is the relatively poor measurement of the Einstein radius $\\theta_{\\rm E}$, rather than uncertainty in $\\pi_{\\rm E}"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1410.4219","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"}