{ "id": "1611.00855", "version": "v1", "published": "2016-11-03T01:18:42.000Z", "updated": "2016-11-03T01:18:42.000Z", "title": "ALMA band 8 continuum emission from Orion Source I", "authors": [ "Tomoya Hirota", "Masahiro N. Machida", "Yuko Matsushita", "Kazuhito Motogi", "Naoko Matsumoto", "Mi Kyoung Kim", "Ross A. Burns", "Mareki Honma" ], "comment": "5 pages, 2 figures, accepted for publication in the The Astrophysical Journal", "categories": [ "astro-ph.GA", "astro-ph.SR" ], "abstract": "We have measured continuum flux densities of a high-mass protostar candidate, a radio source I in the Orion KL region (Orion Source I) using the Atacama Large Millimeter/Submillimeter Array (ALMA) at band 8 with an angular resolution of 0.1\". The continuum emission at 430, 460, and 490 GHz associated with Source I shows an elongated structure along the northwest-southeast direction perpendicular to the so-called low-velocity bipolar outflow. The deconvolved size of the continuum source, 90 au times 20 au, is consistent with those reported previously at other millimeter/submillimeter wavelength. The flux density can be well fitted to the optically thick black-body spectral energy distribution (SED), and the brightness temperature is evaluated to be 700-800 K. It is much lower than that in the case of proton-electron or H- free-free radiations. Our data are consistent with the latest ALMA results by Plambeck & Wright (2016), in which the continuum emission have been proposed to arise from the edge-on circumstellar disk via thermal dust emission, unless the continuum source consists of an unresolved structure with the smaller beam filling factor.", "revisions": [ { "version": "v1", "updated": "2016-11-03T01:18:42.000Z" } ], "analyses": { "keywords": [ "continuum emission", "orion source", "alma band", "thick black-body spectral energy distribution", "optically thick black-body spectral energy" ], "note": { "typesetting": "TeX", "pages": 5, "language": "en", "license": "arXiv", "status": "editable" } } }