Beuther, H.Zhang, QizhouReid, MarkHunter, T. R.Gurwell, MarkWilner, DavidZhao, Jun-HuiShinnaga, H.Keto, EricHo, P. T. P.Moran, JamesLiu, S.‐Y.2017-04-072006Beuther, H., Q. Zhang, M. J. Reid, T. R. Hunter, M. Gurwell, D. Wilner, J.‐H. Zhao, et al. 2006. “Submillimeter Array 440 μm/690 GHz Line and Continuum Observations of Orion KL.” The Astrophysical Journal 636 (1) (January): 323–331. doi:10.1086/498015.0004-637Xhttp://nrs.harvard.edu/urn-3:HUL.InstRepos:32095368Submillimeter Array observations of Orion-KL at ∼ 1′′ resolution in the 440 µm/690 GHz band reveal new insights about the continuum and line emission of the region. The 440 µm continuum flux density measurement from source I allows us to differentiate among the various proposed physical models: Source I can be well modeled by a “normal” protostellar SED consisting of a proton-electron free-free emission component at low frequencies and a strong dust component in the submillimeter bands. Furthermore, we find that the protostellar object SMA1 is clearly distinct from the hot core. The non-detection of SMA1 at cm and infrared wavelengths suggests that it may be one of the youngest sources in the entire Orion-KL region. The molecular line maps show emission mainly from the sources I, SMA1 and the hot core peak position. An analysis of the CH 3CN(37 K − 36 K) K-ladder ( K = 0...3) indicates a warm gas component of the order 600 ± 200K. In addition, we detect a large fraction ( ∼ 58%) of unidentified lines and discuss the difficulties of line identifications at these frequencies.en-UStechniques: interferometricstars: formationISM: individual (Orion-KL)ISM: moleculesISM: lines and bandssubmillimeterJournal Article2017-02-2820062017-04-0710.1086/498015