The SMA submm view of Orion-KL Henrik Beuther 860 and 440mm continuum emission Thermal line emission in the 345 and 690GHz bands (345GHz: ApJL, 616, L31 & ApJ submitted; 690GHz: work in progress) In collaboration with: Q. Zhang, M. Reid, D. Wilner, E. Keto, T. Hunter, H. Shinnaga, P. Ho, J. Moran, M. Gurwell, D. Marrone. R. Rao, L. Humphreys, N. Patel, G. Melnick (all CfA) S.-Y. Liu, C.-M. Chang (both ASIAA)

Spectra at 338 and 348GHz Approximately 150 spectral lines from 26 species 90% of them could be identified Additional low-level emission which needs further work 15% of the lines were not detected by previous single-dish studies (plus low-level emission)

860mm Submillimeter Continuum

860 and 440mm Submm Continuum emission 690GHz observations: UV-coverage not great and calibrator Titan about 40o away ---> imaging difficult! - 2 point sources likely correspond to source I and SMA1 - The SED of I well fits “free-free+dust” - Spectral index of SMA1 S~n3.2

Spectral line emission Toward source I mainly SiO Sulphur-bearing species toward Hot Core and Compact Ridge Sulphur- and oxygen-bearing species toward IRc6 Imaging helps to identify lines Oxygen-bearing molecules weaker toward Hot Core and strong toward Compact Ridge Nitrogen-bearing molecules strong toward Hot Core

Rotation temperatures from CH3OH

Orion-KL: 690 GHz spectra

Line images Source I SMA1

Summary Derive physical properties from source I Identify a new protostellar source SMA1 Imaging the spatial structure of many molecular lines in various submm wavelength bands Temperature structure of the whole region - Using the image capabilities to identify lines