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By Rine Bottinelli A, Ken H. Young B, Richard Chamberlin C, Remo P. J. Tilanus D, Mark A, Gurwell B, Dave J. Wilner B, Hiroko Shinnaga C, Hiroshige Yoshida C, Per Friberg D, Huib Jan Van, Langevelde E, Ewine F. Van Dishoeck A, Michiel R. Hogerheijde A, A. Meredith Hughes B, Robert D. Christensen H, Richard E. Hills G, John S. Richer G, Emily Curtis G and The Esma

Abstract

The eSMA (“extended SMA”) combines the SMA, JCMT and CSO into a single facility, providing enhanced sensitivity and spatial resolution owing to the increased collecting area at the longest baselines. Until ALMA early science observing (2011), the eSMA will be the facility capable of the highest angular resolution observations at 345 GHz. The gain in sensitivity and resolution will bring new insights in a variety of fields, such as protoplanetary/transition disks, high-mass star formation, solar system bodies, nearby and high-z galaxies. Therefore the eSMA is an important facility to prepare the grounds for ALMA and train scientists in the techniques. Over the last two years, and especially since November 2006, there has been substantial progress toward making the eSMA into a working interferometer. In particular, (i) new 345-GHz receivers, that match the capabilities of the SMA system, were installed at the JCMT and CSO; (ii) numerous tests have been performe

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