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Proceedings Paper

The eSMA: description and first results
Author(s): Sandrine Bottinelli; Ken H. Young; Richard Chamberlin; Remo P. J. Tilanus; Mark A. Gurwell; Dave J. Wilner; Hiroko Shinnaga; Hiroshige Yoshida; Per Friberg; Huib Jan van Langevelde; Ewine F. van Dishoeck; Michiel R. Hogerheijde; A. Meredith Hughes; Robert D. Christensen; Richard E. Hills; John S. Richer; Emily Curtis
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Paper Abstract

The eSMA ("expanded 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 performed for receiver, correlator and baseline calibrations in order to determine and take into account the effects arising from the differences between the three types of antennas; (iii) First fringes at 345 GHz were obtained on August 30 2007, and the array has entered the science-verification stage. We report on the characteristics of the eSMA and its measured performance at 230 GHz and that expected at 345 GHz. We also present the results of the commissioning and some initial science-verification observations, including the first absorption measurement of the C/CO ratio in a galaxy at z=0.89, located along the line of sight to the lensed quasar PKS 1830-211, and on the imaging of the vibrationally excited HCN line towards IRC+10216.

Paper Details

Date Published: 10 July 2008
PDF: 12 pages
Proc. SPIE 7012, Ground-based and Airborne Telescopes II, 70120D (10 July 2008); doi: 10.1117/12.788949
Show Author Affiliations
Sandrine Bottinelli, Leiden Observatory, Leiden Univ. (Netherlands)
Ken H. Young, Harvard-Smithsonian Ctr. for Astrophysics (United States)
Richard Chamberlin, Caltech Submillimeter Observatory (United States)
Remo P. J. Tilanus, Joint Astronomy Ctr. (United States)
Netherlands Organisation for Scientific Research (Netherlands)
Mark A. Gurwell, Harvard-Smithsonian Ctr. for Astrophysics (United States)
Dave J. Wilner, Harvard-Smithsonian Ctr. for Astrophysics (United States)
Hiroko Shinnaga, Caltech Submillimeter Observatory Office (United States)
Hiroshige Yoshida, Caltech Submillimeter Observatory Office (United States)
Per Friberg, Joint Astronomy Ctr. (United States)
Huib Jan van Langevelde, Joint Institute for VLBI in Europe (Netherlands)
Leiden Observatory, Leiden Univ. (Netherlands)
Ewine F. van Dishoeck, Leiden Observatory, Leiden Univ. (Netherlands)
Max-Planck-Institut für Extraterrestrische Physik (Germany)
Michiel R. Hogerheijde, Leiden Observatory, Leiden Univ. (Netherlands)
A. Meredith Hughes, Harvard-Smithsonian Ctr. for Astrophysics (United States)
Robert D. Christensen, Harvard-Smithsonian Ctr. for Astrophysics (United States)
Richard E. Hills, Cavendish Lab., Univ. of Cambridge (United Kingdom)
John S. Richer, Cavendish Lab., Univ. of Cambridge (United Kingdom)
Emily Curtis, Cavendish Lab., Univ. of Cambridge (United Kingdom)

Published in SPIE Proceedings Vol. 7012:
Ground-based and Airborne Telescopes II
Larry M. Stepp; Roberto Gilmozzi, Editor(s)

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