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Title:
MUSTANG: 90 GHz Astronomy on a 100 Meter Telescope
Authors:
Dicker, Simon; Mason, B. S.; Korngut, P. M.; Ade, P. A. R.; Aguirre, J.; Ames, T. J.; Benford, D. J.; Chen, T. C.; Chervenak, J. A.; Cotton, W. D.; Devlin, M. J.; Figueroa-Feliciano, E.; Irwin, K. D.; Maher, S.; Mello, M.; Moseley, S. H.; Tally, D. J.; Tucker, C.; White, S. D.
Affiliation:
AA(University of Pennsylvania), AB(National Radio Astronomy Observatory), AC(University of Pennsylvania), AD(Cardiff University, United Kingdom), AE(University of Pennsylvania), AF(Nasa Goddard Space Flight Center), AG(Nasa Goddard Space Flight Center), AH(Nasa Goddard Space Flight Center), AI(Nasa Goddard Space Flight Center), AJ(National Radio Astronomy Observatory), AK(University of Pennsylvania), AL(Massachusetts Institute of Technology), AM(National Institute of Standards and Technology), AN(Nasa Goddard Space Flight Center), AO(National Radio Astronomy Observatory), AP(Nasa Goddard Space Flight Center), AQ(Nasa Goddard Space Flight Center), AR(Cardiff University, United Kingdom), AS(National Radio Astronomy Observatory)
Publication:
American Astronomical Society, AAS Meeting #213, #474.27; Bulletin of the American Astronomical Society, Vol. 41, p.432
Publication Date:
01/2009
Origin:
AAS
Bibliographic Code:
2009AAS...21347427D

Abstract

MUSTANG, the MUltiplexed SQUID TES Array at Ninety GHz, is an 8 by 8 array of TES bolometers now functioning as a user instrument on the 100 m diameter Green Bank radio Telescope (GBT). MUSTANG is the GBT's first 90 GHz instrument and its first focal plane array. As a continuum receiver on a large single dish, MUSTANG offers a unique combination of 8 arcsecond angular resolution and high sensitivity to extended structure.

During commissioning in the winter of 2007/2008, MUSTANG was able to map a 3 by 3 arcminute square to an RMS noise of 2.5mJy in one hour. In the summer of 2008 MUSTANG's cold optics were changed so as to increase the camera's field of view. This, and improvements to the GBT's surface, have increased signal to noise by a factor of 3 so we now capable of mapping 13 square arcminutes to an RMS noise of 1mJy in one hour. Observers are planning to use this sensitivity to study star-forming regions, high redshift quasars, and distant clusters of galaxies.

This winter MUSTANG will be installed on the GBT in January and will have observations scheduled into the summer. Improvements are being made to the user interface and the data reduction pipeline so that astronomers who wish to use MUSTANG will not need the help of the instrument team. Meanwhile we are hoping to build on MUSTANG's success and are looking forward to the possibility of larger, more sensitive bolometer arrays on the GBT.

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