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Published January 10, 2012 | Submitted + Published
Journal Article Open

143 GHz brightness measurements of Uranus, Neptune, and other secondary calibrators with Bolocam between 2003 and 2010


Bolocam began collecting science data in 2003 as the long-wavelength imaging camera at the Caltech Submillimeter Observatory. The planets, along with a handful of secondary calibrators, have been used to determine the flux calibration for all of the data collected with Bolocam. Uranus and Neptune stand out as the only two planets that are bright enough to be seen with high signal-to-noise in short integrations without saturating the standard Bolocam readout electronics. By analyzing all of the 143 GHz observations made with Bolocam between 2003 and 2010, we find that the brightness ratio of Uranus to Neptune is 1.027 ± 0.006, with no evidence for any variations over that period. Including previously published results at ≃ 150 GHz, we find a brightness ratio of 1.029 ± 0.006 with no evidence for time variability over the period 1983-2010. Additionally, we find no evidence for time variability in the brightness ratio of either Uranus or Neptune to the ultracompact H II region G34.3 or the protostellar source NGC 2071IR. Using recently published Wilkinson Microwave Anisotropy Probe results we constrain the absolute 143 GHz brightness of both Uranus and Neptune to ≃ 3%. Finally, we present ≃ 3% absolute 143 GHz peak flux density values for the ultracompact H II regions G34.3 and K3-50A and the protostellar source NGC 2071IR.

Additional Information

© 2012 The American Astronomical Society. Received 2011 October 16; accepted 2011 November 30; published 2011 December 22. We acknowledge the assistance of the Bolocam instrument team: Peter Ade, James Aguirre, James Bock, Sam Edgington, Jason Glenn, Alexy Goldin, Sunil Golwala, Douglas Haig, Andrew Lange, Glenn Laurent, Phil Mauskopf, Hien Nguyen, Philippe Rossinot, and Jack Sayers; Matt Ferry, Matt Hollister, Patrick Koch, Kai-Yang Lin, Sandor Molnar, Seth Siegel, and Keiichi Umetsu who, in addition to the Bolocam instrument team, helped collect the data presented in this manuscript; the day crew and Hilo staff of the Caltech Submillimeter Observatory, who provided invaluable assistance during commissioning and data-taking for this data set; Kathy Deniston, Barbara Wertz, and Diana Bisel, who provided effective administrative support at Caltech and in Hilo; and the referee, who provided helpful comments and suggestions. Bolocam was constructed and commissioned using funds from NSF/AST-9618798, NSF/AST-0098737, NSF/AST-9980846, NSF/AST-0229008, and NSF/AST-0206158. J.S. was partially supported by a NASA Graduate Student Research Fellowship, a NASA Postdoctoral Program Fellowship, NSF/AST-0838261, and NASA/NNX11AB07G; N.C. was partially supported by NASA Graduate Student Research Fellowship; S.G. acknowledges an Alfred P. Sloan Foundation Fellowship.

Attached Files

Published - Sayers_2012_ApJ_744_169.pdf

Submitted - 1110.3473v1.pdf


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