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G.T. Laurent, J.E. Aguirre (University of Colorado), J. Bock (J.P.L.), S. Edgington, M. Enoch (California Institute of Technology), J. Glenn (University of Colorado), A. Goldin (J.P.L.), S. Golwala (California Institute of Technology), D.J. Haig (Cardiff University), P. Maloney (University of Colorado), P. Mauskopf (Cardiff University), H. Nguyen (J.P.L), P. Rossinot, J. Sayers (California Institute of Technology), P. Stover (University of Colorado)
Submillimeter galaxies are dusty, high-redshift galaxies with extreme luminosities (>1012 L\sun) and implied star formation rates (100-1000 M\sun per year). Characterizing submillimeter galaxies is crucial to understanding galaxy formation and evolution. Cumulatively, surveys to date have detected hundreds of these galaxies.
Bolocam is a millimeter-wavelength bolometer-array camera designed for mapping large fields. This survey uses Bolocam to detect submillimeter galaxies at the bright end of the luminosity function. Due to the strong negative K-correction at 1.1 mm, Bolocam's detection sensitivity is approximately uniform for galaxies of a given intrinsic luminosity for redshifts 1 < z < 10.
We present preliminary results from our 1.1 mm galaxy survey made with the Caltech Submillimeter Observatory during January and May 2003. We achieved a sensitivity of 24 mJy s1/2 and integrated down to an rms noise level of approximately 1 mJy over 400 arcmin2 in the Lockman Hole. The data have been processed using our IDL-based analysis pipeline, which removes atmospheric noise and provides diagnostic quantities. Monte Carlo simulations have been implemented to quantify uncertainties, systematic effects, completeness, and source confusion.
This research is funded in part by grants from NASA (NGT5-50384) and NSF (AST-0206158, AST-0098737).
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.