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G.T. Laurent, J. Aguirre (U. Colorado), J. Bock (JPL), S. Edgington, M. Enoch (Caltech), J. Glenn (U. Colorado), A. Goldin (JPL), S. Golwala (Caltech), D. Haig (U. Wales), P. Maloney (U. Colorado), P. Mauskopf (U. Wales), H. Hguyen (JPL), P. Rossinot, J. Sayers (Caltech), P. Stover (U. Colorado)
Submillimeter galaxies are dusty, high-redshift galaxies with extreme luminosities (>1012 Lsolar) and implied star formation rates (100-1000 Msolar 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 final results from our 1.1 mm galaxy survey made with the Caltech Submillimeter Observatory during January and May 2003. A source list and number counts are presented with the statistical significance of each potential source. Monte-Carlo simulations with real and simulated data were implemented to confirm the robustness of our source candidates, quantify our false detection rate, determine our detection threshold and completeness of this survey, and estimate the impact of source confusion. We compare our estimates of submillimeter counts with estimates derived from other surveys and models.
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, 36 #2
© YEAR. The American Astronomical Soceity.