Aa 400, 1163--1172 (2003)

To investigate the low-atmosphere turbulence at the South Pole, we have measured, using a SODAR, the temperature fluctuation constant (C T ) during winter, as a function of altitude up to 890 m. We found that the turbulence was on average concentrated inside a boundary layer sitting below 270 m. While at the peak of winter the turbulence was stable and clearly bounded, during other seasons there was a more complex turbulence profile which extended to higher altitudes. We found that this behaviour could be explained by the horizontal wind speed conditions whose altitude profile closely matched the turbulence profile. We also observed the presence of a vertical wind velocity change of direction at an altitude range corresponding to the turbulent region. The turbulence gives rise to an average seeing of 1.73 ## , which compares poorly with the best astronomy sites

Draft: March 17, 2006 Wilkinson Microwave Anisotropy Probe (WMAP) Three Year

A simple cosmological model with only six parameters (matter density, , baryon , Hubble Constant, H 0 , amplitude of fluctua1 Dept. of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544-1001 Visiting Scientist, Cerro-Tololo Inter-American Observatory 612 Space Sciences Building, Cornell University, Ithaca, NY 14853 Canadian Institute for Theoretical Astrophysics, 60 St. George St, University of Toronto, Toronto, ON Canada M5S 3H8 Dept. of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544-0708 Code 665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771 Dept. of Physics & Astronomy, The Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218-2686 Department of Astronomy, University of Texas, Austin, TX Depts. of Astrophysics and Physics, KICP and EFI, University of Chicago, Chicago, IL 60637 Hubble Fellow 11 Department of Physics, University of Pennsylvania, Philadelphia, PA Dept. of Physics and Astronomy, University of British Columbia, Vancouver, BC Canada V6T 1Z1 Dept. of Physics, Brown University, 182 Hope St., Providence, RI 02912-1843 UCLA Astronomy, PO Box 951562, Los Angeles, CA 90095-1562 15 Science Systems and Applications, Inc. (SSAI), 10210 Greenbelt Road, Suite 600 Lanham, Maryland 20706 -- 2 -- tions, # 8 , optical depth, # , and a slope for the scalar perturbation spectrum, n s ) fits not only the three year WMAP temperature and polarization data, but also small scale CMB data, light element abundances, largescale structure observations, and the supernova luminosity/distance relationship