ball1.gif Viper

Peterson et al. use Q band (centered on 40 GHz) data from the ground-based Viper experiment at the South Pole to constrain CMBR anisotropy.

The window functions were provided by G. Griffin. The first column in the window function file is $\ell$, which runs from 2 to 2200. The next six columns are the Viper zero-lag $W_\ell$'s.


Table: Viper zero-lag Window Function Parameters
$\ell_{e^{-0.5}}$ $\ell_{\rm e}$ $\ell_{\rm m}$ $\ell_{e^{-0.5}}$ $\sqrt{I(W_\ell)}$
46 108.4 84 135 1.77
92 172.8 136 193 1.07
148 237.4 206 283 0.893
157 263.1 286 441 1.37
298 422.4 444 607 0.627
443 587.7 610 794 0.337

The quoted bandtemperature values are computed for a flat bandpower spectrum. They are from Peterson et al., with 8% added in quadrature to the statistical 1 $\sigma$ error bars to account for the 1 $\sigma$ calibration uncertainty.

Fig.: Viper zero-lag window functions. (Postscript version here.) win_Viper.gif

REFERENCES

ball23.gifLink to the experiment webpage.

J.B. Peterson, et al., ``First Results from Viper: Detection of Small-Scale Anisotropy at 40 GHz",Astrophys. J. Lett. 532, L83 (2000).


Bharat Ratra and Tarun Souradeep
Department of Physics, Kansas State University
Last updated: 2000-08-31