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.)

REFERENCES

Link 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).