Gundersen et al. use Ka band (centered on 30 GHz) and Q band (centered on
40 GHz) data from the ground-based UCSB South Pole 1994 experiment at the
South Pole to constrain CMBR anisotropy. Ganga et al. summarize the experiment.
The Ka band is multiplexed into four channels (channel number
centered at frequency
GHz) and the Q
band is multiplexed into three (channel number ,
The FWHM of the beams, assumed to be gaussian, are
for (both one
deviation uncertainty). The zero-lag window function of the smooth-scan, square
wave lockin experiment, for channels is
Gundersen et al. define data-weighted average windows,
The first column in the window function file
is , which runs from
2 to 400. The second and third columns are data-weighted Ka and Q band
The quoted bandtemperature values are from Ganga et al.. They were computed
assuming a flat bandpower spectrum and account for the UCSB South Pole 1994
absolute calibration uncertainty of 10% as well as the beamwidth uncertainty.
Ganga et al. and Ratra et al. use the UCSB South Pole 1994 data to constrain
Link to the experiment webpage.
K. Ganga, B. Ratra, J.O. Gundersen, and N. Sugiyama, ``UCSB South Pole
1994 Cosmic Microwave Background Anisotropy Measurement Constraints on
Open and Flat- Cold Dark Matter Cosmogonies",
Astrophys. J. 484, 7
J.O. Gundersen, et al., ``Degree-Scale Anisotropy in the Cosmic Microwave
Background: SP94 Results", Astrophys. J. Lett. 443, L57 (1995).
B. Ratra, R. Stompor, K. Ganga, G. Rocha, N. Sugiyama, and K.M. Górski, ``Cosmic Microwave Background Anisotropy Constraints on Open and Flat- Cold Dark Matter Cosmogonies from UCSB South Pole, ARGO, MAX, White Dish, and SuZIE Data", Astrophys. J. 517, 549 (1999).