Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...443l..57g&link_type=abstract
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 443, no. 2, p. L57-L60
Astronomy and Astrophysics
Astronomy
103
Anisotropy, Background Radiation, Cosmic Dust, Microwave Spectra, Millimeter Waves, Power Spectra, Astronomical Models, Brightness Temperature, Correlation Detection, Data Reduction, Sky Surveys (Astronomy), Telescopes
Scientific paper
We present results from two observations of the cosmic microwave background (CMB) performed from the South Pole during the 1993-1994 austral summer. Each observation employed a 3 deg peak-to-peak sinusoidal, single-difference chop and consisted of a 20 deg x 1 deg strip on the sky. The first observation used a receiver which operates in three channels between 38 and 45 GHz (Q-band) with a full width half maximum (FWHM) beam which varies from 1 deg to 1.15 deg. The second observation overlapped the first observation and used a receiver which operates in four channels between 26 and 36 GHz (Ka-band) with a FWHM beam which varies from 1.5 deg to 1.7 deg. Significant correlated structure is observed in all channels for each observation. The spectrum of the structure is consistent with a CMB spectrum and is formally inconsistent with diffuse synchrotron and free-free emission at the 5 sigma level. The amplitude of the structure is inconsistent with 20 K interstellar dust; however, the data do not discriminate against flat or inverted spectrum point sources. The root mean square amplitude (+/- 1 sigma) of the combined (Ka + Q) data is Delta Trms = 41.2+15.5-6.7 micro-K for an average window function which has a peak value of 0.97 at l = 68 and drops to e-0.5 of the peak value at l = 36 and l = 106. A band power estimate of the CMB power spectrum, Cl, gives average value of (Cll(l + 1)/(2 pi))B = 1.77+1.58-0.54 x 10-10.
Cook Garry
Figueiredo Newton
Gaier Todd Charles
Gundersen Josh O.
Koch Th.
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