Observations in the BOOMERanG Field at 1.4 GHz

Details Observations in the BOOMERanG Field at 1.4 GHz Observations in the BOOMERanG Field at 1.4 GHz

Feb 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004mim..proc..201c&link_type=abstract

The Magnetized Interstellar Medium, Proceedings of the conference, held in Antalya, Turkey, September 8 - 12, 2003, Eds: B. Uyan

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The synchrotron emission is expected to be the most important Galactic foreground noise for measurements of the polarization of the Cosmic Microwave Background (CMBP) and the identification of sky areas with low polarized emission by this contaminant is crucial. Observations at low radio frequencies allow both the definition of target regions for deep observations and the estimate of the residual contamination in the frequency range typical of CMBP experiments (30-150 GHz). We present the first observation of the diffuse polarized synchrotron radiation of a patch (about 3 degrees x 3 degres) in the BOOMERanG field, one of the areas with the lowest foreground emission in total intensity. The work has been carried out with the Australia Telescope Compact Array at 1.4 GHz with 3.4 arcmin resolution. The mean polarized signal has been found to be Iprms = sqrt{(Qrms2 + Urms2)} = 11.6 ± 0.6 mK, nearly one order of magnitude below that in the Galactic Plane. Extrapolations to frequencies of interest for cosmological investigations suggest that the detection of the CMBP E-mode should be accessible with no relevant foreground contamination at 90 GHz and even the B-mode detection for T/S > 0.01 is not ruled out.

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