Polarized Diffuse Emission at 2.3 GHz in a High Galactic Latitude Area

Details Polarized Diffuse Emission at 2.3 GHz in a High Galactic Latitude Area Polarized Diffuse Emission at 2.3 GHz in a High Galactic Latitude Area

2005-03-02

arxiv.org/abs/astro-ph/0503043v1

Mon.Not.Roy.Astron.Soc.Lett.360:L10-L14,2005

Astronomy and Astrophysics

Astrophysics

5 pages, 6 figures, accepted for publication in MNRAS Letters

Scientific paper

10.1111/j.1745-3933.2005.00034.x

Polarized diffuse emission observations at 2.3 GHz in a high Galactic latitude area are presented. The 2\degr X 2\degr field, centred in (\alpha=5^h,\delta=-49\degr), is located in the region observed by the BOOMERanG experiment. Our observations has been carried out with the Parkes Radio telescope and represent the highest frequency detection done to date in low emission areas. Because of a weaker Faraday rotation action, the high frequency allows an estimate of the Galactic synchrotron contamination of the Cosmic Microwave Background Polarization (CMBP) that is more reliable than that done at 1.4 GHz. We find that the angular power spectra of the E- and B-modes have slopes of \beta_E = -1.46 +/- 0.14 and \beta_B = -1.87 +/- 0.22, indicating a flattening with respect to 1.4 GHz. Extrapolated up to 32 GHz, the E-mode spectrum is about 3 orders of magnitude lower than that of the CMBP, allowing a clean detection even at this frequency. The best improvement concerns the B-mode, for which our single-dish observations provide the first estimate of the contamination on angular scales close to the CMBP peak (about 2 degrees). We find that the CMBP B-mode should be stronger than synchrotron contamination at 90 GHz for models with T/S > 0.01. This low level could move down to 60-70 GHz the optimal window for CMBP measures.

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