Foregrounds for observations of the cosmological 21 cm line
II. Westerbork observations of the fields around 3C 196 and the North Celestial Pole
Kapteyn Astronomical Institute, University of Groningen,
PO Box 800,
2 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
3 ASTRON, PO Box 2, 7990 AA Dwingeloo, The Netherlands
4 Max-Planck Institute for Astrophysiscs, Karl-Schwarzschild-Straße 1, 85748 Garching, Germany
5 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
6 Institute for the Mathematics and Physics of the Universe (IPMU), The University of Tokyo, Chiba 277-8582, Japan
Accepted: 4 August 2010
Context. In the coming years a new insight into galaxy formation and the thermal history of the Universe is expected to come from the detection of the highly redshifted cosmological 21 cm line.
Aims. The cosmological 21 cm line signal is buried under Galactic and extragalactic foregrounds which are likely to be a few orders of magnitude brighter. Strategies and techniques for effective subtraction of these foreground sources require a detailed knowledge of their structure in both intensity and polarization on the relevant angular scales of 1–30 arcmin.
Methods. We present results from observations conducted with the Westerbork telescope in the 140–160 MHz range with 2 arcmin resolution in two fields located at intermediate Galactic latitude, centred around the bright quasar 3C 196 and the North Celestial Pole. They were observed with the purpose of characterizing the foreground properties in sky areas where actual observations of the cosmological 21 cm line could be carried out. The polarization data were analysed through the rotation measure synthesis technique. We have computed total intensity and polarization angular power spectra.
Results. Total intensity maps were carefully calibrated, reaching a high dynamic range, 150 000:1 in the case of the 3C 196 field. No evidence of diffuse Galactic emission was found in the angular power spectrum analysis on scales smaller than ~10 arcmin in either of the two fields. On these angular scales the signal is consistent with the classical confusion noise of ~3 mJy beam-1. On scales greater than 30 arcmin we found an excess of power attributed to the Galactic foreground with an rms of 3.4 K and 5.5 K for the 3C 196 and the NCP field respectively. The intermediate angular scales suffered from systematic errors which prevented any detection.
Patchy polarized emission was found only in the 3C 196 field whereas the polarization in the NCP area was essentially due to radio frequency interference. The polarized signal in the 3C 196 field is close to the thermal noise for angular scales smaller than ~10 arcmin. On scales greater than 30 arcmin it has an rms value of 0.68 K. The polarized signal appears mainly at rotation measure values smaller than 4 rad m-2.
Conclusions. In regard of the detection of the cosmological 21 cm line, we conclude that Galactic total intensity emission lacks small-scale power, which is below the confusion noise level at the angular resolution of 2 arcmin. Galactic polarization, given its relative weakness and its small rotation measure values, is less severe than expected as a contaminant of the cosmological 21 cm line.
Key words: polarization / diffuse radiation / cosmology: observations / ISM: general
© ESO, 2010