A&A 501, 801-812 (2009)
DOI: 10.1051/0004-6361/200811267

Multi-frequency measurements of the NVSS foreground sources in the cosmic background imager fields

I. Data release

E. Angelakis¹, A. Kraus¹, A. C. S. Readhead², J. A. Zensus¹, R. Bustos^{3, 4}, T. P. Krichbaum¹, A. Witzel¹, and T. J. Pearson<sup>2

1</sup>  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
    e-mail: angelaki@mpifr-bonn.mpg.de
²  California Institute of Technology, 1200 East California Boulevard, California 91125, Pasadena, USA
³  Universidad de Concepción, Casilla 160-C, Concepción, Chile
⁴  University of Miami, Department of Physics, 1320 Campo Sano Drive, FL 33146, USA

Received 31 October 2008 / Accepted 14 April 2009

Abstract
Context. We present the results of the flux density measurements at 4.85 GHz and 10.45 GHz of a sample of 5998 NVSS radio sources with the Effelsberg 100 m telescope.
Aims. The initial motivation was the need to identify the NVSS radio sources that could potentially contribute significant contaminating flux in the frequency range at which the Cosmic Background Imager experiment operated.
Methods. An efficient way to achieve this challenging goal has been to compute the high frequency flux density of those sources by extrapolating their radio spectrum. This is determined by the three-point spectral index measured on the basis of the NVSS entry at 1.4 GHz and the measurements at 4.85 GHz and 10.45 GHz carried out with the 100 m Effelsberg telescope.
Results. These measurements are important since the targeted sample probes the weak part of the flux density distribution, hence the decision to make the data available.
Conclusions. We present the table with flux density measurements of 3434 sources that showed no confusion allowing reliable measurements, their detection rates, their spectral index distribution and an interpretation which explains satisfactorily the observed uncertainties.

Key words: radio continuum: general -- catalogs -- galaxies: active -- cosmic microwave background

© ESO 2009

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