Detalles de publicación
PP 09066
Follow-up observations at 16 and 33GHz of extragalactic sources from WMAP 3-yr data: I - Spectral properties
(1) Astrophysics Group, Cavendish Laboratory, University of Cambridge
(2) Jodrell Bank Centre for Astrophysics, University of Manchester
(3) Instituto de Astrofísica de Canarias, Universidad de La Laguna
(4) Kavli Institute for Cosmology Cambridge
We present follow-up observations of 97 point sources from the Wilkinson Microwave Anisotropy Probe (WMAP) 3-yr data, contained within the New Extragalactic WMAP Point Source catalogue between −4 deg ≤δ ≤60 deg; the sources form a flux-density-limited sample complete to 1.1 Jy (≈5σ) at 33 GHz. Our observations were made at 16 GHz using the Arcminute Microkelvin Imager and at 33 GHz with the Very Small Array (VSA).
94 of the sources have reliable, simultaneous – typically a few minutes apart – observations with both telescopes. The spectra between 13.9 and 33.75 GHz are very different from those of bright sources at low frequency: 44 per cent have rising spectra (α(33.75,13.9) < 0.0), where S ∝ ν^−α, and 93 per cent have spectra with α(33.75,13.9) < 0.5); the median spectral index is 0.04.
For the brighter sources, the agreement between VSA and WMAP 33-GHz flux densities averaged over sources is very good. However, for the fainter sources, the VSA tends to measure lower values for the flux densities than WMAP. We suggest that the main cause of this effect is the Eddington bias arising from variability.
94 of the sources have reliable, simultaneous – typically a few minutes apart – observations with both telescopes. The spectra between 13.9 and 33.75 GHz are very different from those of bright sources at low frequency: 44 per cent have rising spectra (α(33.75,13.9) < 0.0), where S ∝ ν^−α, and 93 per cent have spectra with α(33.75,13.9) < 0.5); the median spectral index is 0.04.
For the brighter sources, the agreement between VSA and WMAP 33-GHz flux densities averaged over sources is very good. However, for the fainter sources, the VSA tends to measure lower values for the flux densities than WMAP. We suggest that the main cause of this effect is the Eddington bias arising from variability.