Macromolecules in the galaxy and the cosmic microwave background

Abstract

A deep search for the predicted Galactic microwave dipole emission of spinning interstellar fullerene-type molecules has been conducted using the RATAN-600 radio telescope. This effect is of interest both in its own right and as a new form of Galactic screen between the cosmic microwave background (CMB) and the observer. The power of this noise component on angular scales of about 0.1° (l=1000) is estimated. These scales are of primary interest for the “Cosmological Gene of the Universe” (RATAN-600), PLANCK Surveyor Mission, and other projects. At the frequencies of the expected emission peak of this dust component, the small-scale noise is a factor of 20 weaker than the predicted noise. It is shown that the role of this dust component is negligible, at least at the main PLANCK frequencies. The first estimates of the contribution from Galactic polarization noise are given for λ=3.9 cm, where the theory predicts a maximum in the CMB polarization (l∼1000). At wavelengths of ∼1 cm and shorter, macromolecules contribute less than 1 µK, and should not hinder CMB polarization studies. Galactic synchrotron polarization, likewise, should not prevent CMB polarization experiments at the main PLANCK frequencies.