Microwave Emission from Galactic Dust Grains
Abstract
Observations of the cosmic microwave background have revealed a component of 10-60 GHz emission from the Galaxy which correlates with 100-140um emission from interstellar dust but has an intensity much greater than expected for the low-frequency tail of the "electric dipole vibrational" emission peaking at \~130um. This "anomalous emission" is more than can be accounted for by dust-correlated free-free emission. The anomalous emission could be due in part to magnetic dipole emission from thermal fluctuations of the magnetization within interstellar dust grains, but only if a substantial fraction of the Fe in interstellar dust resides in magnetic materials such as metallic iron or magnetite. The observed anomalous emission is probably due primarily to electric dipole radiation from spinning ultrasmall interstellar dust grains. This rotational emission is expected to be partially polarized. From the standpoint of minimizing confusion with non-CBR foregrounds, 60-120 GHz appears to be the optimal frequency window.
Cite
@article{arxiv.astro-ph/9902356,
title = {Microwave Emission from Galactic Dust Grains},
author = {B. T. Draine and A. Lazarian},
journal= {arXiv preprint arXiv:astro-ph/9902356},
year = {2007}
}
Comments
Invited review for the "Sloan Summit on Microwave Foregrounds", ed. A. de Oliveira-Costa and M. Tegmark. Latex, paspconf style, 17 pages including 7 eps figures