Hostname: page-component-78c5997874-t5tsf Total loading time: 0 Render date: 2024-11-05T06:48:08.593Z Has data issue: false hasContentIssue false

Polarized Microwave Radiation from Dust

Published online by Cambridge University Press:  26 May 2016

A. Lazarian*
Affiliation:
Department of Astronomy, University of Wisconsin, Madison, WI 53706, USA

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Observations of cosmic microwave background in the range 10-90 GHz have revealed an anomalous foreground component well correlated with 12 μm, 60 μm and 100 μm emission from interstellar dust. As the recent cross-correlation analysis of WHAM Hα maps with the Tenerife 10 and 15 GHz maps supports an earlier conclusion that the emission does not arise from free-free radiation, the interstellar dust origin of it is left as the only suspect. Two competing models of this emission exist. The more favored at the moment is the spinning dust model, the other is the model that uses grains with strong magnetic response. In the spinning dust model the emission arises from rapid rotation of ultrasmall grains that have dipole moments, while in the other model magnetic grains emit due to thermal vibrations of magnetic dipoles. Both models predict the emission to be partially polarized and this emission can seriously interfere with the CMB polarization measurements. We discuss observational signatures that can be used to distinguish and eventually filter out the polarized component of the microwave dust radiation.

Type
Part IV: Interpreting CMB Observations
Copyright
Copyright © Astronomical Society of the Pacific 2005 

References

Altshuler, S. A. & Kozyrev, B. M. 1964, Electron Paramagnetic Resonance, Academic Press, New York.Google Scholar
Atherton, N. M. 1973, Electron Spin Resonance, John Willey & Sons, New York.Google Scholar
Davies, R. D. & Wilkinson, A. 1999 in ASP Conf. Ser. Vol. 181, “Microwave Foregrounds”, eds. de Oliveira-Costa, Angelica and Tegmark, Max, (San Francisco: ASP), 77 (henceforth “Microwave Foregrounds”).Google Scholar
Bloch, F. 1946, Phys. Rev., 70, 460.CrossRefGoogle Scholar
Boulanger, F. & Pérault, M. 1988, ApJ, 330, 964.Google Scholar
Davis, L. & Greenstein, J. L. 1951, ApJ, 114, 206.Google Scholar
de Oliveira-Costa, et al. 1997, ApJ, 482, L17.CrossRefGoogle Scholar
de Oliveira-Costa, et al. 1998, ApJ, 509, L9.CrossRefGoogle Scholar
de Oliveira-Costa, et al. 1999, ApJ, 527, L9.CrossRefGoogle Scholar
de Oliveira-Costa, et al. 2000, ApJ, submitted (astro-ph 0010527).Google Scholar
Désert, Boulanger, F. & Puget, J. L. 1990, A & A 237, 215.Google Scholar
Draine, B. T. & Lazarian, A. 1998a, ApJ, 494, L19 (DL98a).Google Scholar
Draine, B. T. & Lazarian, A. 1998b, ApJ, 508, 157 (DL98b).Google Scholar
Draine, B. T. & Lazarian, A. 1999, ApJ, 512, 000 (DL99).Google Scholar
Draine, B. T. & Lazarian, A. 1999 in “Microwave Foregrounds”, 133.Google Scholar
Finkbeiner, D. P. et al. 2000 preprint.Google Scholar
Goodman, A. A. & Whittet, D. C. B. 1995, ApJ, 455, L181.Google Scholar
Haslam, C. G. T. et al. 1982, A&AS, 47, 1.Google Scholar
Hildebrand, R. H. 1988, QJRAS, 29, 327.Google Scholar
Jones, R. V. & Spitzer, L. Jr. 1967, ApJ, 147, 943.Google Scholar
Kogut, A. et al. 1996a, ApJ, 460, 1.Google Scholar
Kogut, A. et al. 1996b, ApJ, 464, L5.Google Scholar
Kogut, A. 1999 in “Microwave Foregrounds”, 91.Google Scholar
Landau, L. D. & Lifshitz, E. M. 1960, Electrodynamics of continuous Media, Reading, MA: Addison-Wesley, p. 144.Google Scholar
Lazarian, A. 2000, astro-ph/0003314.Google Scholar
Lazarian, A. & Efroimsky, M. 1999, MNRAS, 303, 673.Google Scholar
Lazarian, A. & Draine, B. T. 1999, ApJ, 520, L67.Google Scholar
Lazarian, A. & Draine, B. T. 2000, ApJ, 535, L15.Google Scholar
Lazarian, A. & Roberge, W. G. 1997, ApJ, 484, 230.CrossRefGoogle Scholar
Léger, A. & Puget, J. L. 1984, ApJ, 278, L19.Google Scholar
Li, A. & Draine, B. T. 2001, in preparation.Google Scholar
Martin, P. G. 1995, ApJ, 445, L63.Google Scholar
Mathis, J. S. 1986, ApJ, 308, 281.Google Scholar
McCullough, et al. 1999 “Microwave Foregrounds”, 253.Google Scholar
Mikheerjee, P. et al. 2000, astro-ph/0002305.Google Scholar
Omont, A. 1986, A&A, 164, 159.Google Scholar
Prunet, S. & Lazarian, A. 1999 “Microwave Foregrounds”, 113.Google Scholar
Reich, P. & Reich, W. 1988, A&AS, 74, 7.Google Scholar
Savage, B. D. & Sembach, K. R. 1996, ARA&A, 34, 279.Google Scholar
Staggs, S. T., Gundersen, J. O. & Church, S. E. 1999 “Microwave Foregrounds”, 299.Google Scholar
Tegmark, et al. 1999 in “Microwave Foregrounds”, 3.Google Scholar
Weingartner, J. C. & Draine, B. T. 2000, astro-ph/0010117.Google Scholar
Weingartner, J. C. & Draine, B. T. 2001, ApJ, 548, 000.CrossRefGoogle Scholar