On the Small-Scale Distribution of Galactic Dust

Details On the Small-Scale Distribution of Galactic Dust On the Small-Scale Distribution of Galactic Dust

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21540701s&link_type=abstract

American Astronomical Society, AAS Meeting #215, #407.01; Bulletin of the American Astronomical Society, Vol. 42, p.231

Astronomy and Astrophysics

Astronomy

Scientific paper

Galactic dust absorbs UV and optical light, re-emitting radiation at microwave frequencies. This emission is one of the dominant foregrounds for Cosmic Microwave Background (CMB) experiments. Characterizing the distribution of interstellar dust in the Galaxy is therefore an important goal in the community's quest to accurately separate its emission from the CMB. The current state-of-the-art dust map was produced by Schlegel, Finkbeiner and Davis (SFD) with data from the COBE/DIRBE and IRAS satellite missions. This full-sky map has a resolution of 6.1'. However, the current generation of microwave experiments, including the Atacama Cosmology Telescope (ACT) and the South Pole Telescope (SPT), operates at resolutions of about 1'. In order to shed light on the small-scale distribution of Galactic dust, we take advantage of the fact that dust emission is not correlated with the CMB. By cross-correlating microwave data from ACT observations with the SFD map, we study the statistical properties of the Galactic dust distribution at small angular scales. We then use Spitzer data to build a higher resolution dust map in the ACT field. The cross-correlation of this new template with the SFD map enables us to improve on our previous analysis.

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