ON THE NATURE OF THE SMALL-SCALE STRUCTURE IN THE COSMIC MICROWAVE BACKGROUND OBSERVED BY PLANCK AND WMAP

Small-scale features observed by Wilkinson Microwave Anisotropy Probe. (WMAP) and PLANCK in the frequency range of 22-90 GHz show a nearly flat spectrum, which meets with expectations that they originate in the early universe. However, free-free emission from electrons in small angular scale galactic sources that suffer beam dilution very closely mimic the observed spectrum in this frequency range. Fitting such a model to the PLANCK and WMAP data shows that the angular size required to fit the data is comparable to the angular width of associated HI filaments found in the Galactic Arecibo L-Band Feed Array-H Isurvey data. Also, the temperature of the electrons is found to be in the range of. 100-300 K. The phenomenon revealed by these data may contribute to a more precise characterization of the foreground masks required to interpret the cosmological aspect of PLANCK and WMAP data.