In 1969 Edward Conklin measured the anisotropy in celestial emission at 8 GHz with a resolution of 16.2 ^ { \circ } and used the data to report a detection of the CMB dipole .
Given the paucity of 8 GHz observations over large angular scales and the clear evidence for non-power law Galactic emission near 8 GHz , a new analysis of Conklin ’ s data is informative .
In this paper we compare Conklin ’ s data to that from Haslam et al .
( 0.4 GHz ) , Reich and Reich ( 1.4 GHz ) , and WMAP ( 23-94 GHz ) .
We show that the spectral index between Conklin ’ s data and the 23 GHz WMAP data is \beta = -1.7 \pm 0.1 , where we model the emission temperature as T \propto \nu ^ { \beta } .
Free-free emission has \beta \approx - 2.15 , synchrotron emission has \beta \approx - 2.7 to -3 .
Thermal dust emission ( \beta \approx 1.7 ) is negligible at 8 GHz .
We conclude that there must be another distinct non-power law component of diffuse foreground emission that emits near 10 GHz , consistent with other observations in this frequency range .
By comparing to the full complement of data sets , we show that a model with an anomalous emission component , assumed to be spinning dust , is preferred over a model without spinning dust at 5 \sigma ( \Delta \chi ^ { 2 } = 31 ) .
However , the source of the new component can not be determined uniquely .