We have surveyed two science fields totaling one square degree with Bolocam at 2.1 mm to search for secondary CMB anisotropies caused by the Sunyaev-Zel ’ dovich effect ( SZE ) .
The fields are in the Lynx and Subaru/XMM SDS1 fields .
Our survey is sensitive to angular scales with an effective angular multipole of \ell _ { eff } = 5700 with FWHM _ { \ell } = 2800 and has an angular resolution of 60 arcseconds FWHM .
Our data provide no evidence for anisotropy .
We are able to constrain the level of total astronomical anisotropy , modeled as a flat band power in \mathcal { C } _ { \ell } , with frequentist 68 % , 90 % , and 95 % CL upper limits of 590 , 760 , and 830 \mu K _ { CMB } ^ { 2 } .
We statistically subtract the known contribution from primary CMB anisotropy , including cosmic variance , to obtain constraints on the SZE anisotropy contribution .
Now including flux calibration uncertainty , our frequentist 68 % , 90 % and 95 % CL upper limits on a flat band power in \mathcal { C } _ { \ell } are 690 , 960 , and 1000 \mu K _ { CMB } ^ { 2 } .
When we instead employ the analytic spectrum suggested by Komatsu and Seljak ( 31 ) , and account for the non-Gaussianity of the SZE anisotropy signal , we obtain upper limits on the average amplitude of their spectrum weighted by our transfer function of 790 , 1060 , and 1080 \mu K _ { CMB } ^ { 2 } .
We obtain a 90 % CL upper limit on \sigma _ { 8 } , which normalizes the power spectrum of density fluctuations , of 1.57 .
These are the first constraints on anisotropy and \sigma _ { 8 } from survey data at these angular scales at frequencies near 150 GHz .