We have observed the Corona Borealis supercluster with the Millimeter and Infrared Testa Grigia Observatory ( MITO ) , located in the Italian Alps , at 143 , 214 , 272 , and 353 GHz .
We present a description of the measurements , data analysis , and results of the observations together with a comparison with observations performed at 33 GHz with the Very Small Array ( VSA ) interferometer situated at the Teide Observatory ( Tenerife , Spain ) .
Observations have been made in the direction of the supercluster towards a cosmic microwave background ( CMB ) cold spot previously detected in a VSA temperature map .
Observational strategy and data analysis are described in detail , explaining the procedures used to disentangle primary and secondary anisotropies in the resulting maps .
From a first level of data analysis we find evidence in MITO data of primary anisotropy but still with room for the presence of secondary anisotropy , especially when VSA results are included .
With a second level of data analysis using map making and the maximum entropy method we claim a weak detection of a faint signal compatible with a SZ effect characterized at most by a Comptonization parameter y = ( 7.8 ^ { +5.3 } _ { -4.4 } ) \times 10 ^ { -6 } 68 % CL .
The low level of confidence in the presence of a SZ signal invite us to study this sky region with higher sensitivity and angular resolution experiments such as the already-planned upgraded versions of VSA and MITO .