We present details of the construction and characterization of the coaddition of the Sloan Digital Sky Survey Stripe 82 ugriz imaging data .
This survey consists of 275 deg ^ { 2 } of repeated scanning by the SDSS camera of 2.5 \arcdeg of \delta over -50 \arcdeg \leq \alpha \leq 60 \arcdeg centered on the Celestial Equator .
Each piece of sky has \sim 20 runs contributing and thus reaches \sim 2 magnitudes fainter than the SDSS single pass data , i.e .
to r \sim 23.5 for galaxies .
We discuss the image processing of the coaddition , the modeling of the PSF , the calibration , and the production of standard SDSS catalogs .
The data have r -band median seeing of 1.1″ , and are calibrated to \leq 1 \% .
Star color-color , number counts , and psf size vs modelled size plots show the modelling of the PSF is good enough for precision 5-band photometry .
Structure in the psf-model vs magnitude plot show minor psf mis-modelling that leads to a region where stars are being mis-classified as galaxies , and this is verified using VVDS spectroscopy .
As this is a wide area deep survey there are a variety of uses for the data , including galactic structure , photometric redshift computation , cluster finding and cross wavelength measurements , weak lensing cluster mass calibrations , and cosmic shear measurements .