to the tSZ effect before the 2009 observing season. This refurbishment added science-quality 95GHz detectors and removed half of the 220GHz detectors. As a result, the 2009-2011 data are comparatively shallower at 220GHz, but much deeper at 95GHz. The remaining two fields (200), first observed in 2008, were reobserved in 2010 and 2011 to acquire higher quality 95GHz data. Thus these two fields have $\sim$$\sqrt{2}$ lower noise at 150GHz. The approximate statistical weight of data from each year \[2008, 2009, 2010, 2011\] is \[0, 0.18, 0.42, 0.40\] at 95GHz, \[0.08, 0.19, 0.40, 0.33\] at 150GHz, and \[0.20, 0.17, 0.39, 0.25\] at 220GHz. Details of the time-ordered data (TOD), filtering, and map-making can be found in S11.

Beams and calibration {#sec:beamcal}
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The SPT beams are measured using a combination of bright point sources in each field, Venus, and Jupiter as described in S11. The main lobes of the SPT beam at 95, 150, and 220$\,$GHz are well-represented by 1.7$^\prime$, 1.2$^\prime$, and 1.0$^\prime$ FWHM Gaussians.

The observation-to-observation relative calibrations of the TOD are determined from measurements of a galactic H[II]{} region, RCW38, repeated several times per day. The absolute calibration at each frequency is determined by comparing the [[*Planck*]{}]{} combined CMB 