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The Q/U Imaging ExperimenT (QUIET) employs coherent receivers at 43GHz and95GHz, operating on the Chajnantor plateau in the Atacama Desert in Chile, tomeasure the anisotropy in the polarization of the CMB. QUIET primarily targetsthe B modes from primordial gravitational waves. The combination of thesefrequencies gives sensitivity to foreground contributions from diffuse Galacticsynchrotron radiation. Between 2008 October and 2010 December, >10,000hours ofdata were collected, first with the 19-element 43GHz array (3458hours) and thenwith the 90-element 95GHz array. Each array observes the same four fields,selected for low foregrounds, together covering ~1000deg^2. This paper reportsinitial results from the 43GHz receiver which has an array sensitivity to CMBfluctuations of 69uK sqrt(s). The data were extensively studied with a largesuite of null tests before the power spectra, determined with two independentpipelines, were examined. Analysis choices, including data selection, weremodified until the null tests passed. Cross correlating maps with differenttelescope pointings is used to eliminate a bias. This paper reports the EE, BBand EB power spectra in the multipole range ell=25-475. With the exception ofthe lowest multipole bin for one of the fields, where a polarized foreground,consistent with Galactic synchrotron radiation, is detected with 3sigmasignificance, the E-mode spectrum is consistent with the LCDM model, confirmingthe only previous detection of the first acoustic peak. The B-mode spectrum isconsistent with zero, leading to a measurement of the tensor-to-scalar ratio ofr=0.35+1.06-0.87. The combination of a new time-stream double-demodulationtechnique, Mizuguchi-Dragone optics, natural sky rotation, and frequentboresight rotation leads to the lowest level of systematic contamination in theB-mode power so far reported, below the level of r=0.1

First Season QUIET Observations: Measurements of CMB Polarization Power Spectra at 43 GHz in the Multipole Range 25 <= ell <= 475