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We have serendipitously detected a strong O VI-bearing Lyman limit system atz_abs = 0.3558 toward the QSO J1009+0713 (z_em = 0.456) in our survey oflow-redshift galaxy halos with the Hubble Space Telescope's Cosmic OriginsSpectrograph. Its rest-frame equivalent width of W_r = 835 +/- 49 mA is thehighest for an intervening absorber yet detected in any low-redshift QSOsightline, with absorption spanning 400 km s^-1 in its rest frame. HST/WFC3images of the galaxy field show that the absorber is associated with twogalaxies lying at 14 and 46 kpc from the QSO line of sight. The bulk of theabsorbing gas traced by H I resides in two strong, blended component groupsthat possess a total logN(HI) = 18 - 18.8. The ion ratios and column densitiesof C, N, O, Mg, Si, S, and Fe, except the O VI, can be accommodated into asimple photoionization model in which diffuse, low-metallicity halo gas isexposed to a photoionizing field from stars in the nearby galaxies thatpropagates into the halo at 10% efficiency. We constrain the metallicity firmlywithin the range 0.1 - 1 Zsun, and photoionization modeling indirectlyindicates a subsolar metallicity of 0.05 - 0.5 Zsun. The appearance of strong OVI and nine Mg II components and our review of similar systems in theliterature support the "interface" picture of high-velocity O VI: the totalstrength of the O VI shows a positive correlation with the number of detectedcomponents in the low-ionization gas, however the total O VI column densitiesstill far exceed the values expected from interface models for the number ofdetected clouds.

Multiphase Gas In Galaxy Halos: The OVI Lyman-limit System toward J1009+0713