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This paper reports the first measurement of the relationship betweenturbulent velocity and cloud size in the diffuse circumgalactic medium (CGM) intypical galaxy halos at redshift z~0.4-1. Through spectrally-resolvedabsorption profiles of a suite of ionic transitions paired with carefulionization analyses of individual components, cool clumps of size as small asl_cl~1 pc and density lower than nH = 0.001 cm^-3 are identified in galaxyhalos. In addition, comparing the line widths between different elements forkinematically matched components provides robust empirical constraints on thethermal temperature T and the non-thermal motions bNT, independent of theionization models. On average, bNT is found to increase with l_cl following bNT\propto l_cl^0.3 over three decades in spatial scale from l_cl~1 pc to l_cl~1kpc. Attributing the observed bNT to turbulent motions internal to the clumps,the best-fit bNT-l_cl relation shows that the turbulence is consistent withKolmogorov at <1 kpc with a roughly constant energy transfer rate per unit massof epsilon~0.003 cm^2 s^-3 and a dissipation time scale of <~ 100 Myr. Nosignificant difference is found between massive quiescent and star-forminghalos in the sample on scales less than 1 kpc. While the inferred epsilon iscomparable to what is found in CIV absorbers at high redshift, it isconsiderably smaller than observed in star-forming gas or in extendedline-emitting nebulae around distant quasars. A brief discussion of possiblesources to drive the observed turbulence in the cool CGM is presented.

The Cosmic Ultraviolet Baryon Survey: Empirical Characterization of Turbulence in the Cool Circumgalactic Medium