  We use observed optical to near infrared spectral energy distributions (SEDs)
of 266 galaxies in the COSMOS survey to derive the wavelength dependence of the
dust attenuation at high redshift. All of the galaxies have spectroscopic
redshifts in the range z = 2 to 6.5. The presence of the CIV absorption
feature, indicating that the rest-frame UV-optical SED is dominated by OB
stars, is used to select objects for which the intrinsic, unattenuated spectrum
has a well-established shape. Comparison of this intrinsic spectrum with the
observed broadband photometric SED then permits derivation of the wavelength
dependence of the dust attenuation. The derived dust attenuation curve is
similar in overall shape to the Calzetti curve for local starburst galaxies. We
also see the 2175 \AA~bump feature which is present in the Milky Way and LMC
extinction curves but not seen in the Calzetti curve. The bump feature is
commonly attributed to graphite or PAHs. No significant dependence is seen with
redshift between sub-samples at z = 2 - 4 and z = 4 - 6.5. The 'extinction'
curve obtained here provides a firm basis for color and extinction corrections
of high redshift galaxy photometry.
