We present a new method for probing the physical conditions and metal enrichment of the intergalactic medium: the composite spectrum of Lyα forest absorbers. We apply this technique to a sample of 9480 Lyα absorbers with redshift 2 < z < 3.5 identified in the spectra of 13,279 high-redshift quasars from the Sloan Digital Sky Survey (SDSS) Fifth Data Release (DR5). Absorbers are selected as local minima in the spectra with 2.4 < τLyα < 4.0; at SDSS resolution (≈150 km s−1 FWHM), these absorbers are blends of systems that are individually weaker. In the stacked spectra, we detect seven Lyman series lines and metal lines of O vi, N v, C iv, C iii, Si iv, C ii, Al ii, Si ii, Fe ii, Mg ii, and O i. Many of these lines have peak optical depths of <0.02, but they are nonetheless detected at high statistical significance. Modeling the Lyman series measurements implies that our selected systems have total H i column densities . Assuming typical physical conditions , T = 104–104.5 K, and [Fe/H]=−2 yields reasonable agreement with the line strengths of high-ionization species, but it underpredicts the low-ionization species by two orders of magnitude or more. This discrepancy suggests that the low-ionization lines arise in dense, cool, metal-rich clumps, present in some absorption systems.