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We present a spectrum of the diffuse Galactic light (DGL) between 3700 and10,000 A, obtained by correlating optical sky intensity with far-infrared dustemission. We use nearly 250,000 blank-sky spectra from BOSS/SDSS-III togetherwith IRIS-reprocessed maps from the IRAS satellite. The larger sample sizecompared to SDSS-II results in a factor-of-two increase in signal to noise. Wecombine these data sets with a model for the optical/far-infrared correlationthat accounts for self-absorption by dust. The spectral features of the DGLagree remarkably well with features present in stellar spectra. There isevidence for a difference in the DGL continuum between the regions covered byBOSS in the northern and southern Galactic hemisphere. We interpret thedifference at red wavelengths as the result of a difference in stellarpopulations, with mainly old stars in both regions but a higher fraction ofyoung stars in the south. There is also a broad excess in the southern DGLspectrum over the prediction of a simple radiative transfer model, without aclear counterpart in the north. We interpret this excess, centered at ~6500 A,as evidence for luminescence in the form of extended red emission (ERE). Theobserved strength of the 4000 A break indicates that at most ~7% of thedust-correlated light at 4000 A can be due to blue luminescence. Our DGLspectrum provides constraints on dust scattering and luminescence independentof measurements of extinction.

An Optical Spectrum of the Diffuse Galactic Light from BOSS and IRIS