A new emission-line solar coronagraph is described that photographically records coro-nal emission of the Fe XIV (5303 Å) and Fe X (6374 Å) lines, and prominences and the solar disk in Hα (6563 Å). The basic optical system consists of a 20-cm aperture, f/11 aspheric singlet objective and four secondary optical systems--one for each image channel--that are sequentially switched into the beam. Interference filters and a specially-designed Lyot birefringent filter isolate spectral bands ≈ 1 Å at the three wavelengths. The efficiency of this filtering and special constructional features result in an exceptionally small amount of scattered light reaching the film plane. Coronal images can be recorded in skies some 2.5 times brighter than is typical for earlier designs of emission-line corona-graphs. Features of the data obtained so far, including high contrast and high spatial resolution images and the detection of extremely rapid coronal changes, are discussed.