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We use 189 new radial velocities, an $R$ band CCD mosiac, archival X-rayimages, and gas temperatures to study substructure, masses, luminosityfunctions, and mass-to-light ratios in A2626 and A2440. The symmetric X-rayemission from A2626 suggests a relaxed, single-component system; however, 159redshifts reveals a complex, three component cluster at cz~17,500km/s. Onecomponents is a typical X-ray bright cluster, a second has a cluster-likegalaxy population with lower central galaxy and gas density, and the third is abackground structure with field galaxy composition. A comparison of themagnitude distributions within the two subclusters suggests that A2626 is amerger in progress. Virial masses and a composite luminosity function for aregion with projected radius r=1.5h^{-1}Mpc yield a mass to light ratioM/L_R~610h. Analysis of the X-ray emission from the primary component yields agas mass fraction of 2.2h^{-3/2}% and a baryon fraction of 3.4%. A radialinfall model implies that the virial mass may be an underestimate. In A2440,deep CCD $R$ band photometry indicates a striking correspondence between thegalaxy and gas distributions. The galaxy distribution has three maincomponents, each associated with a giant elliptical galaxy. The two largerpeaks in the galaxy distribution coincide with the primary peaks in the X-rayemission, and the third is associated with a significant X-ray surfacebrightness enhancement. We use this galaxy-gas correspondence and 48 redshiftsto argue that the subclusters are bound within a single system, and that thetwo primary components are beginning to merge. The composite luminosityfunction and estimates of the subcluster virial masses indicate a mass-to-lightratio from 660h to 880h.Comment: 22 pages, to appear in the Astronomical Journal, Nov 9

A Dynamical Analysis of the Poor Galaxy Clusters Abell 2626 and Abell 2440