Double pass photoelectric observations are presented of five Can lines (H, K, 8498 ~, 8542/~, and 8662 ~) in a number of solar plages of different degrees of activity, quiet regions, and a sunspot. The data are compared with previous work. All five lines show increasing emission together in plages and the least opaque of the infrared triplet lines appears to exhibit core emission prior to the more opaque members of the multiplet. The question of source function equality is considered and the differences and similarities among plage profiles and between plage and quiet profiles are shown qualitatively and quantitatively. From the earliest photographic observations of Hale and Deslandres in the 1890's, spectroheliograms taken in the cores of the Call H and K lines have shown large bright regions on the disk called flocculi or plages. These observers noted that plages occur typically near sunspots and that in the plage regions the H and K lines exhibit bright double reversals in the cores. Plages appear in spectroheliograms taken in most strong Fraunhofer lines (cf. Title, 1966) and are usually bright compared to the 'quiet' chromosphere, although exceptions exist such as the 10830 A line of He~ in which plages appear as enhanced absorption (d'Azambuja and d'Azambuja, 1937). Plages are not isolated phenomena in the solar atmosphere, but rather are the chromospheric manifestation of activity which ranges from photospheric faculae below to coronal active regions, coronal streamers, and enhanced solar wind above. Most likely an enhanced magnetic field plays a predominent role in all of these diverse phenomena. The primary aim of our work is to understand what perturbations in such physical properties as temperature, density, and velocity field relative to the distribu- tions of these quantities in the undisturbed chromosphere can account for the range of plage activity. It is possible that the difference between models for plages and those for the average quiet chromosphere may provide important clues as to the differences between quiet and active stellar chromospheres. Several measurements of the CalI resonance lines (H and K at 3968 A and 3933 A) and lowest lying subordinate lines (the infrared triplet at 8498 A, 8542 A and 8662 A)