Recent observations of the 21 cm emission line of hydrogen ( Blaauw 1962) have revealed the existence of massive interstellar cloud complexes at considerable distances from the galactic plane. The region 126° < ln < 142°, -19° < bn < -7°, near the association I Persei, in particular, shows a high level of emission at velocities of -48 km/sec (feature "1") and -26 km/sec (feature "2"). The nature and origin of these complexes is not understood at present, and additional evidence regarding the clouds appears highly desirable. In principle, the observation of interstellar absorption lines in the spectra of stars located in the general direction of the cloud complexes can provide limits to their distances from the sun. With this purpose in mind, a number of early-type stars, chosen from a list compiled by H. van Woerden, have been observed with the coude spectrograph of the 200-inch reflector in the region of the Can lines, under dispersions of 4.5 Â/mm (Pb plates), and/or 9.2 Â/mm (Pc plates), depending on the apparent brightness. The results of the observations are summarized in Table I, where the stars are identified by their catalog numbers and galactic coordinates. Those apparent magnitudes, m, given to two decimal places are photoelectric, and the others are photographic from the AGK2. The heliocentric radial velocities, V, of the various components of the interstellar Ca ii lines are given in the sixth column with those corresponding to barely detectable components in parentheses. The correction, AV, for standard solar motion is given in the next column. Equivalent widths have been measured for a few stars and are given in order of increasing velocity in the last column. For other stars only eye estimates of the intensities have been made and are given to one significant figure. The appearance of the K line on the Pb plate of HD 15137 and its degree of resolution into compo-