  We report spectroscopy and photometry of the cataclysmic variable stars
ASASSN-14ho and V1062 Cyg. Both are dwarf novae with spectra dominated by their
secondary stars, which we classify as approxomately K4 and M0.5, respectively.
Their orbital periods, determined mostly from the secondary stars' radial
velociites, proved to be nearly identical, respectively 350.14 +- 0.15 and
348.25 +- 0.60 min. The H-alpha emission line in V1062 Cyg displays a
relatively sharp emission component that tracks the secondary's motion, which
may arise on the irradiated face of the secondary; tihs is not often seen and
may indicate an unusually strong flux of ionizing radiation. Both systems
exhibit double-peaked orbital modulation consistent with ellipsoidal variation
from the changing aspect of the secondary. We model these variations to
constrain the orbital inclination i, and estimate approximate component masses
based oni and the secondary velocity amplitude K2.
