  Space-based photometric surveys have discovered large numbers of planets
transiting other stars, but these observe in a single band-pass and yield only
the planet radius, orbital period, and transit duration. Information on the
masses, compositions, and any atmospheres of these planets requires additional
observations from the ground or space. The Transiting Exoplanet Survey
Satellite (TESS) will yield thousands of planets around bright stars suitable
for such follow-up. In the absence of spectroscopy or spectrophotometry from
space, observations through the different pass-bands of multiple space
telescopes provide some spectral information useful for identifying false
positive signals, distinguishing between reflected light and thermal emission
from hot Jupiters, and detecting Rayleigh scattering by planetary atmospheres.
We calculated the expected difference in transit depths measured by the TESS
and Characterizing Exoplanets Satellites (CHEOPS) missions, which will be more
sensitive to redder and bluer optical wavelengths, respectively. The difference
due to companion or background stars is small (<3% for main sequence
companions) and likely to be negligible and undetectable. For only a few "hot"
Jupiters, can combined photometry disambiguate between the reflected and
thermal signals from planets. However, Rayleigh scattering by hazy atmospheres
with particles sizes near 0.04 $\mu$m and at pressure altitudes above ~1 mbar
can be detected for ~100 transiting planets, assuming every planet has such an
atmosphere. Hazes with this characteristic particle size do not obscure
observations at longer (near-infrared) wavelengths; CHEOPS follow-up of
TESS-detected planets could thus identify candidates suitable for further study
with the James Webb Space Telescope.
