The star 55 Cancri was one of the first known exoplanet hosts, and each of the planets in this system is remarkable. Planets b and c are in a near 1:3 resonance. Planet d has a 14.5-year orbit and has one of the longest known orbital periods for a gas giant planet. Planet e has a mass of 8M⊕ and transits this bright star, providing a promising target for modeling the interior structure and atmospheric composition of a Super-Earth. Planet e’s orbital axis is well-aligned with the host star’s spin axis, with an unprojected angle of \( {23}_{-23}^{+14} \) degrees. Planet f resides in the habitable zone of the star. If the planets are approximately coplanar, then by virtue of having one transiting planet, this is a system where the Doppler technique has essentially measured the true mass of the planets, rather than just M sin i. The unfolding history of this system provides a good example of how the challenges in understanding the host star lead to inaccuracies in understanding orbiting planets.