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We present the obliquity of the warm Neptune HD 106315c measured via a seriesof spectroscopic transit observations. HD 106315c is a 4.4 REarth warm Neptuneorbiting a moderately rotating late F-star with a period of 21.05 days. HD106315 also hosts a 2.5 REarth super-Earth on a 9.55 day orbit. Our Dopplertomographic analyses of four transits observed by the Magellan/MIKE, HARPS, andTRES facilities find HD 106315c to be in a low stellar obliquity orbit,consistent with being well aligned with the spin axis of the host star atlambda = -10 +3.6/-3.8 deg. We suggest, via dynamical N-body simulations, thatthe two planets in the system must be co-planar, and thus are both well alignedwith the host star. HD 106315 is only the fourth warm Neptune system withobliquities measured. All warm Neptune systems have been found in well alignedgeometries, consistent with the interpretation that these systems are formedin-situ in the inner protoplanetary disk, and also consistent with the majorityof Kepler multi-planet systems that are in low obliquity orbits. With a transitdepth of 1.02 mmag, HD 106315c is among the smallest planets to have beendetected in transit spectroscopy, and we discuss its detection in the contextof TESS and the next generations of spectrographs.

The warm Neptunes around HD 106315 have low stellar obliquities