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HIP 67522 b is a 17 Myr old, close-in ($P_{orb} = 6.96$ d), Jupiter-sized ($R= 10\,R_{\oplus}$) transiting planet orbiting a Sun like star in the Sco-Cen OBassociation. We present our measurement of the system's projected orbitalobliquity via two spectroscopic transit observations using the CHIRONspectroscopic facility. We present a global model that accounts for largesurface brightness features typical of such young stars during spectroscopictransit observations. With a value of $|\lambda| = 5.8^{+2.8\,\circ}_{-5.7}$,it is unlikely that this well-aligned system is the result of a higheccentricity driven migration history. By being the youngest planet with aknown obliquity, HIP 67522 b holds a special place in contributing to ourunderstanding of giant planet formation and evolution. Our analysis shows thefeasibility of such measurements for young and very active stars.

The obliquity of HIP 67522 b: a 17 Myr old transiting hot Jupiter-sized planet