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We present radial velocities for five member stars of the recently discoveredyoung (age= 100-150 Myr) stellar system Price-Whelan 1 (PW 1), that is locatedfar away in the Galactic Halo (D~ 29 kpc, Z~ 15 kpc), and that is probablyassociated to the Leading Arm (LA) of the Magellanic Stream. We measure thesystemic radial velocity of PW 1, V_r=275 +/- 10 km/s, significantly largerthan the velocity of the LA gas in the same direction. We re-discuss the mainproperties and the origin of this system in the light of these newobservations, computing the orbit of the system and comparing its velocity withthat of the HI in its surroundings. We show that the bulk of the gas at thevelocity of the stars is more than 10 deg (5~kpc) away from PW 1 and thevelocity difference between the gas and the stars become larger as gas closerto the stars is considered. We discuss the possibilities that (a) the parentgas cloud was dissolved by the interaction with the Galactic gas, and (b) thatthe parent cloud is the high velocity cloud HVC287.5+22.5+240, lagging behindthe stellar system by ~25 km/s and ~10 deg.

Young stars raining through the Galactic Halo: the nature and orbit of Price-Whelan 1