for GQ Lup A and its companion. We detect no significant change in PA. This would be consistent with an orbital plane that is more edge-on than pole-on or with a highly eccentric orbit, as already argued by Janson et al. (2006) based on the data from 1994 until 2004 only.

The maximum motion of the GQ Lup companion of $\sim 2$ to 3 mas/yr or $\sim 2$ km/s in one dimension is significantly smaller than the expected escape velocity from the GQ Lup A system, which is $5 \pm 2$ km/s, as already concluded with previous data in Mugrauer & Neuhäuser (2005). From the measured projected equatorial rotational velocity $v \cdot \sin i = 6.8 \pm 0.4$ km/s, the newly determined rotation period ($8.45 \pm 0.2$ days), and the luminosity and temperature of GQ Lup A, Broeg et al. (2007) estimated the inclination of the star (GQ Lup A) to be $27 \pm 5^{\circ}$ degrees, which is more pole-on than edge-on. Unless the orbit of the companion is highly eccentric, this may indicate that the stellar equator and the companion have different planes. Normally, one would expect a planet to form in or nearly in the equatorial plane of 