  Open clusters serve as a useful tool for calibrating models of the
relationship between mass, rotation, and age for stars with an outer convection
zone due to the homogeneity of the stars within the cluster. Cluster to cluster
comparisons are essential to determine whether the universality of spin down
relations holds. NGC 6709 is selected as a young open cluster for which no
rotation periods of members have previously been obtained. This cluster is at a
distance of over 1 kpc and has two red giant members. Isochrones place the age
of the cluster at around 150 Myr, or approximately the same age as the
Pleiades. Photometry is obtained over a multi-month observing season at the
robotic observatory STELLA. After basic processing, PSF photometry was derived
using Daophot II, and a suite of related software allowed us to create time
series of relative magnitude changes for each star. Four time series analysis
methods are then applied to these light curves to obtain rotation periods for
members stars. We obtain for the first time rotation periods for 45 FGK cluster
members of NGC 6709. We compare our rotation periods to Gaia EDR3 colors and
find a slow-rotating sequence with increasing rotation periods towards redder
stars and a smaller clump of rapid rotators that have not yet joined this
sequence. NGC 6709 has rotation periods very similar to that of another
Pleiades-age open cluster, NGC 2516.
