  The Karin family is a very young asteroid family created by an asteroid
breakup 5.8 Myr ago. Since the members of this family probably have not
experienced significant orbital or collisional evolution yet, it is possible
that they still preserve properties of the original family-forming event in
terms of their spin state. As we carried out a series of photometric
observations of the Karin family asteroids, here we report an analysis result
of lightcurves including the rotation period of eleven members. The mean
rotation rate of the Karin family members turned out to be much lower than
those of NEAs or smaller MBAs (diameter D<12 km), and even lower than that of
larger MBAs (D>130 km). We investigated a correlation between the peak-to-peak
variation magnitude reduced to zero solar phase angle and the rotation period
of the eleven Karin family asteroids, and found a possible trend that elongated
members have lower spin rate, and less elongated members have higher spin rate.
However, this has to be confirmed by another series of future observations.
