We present three new methods for determining the age of groups of pre-main-sequence stars. The first, creating empirical isochrones allows us to create a robust age ordering, but not to derive actual ages. The second, using the width of the gap in colour-magnitude space between the pre-main-sequence and main-sequence (the radiative convective gap) has promise as a distance and extinction independent measure of age, but is as yet uncalibrated. Finally we discuss tau^2 fitting of the main sequence as the stars approach the terminus of the main sequence.
The Ages of Stars, Proceedings of the International Astronomical Union, IAU Symposium, Volume 258, p. 103-110
