  We build the Yunnan-III evolutionary population synthesis (EPS) models by
using the MESA stellar evolution code, BaSeL stellar spectra library and the
initial mass functions (IMFs) of Kroupa and Salpeter, and present colours and
integrated spectral energy distributions (ISEDs) of solar-metallicity stellar
populations (SPs) in the range of 1Myr-15 Gyr. The main characteristic of the
Yunnan-III EPS models is the usage of a set of self-consistent
solar-metallicity stellar evolutionary tracks (the masses of stars are from 0.1
to 100Msun). This set of tracks is obtained by using the state-of-the-art MESA
code.
  MESA code can evolve stellar models through thermally pulsing asymptotic
giant branch (TP-AGB) phase for low- and intermediate-mass stars. By
comparisons, we confirm that the inclusion of TP-AGB stars make the V-K, V-J
and V-R colours of SPs redder and the infrared flux larger at ages
log(t/yr)>7.6 (the differences reach the maximum at log(t/yr)~8.6, ~0.5-0.2mag
for colours, ~2 times for K-band flux).
  The stellar evolutionary tracks, isochrones, colours and ISEDs can be
obtained on request from the first author or from our website
(http://www1.ynao.ac.cn/~zhangfh/). Using the isochrones, you can build your
EPS models. Now the format of stellar evolutionary tracks is the same as that
in the STARBURST99 code, you can put them into the STARBURST99 code and get the
SP's results. Moreover, the colours involving other passbands or on other
systems (for example, HST $F439W-F555W$ colour on AB system) can also be
obtained on request.
