  The subdwarf B star PG1605+072, with an unusually low log g ~ 5.3, shows a
high number of non-radial pulsation modes, making it a promising candidate for
asteroseismology. This could allow probing the star's interior to gain
important insights in its structure and evolution. Comparison of previous work
conducted over the last decade shows clear amplitude variation and hints of
frequency variation. We analyse white light photometric data of the Multi-Site
Spectroscopic Telescope (MSST) and Whole Earth Telescope (WET) XCov22 campaigns
using prewhitening techniques and O-C diagrams. A total of 85 significant
frequencies are identified, among them more than 20 frequency sums and
harmonics. Moreover, it is shown that the main mode's amplitude varies like a
sine with a period of ~630 d, indicative of long-term beating. Strong hints for
the existence of frequency multiplets support the hypothesis that PG1605+072 is
a slow rotator with V_eq < 0.9 km/s, contrary to previous claims. Existing
asteroseismic models mainly suggest that the star possesses a high mass of ~0.7
M_Sun, presuming the main pulsation mode to be radial. This calls for an
alternate formation channel.
