WTS Results

First planet:
WTS-1b: Inflated hot Jupiter around an F star
http://arxiv.org/abs/1210.1217

Also mentions that WTS-2b is a Jupiter-like planet around a K-star.

More about WTS-2 b (page 9):

http://www.usm.uni-muenchen.de/~tilman/planets2012/talks/uploads/73.pdf

http://www.mpe.mpg.de/events/ropacs-2012/Talks/Birkby.pdf

Zendejas et al. "Searching for transits in the WTS with difference imaging light curves"
http://arxiv.org/abs/1310.1914

One giant planet candidate (19b-1-02162), orbiting a G-star.

The same paper regards WTS-2 b as "confirmed":
 

Quote :

Two objects are common detections in both the DI and AP light curves, of which one candidate is WTS-2b that has recently been confirmed as a planet by the RoPACS community (Birkby et al., 2013a,b)

 
 
I suppose one of those reference to match with this (open access) one.
  
EPE doesn't mention this.

I've gotta have some kind of a magic skill, since as I talk an EPE update appears...  

http://exoplanet.eu/catalog/wts-2_b/

Published at last

WTS-2 b: a hot Jupiter orbiting near its tidal destruction radius around a K-dwarf

Quote :

We report the discovery of WTS-2 b, an unusually close-in 1.02-day hot Jupiter (Mp=1.12MJ, Rp=1.363RJ) orbiting a K2V star, which has a possible gravitationally-bound M-dwarf companion at 0.6 arcsec separation contributing ~20 percent of the total flux in the observed J-band light curve. The planet is only 1.5 times the separation from its host star at which it would be destroyed by Roche lobe overflow, and has a predicted remaining lifetime of just ~40 Myr, assuming a tidal dissipation quality factor of Q'*=10^6. Q'* is a key factor in determining how frictional processes within a host star affect the orbital evolution of its companion giant planets, but it is currently poorly constrained by observations. We calculate that the orbital decay of WTS-2 b would correspond to a shift in its transit arrival time of T_shift~17 seconds after 15 years assuming Q'*=10^6. A shift less than this would place a direct observational constraint on the lower limit of Q'* in this system. We also report a correction to the previously published expected T_shift for WASP-18 b, finding that T_shift=356 seconds after 10 years for Q'*=10^6, which is much larger than the estimated 28 seconds quoted in WASP-18 b discovery paper. We attempted to constrain Q'* via a study of the entire population of known transiting hot Jupiters, but our results were inconclusive, requiring a more detailed treatment of transit survey sensitivities at long periods. We conclude that the most informative and straight-forward constraints on Q'* will be obtained by direct observational measurements of the shift in transit arrival times in individual hot Jupiter systems. We show that this is achievable across the mass spectrum of exoplanet host stars within a decade, and will directly probe the effects of stellar interior structure on tidal dissipation.

WTS-2 is a KIC star O_o KIC 1173581