Context : Direct imaging has developed into a very successful technique for the detection of exoplanets in wide orbits , especially around young stars .
Directly imaged planets can be both followed astrometrically on their orbits and observed spectroscopically and thus provide an essential tool for our understanding of the early solar system .

Aims : We surveyed the 25 Ori association for direct-imaging companions .
This association has an age of only few million years .
Among other targets , we observed CVSO 30 , which has recently been identified as the first T Tauri star found to host a transiting planet candidate .

Methods : We report on photometric and spectroscopic high-contrast observations with the Very Large Telescope , the Keck telescopes , and the Calar Alto observatory .
They reveal a directly imaged planet candidate close to the young M3 star CVSO 30 .

Results : The JHK-band photometry of the newly identified candidate is at better than 1 \sigma consistent with late-type giants , early-T and early-M dwarfs , and free-floating planets .
Other hypotheses such as galaxies can be excluded at more than 3.5 \sigma .
A lucky imaging z ^ { \prime } photometric detection limit z ^ { \prime } = 20.5 mag excludes early-M dwarfs and results in less than 10 M _ { \mathrm { Jup } } for CVSO 30 c if bound .
We present spectroscopic observations of the wide companion that imply that the only remaining explanation for the object is that it is the first very young ( < 10 Myr ) L – T-type planet bound to a star , meaning that it appears bluer than expected as a result of a decreasing cloud opacity at low effective temperatures .
Only a planetary spectral model is consistent with the spectroscopy , and we deduce a best-fit mass of 4 - 5 Jupiter masses ( total range 0.6 – 10.2 Jupiter masses ) .

Conclusions : This means that CVSO 30 is the first system in which both a close-in and a wide planet candidate are found to have a common host star .
The orbits of the two possible planets could not be more different : they have orbital periods of 10.76 hours and about 27000 years .
The two orbits may have formed during a mutual catastrophic event of planet-planet scattering .