  HD113337 is a Main-Sequence F6V field star more massive than the Sun, hosting
one (possibly two) radial velocity (RV) giant planet(s) and a cold debris disk
(marked by an infrared excess). We used the VEGA interferometer on the CHARA
array to measure HD113337 angular diameter, and derived its linear radius using
the Gaia parallax. We computed the bolometric flux to derive its effective
temperature and luminosity, and we estimated its mass and age using
evolutionary tracks. We used Herschel images to partially resolve the outer
disk, and high-contrast images of HD113337 with the LBTI to probe the 10-80 au
separation range. Finally, we combined the deduced contrast maps with previous
RV of the star using the MESS2 software to bring upper mass limits on possible
companions at all separations up to 80 au, taking advantage of the constraints
on the age and inclination (brought by the fundamental parameter analysis and
the disk imaging, respectively). We derive a limb-darkened angular diameter of
0.386 $\pm$ 0.009 mas that converts into a linear radius of 1.50 $\pm$ 0.04
solar radius. The fundamental parameter analysis leads to an effective
temperature of 6774 $\pm$ 125 K, and to two possible age solutions: one young
within 14-21 Myr and one old within 0.8-1.7 Gyr. We partially resolve the known
outer debris disk and model its emission. Our best solution corresponds to a
radius of 85 $\pm$ 20 au, an extension of 30 $\pm$ 20 au and an inclination
within 10-30 degrees for the outer disk. The combination of imaging contrast
limits, published RV, and our new age and inclination solutions leads to a
first possible estimation of the true masses of the planetary companions: $\sim
7_{-2}^{+4}$ Jupiter masses for HD113337 b (confirmed companion), and $\sim
16_{-3}^{+10}$ Jupiter masses for HD113337 c (candidate). We also constrain
possible additional companions at larger separations.
