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HD 135344B is an accreting (pre-) transition disk that displays the emissionof warm CO extending tens of AU inside its 30 AU dust cavity. We used the dustradiative transfer code MCFOST and the thermochemical code ProDiMo to derivethe disk structure from the simultaneous modeling of the spectral energydistribution (SED), VLT/CRIRES CO P(10) 4.75 micron, Herschel/PACS [O I] 63micron, Spitzer-IRS, and JCMT 12CO J=3-2 spectra, VLTI/PIONIER H-bandvisibilities, and constraints from (sub-)mm continuum interferometry andnear-IR imaging. We found a disk model able to describe the currentobservations simultaneously. This disk has the following structure. (1) Toreproduce the SED, the near-IR interferometry data, and the CO ro-vibrationalemission, refractory grains (we suggest carbon) are present inside the silicatesublimation radius (0.08<R<0.2 AU). (2) The dust cavity (R<30 AU) is filledwith gas, the surface density of this gas must increase with radius to fit theCO P(10) line profile, a small gap of a few AU in the gas is compatible withcurrent data, and a large gap in the gas is not likely. (4) The gas/dust ratioinside the cavity is > 100 to account for the 870 micron continuum upper limitand the CO P(10) line flux. (5) The gas/dust ratio at 30<R<200 AU is < 10 tosimultaneously describe the [O I] 63 micron line flux and the CO P(10) lineprofile. (6) In the outer disk, most of the mass should be located in themidplane, and a significant fraction of the dust is in large grains.Conclusions: Simultaneous modeling of the gas and dust is required to break themodel degeneracies and constrain the disk structure. An increasing gas surfacedensity with radius in the inner dust cavity echoes the effect of a migratingJovian planet. The low gas mass (a few MJupiter) in the HD 135344B's disksuggests that it is an evolved disk that has already lost a large portion ofits mass.

Constraining the structure of the transition disk HD 135344B (SAO 206462) by simultaneous modeling of multiwavelength gas and dust observations