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tokens: abundances in Paper III ( Rab et al. 2015 ). We intend to offer our modelling tools and collected data sets to the community at the end of the FP7 DIANA project 12 . Appendix A: Stellar parameters and irradiation Appendix A.1: Stellar parameters The photospheric component of the stellar emission is characterised by the effective temperature , the surface gravity , and the stellar (photospheric) luminosity . Since these properties are fairly well-known for most of our target objects in the literature, we have decided not to put too much efforts into this issue. Assuming solar abundances for the star, we use standardPHOENIX stellar atmosphere models ( Brott Hauschildt 2005 ) to fit , and the interstellar extinction , to our photometric and spectroscopic data (see Fig. A.1 ). A thorough determination of requires to fit high-resolution optical spectra. For most target objects, this has been done already in the literature, so we can pick from the literature and only fit and for the assumed distance , using at first an estimate of the surface gravity . Once and are determined, we involve pre-main sequence stellar evolutionary models ( Siess et al. 2000 ) to find the stellar mass and the age. The stellar radius and surface gravity are then given by and . We use the resulting value for to redo the fitting above. This procedure is found to converge very quickly, and – thanks to having fixed from the literature – gives quite unambiguous results, see examples in Table A.1 . Fig. A.1 Fitting stellar parameters, and compilation of the stellar irradiation for two examples, TW Hya ( left ) and AB Aur ( right ). The upper plots show measured photometric fluxes (coloured symbols) as function of wavelength , in comparison to our best fitting, reddened Phoenix stellar atmosphere model spectrum (black), and the averaged observed FUV data (orange). The lower plots show the de-reddened surface intensities (black), and the averaged, de-reddened FUV data ( nm, red). The blue lines show fits to de-absorbed X-ray data, using a two-component X-ray gas emission model (energy keV). The dashed grey line marks the EUV regime in between, which is assumed to be absorbed by neutral hydrogen between the star and the disk and hence disregarded in the disk model. The dashed magenta lines show quick parametric fits to the UV and X-ray data, see Eqs. ( A.1 ) and ( A.2 ) and text, not used for the TW Hya and AB Aur models. Appendix A.2: Stellar UV irradiation The UV irradiation by the central star is much more difficult to determine, and hampered by the lack of high-quality UV data, especially in the hard FUV region (130 nm), and for Ly. We have systematically scanned and collected UV data from IUE, FUSE, HST/STIS, HST/COS, and HST/ACS. These data have been re-binned and collated, using the inverse square of the flux uncertainties as weighting factors, following the idea used by Valenti et al. (2000 , 2003) . The results of this data collection will be described elsewhere