2837 20160706140436.0 ASTROimport-994 Stancil, P. C. 2011 Molecules are primarily destroyed in diffuse and translucent regions, in protoplanetary disks, in cool stellar atmospheres, in photodissociation regions, and in x-ray dominated regions via photodissociation (PD) due to the incident radiation field. The majority of astrochemical/spectral modeling codes available today use pre-computed exponentially-attenuated photorates based on dust scattering/absorption for an ``average" interstellar cloud. Since there is clearly a large scatter in the dust properties and local radiation field for various environments in the Galaxy and beyond, the adoption of such pre-computed photorates can lead to considerable errors in predicted abundances. To improve current modeling capabilities, we are computing new rovibrationally-resolved PD cross sections for H_2, HD, HeH+, NH, C_2, CN, and CS and implementing the cross sections in the spectral simulation code Cloudy for explicit computation of local photorates. We present model results using the new photodissociation cross sections for a variety of environments emphasizing differences in total and state-specific molecular column densities. This work was partially supported by NASA grants NNG06GJ11G and HST-AR-11776.01-A, NSF grant AST-0607733, and the PRODEX Programme of ESA. Accurate Photodissociation in UV and X-ray Irradiated Molecular Gas Gay, C. D. Cieszewski, R. M. el-Qadi, W. Kuri, A. Miyake, S. Abel, N. Porter, R. L. Shaw, G. Ferland, G. J. van Hoof, P. A. M. 134.03 Bulletin of the American Astronomical Society 43 2011 http://esoads.eso.org/abs/2011AAS...21813403S published in NONREF