Shape Dataset Organization This shape-model dataset includes a wide variety of shape models of comet 67P/Churyumov-Gerasimenko. They have been developed by several different groups, using data from several different portions of the Rosetta mission, using a variety of techniques, and intended for a variety of different purposes. Several of these models have been cited in the literature as underlying various investigations. The different shape models are collected together in order to make it easier for users to choose the appropriate model, but the wide variety means that there are many possible ways to organize the archive. At the time this document is written (February 2016), only a few of the anticipated models have been archived (and some models have not yet even been created), but to understand the organization we discuss generically all the models that we hope will be archived. All the shape models tesselate the surface of the nucleus into triangular, flat plates. At the highest level, the datasets are separated into ascii formats and binary formats. The binary formats are exclusively the Digital Shape Kernels that are used in SPICE (routines currently in beta-test version but expected to be in the general release in spring 2016). The ascii versions are designed for non-SPICE users and for simple visualization of the geometry. They always include an ascii version that follows the standard used in PDS-SBN for decades (long prior to the availability of DSK) that includes a wrapper that makes them viewable in any VRML-aware application, of which there are many available. At the next level, the models are divided into groups corresponding to the team that produced the models and the method that team used. The four groups at this level are, as abbreviated in directory names and file names: 1) mspcd_lam, Modified StereoPhotoClinometry by Distortion, produced at the Laboratoire d’Astrophysique de Marseille, 2) spc_esa, StereoPhotoClinometry produced by the flight operations team of ESA (European Space Agency) and converted to standard formats by the Rosetta Mission Operations Center (RMOC), 3) spc_lam_psi, StereoPhotoClinometry produce by a collaboration between the Laboratoire d’Astrophysique de Marseille and the Planetary Science Institute, and 4) spg_dlr, StereoPhotoGranulometry produced at the German Aerospace Center (DLR) group in Berlin. This grouping also separates the models by the instruments used to obtain the input images, the models from ESA having been derived entirely from the NAVCAMs (NAVCAM1 and NAVCAM2 are nominally identical), whereas the other three groups are based entirely on the scientific cameras, OSIRIS-NAC and OSIRIS-WAC. At this writing, there are currently no models available in group 4. See other documents to understand the differences among the techniques. At the third level, the models are sorted by the time period of the data used, which affects the geographic coverage of the data and the best spatial resolution achieved. For the models from ESA, this is denoted by the last MTP (Medium Term Planning) cycle of the data, whereas for the models using the scientific cameras, the OSIRIS teams used sequential numbers to indicate the time period, with detail s given in the relevant subdirectories. At this writing, the ESA models utilize data obtained through MTP09 (through mid-November 2014, i.e., data prior to the release of the Philae Lander). The OSIRIS models currently on hand are all SHAP2, using data only through 3 August 2014. Anticipated future deliveries include an SPG version of SHAP4, SPC and MSPCD versions of SHAP5, and TBD versions of SHAP7 (data being taken as this is written). At the next level, because the full-resolution models are very large, there are models with various levels of reduced resolution available, intended for purposes that do not require the highest resolution and therefore speed up calculations.