Shock-crossing data obtained from spacecraft are used to test the shock location models derived by Chapman and Cairns  . Three sets of data are considered: (1) ISEE 1 for 24–25 September 1987, (2) Wind, Geotail, IMP 8, and Interball for the intervals 26–27 April and 10–13 May 1999, and (3) IMP 8, Geotail, Magion-4, and Cluster during the period 1973–2003 from the bow shock database (available at http://nssdc.gsfc.nasa.gov/ftphelper/bowshock.html). Derived from MHD simulations, the two shock models are for angles θ IMF = 45° and 90° between the upstream magnetic field B IMF and solar wind velocity v sw . These models have azimuthal asymmetries, and they depend explicitly on the upstream Mach number M A and ram pressure P ram. We also test Cairns et al.'s  rotationally symmetric shock model. The new models perform better on average than the rotationally symmetric model, providing some evidence and support for the shock's shape being strongly dependent upon M A and θ IMF. We also compare our analyses here with model/spacecraft comparisons performed by Merka et al. [2003a] and discuss the importance of filtering on the model predictions.