README::: We present here a simulation of a single sunspot in a domain with the dimensions 49.152 × 49.152 × 8.192 Mm^3 with a resolution of 96×96×32 km^3, resulting in a grid size of 512× 512 × 256. Boundary conditions are periodic in the horizontal direction. The bottom boundary is open for convective flows and the magnetic field is vertical. In regions with more than 2.5 kG field strength the bottom boundary is closed to prevent a fast decay of the sunspot on a timescale of hours as a consequence of the rather short convective timescales in an 8Mm deep domain. The top boundary is closed for flows and the magnetic field is matched to a potential field extrapolation. The simulation was started from a thermally relaxed convection run in which we inserted an axisymmetric self-similar magnetic field structure with a total flux of 1.2 × 10^22 Mx. To maintain manageable time steps in the numerical simulation we artificially limited Alfv´en waves to 60 km/s in the region above the sunspot umbra where the ratio of gas pressure to magnetic pressure << 1. Note that the simulated sunspot does not have a penumbra due to a combination of the rather low grid resolution as well as the horizontal periodicity. In proximity of the sunspot converging flows dominate similar to those found around pores (see discussion in Rempel 2011, ApJ 740, 15). The data presented here start from 3 hr after initialization to about 30 hr. The directory "photospheric_data" contains the vertical velocity on the tau=0.01 level together with time averaged intensity and vertical magnetic field. The directory "subsurface_data" contains the subsurface thermal, magnetic and flow structure in form of averages in azimuth and time. For further information see the "Readme" files found in the subdirectories. *** Acknowledgment *** This simulation run is further described and analyzed in Braun et al. 2011, ApJ, 744, 77. Please cite this publication in manuscripts or presentations that result from the use of the data. So that we may acknowledge any use of the data in our own reports and presentations, please send any electronic preprints (or web links) of manuscripts which use the data to rempel@ucar.edu. This may be done after a manuscript is submitted or accepted for publication. For all publications and presentations of results using this data, please add the following acknowledgments: We use data provided by M. Rempel at the National Center for Atmospheric Research (NCAR) and A. Birch at NorthWest Research Associates (NWRA). Support for the production of the data was provided by the NASA Solar Dynamics Observatory (SDO) Science Center program through grant NNH09AK021 awarded to NCAR and contract NNH09CE41C awarded to NWRA. The National Center for Atmospheric Research is sponsored by the National Science Foundation.