Polarization and limb darkening of plane-parallel atmospheres of solar composition for 20 wavelengths between 2800A and 8000A. These results were extracted from MARCS model atmospheres with solar abundances and 1 km/sec microturbulence. The file name is based on the temperature and log gravity: T3500g3.5 is a model with Teff=3500K, log(g)=3.5. There is also a solar model, indicated by T5777g4.44. There are 65 rows in each file. The first row is the effective temperature, log of the gavity, and metal abundance relative to solar of the model. (We present models with Z=1, 1/10 & 1/100.) The second row gives the values of the 20 continuum wavelengths. The third row gives the emergent (astrophysical) flux F_nu at these 20 wavelengths. The fourth row gives the 159 values of \mu (= cos \theta) at which I(\mu) and Q(\mu) are tabulated, while the fifth row is the corresponding angle \theta in degrees. The remaining 60 rows are 20 groups of three: (1) the emergent intensity I(\mu), (2) the Stokes paramenter Q(\mu), and (3) the polarization Q(\mu)/I(\mu). Each row contains 159 values. The first 3 rows are for the 1st wavelength, 8000A, the next 3 for 7500A, and so on until the last 3 rows for 2800A. The polarization is highest for \mu near zero,i.e., for radiation emerging nearly parallel to the surface of the stellar atmosphere, varies rapidly as \mu goes to zero, so I have spaced the values of \mu more closely there. Note that the Stokes vector Q is measured with respect to the vertical, so radiation near the limb (\mu small) is generally negative, as the light is polarized parallel to the surface of the atmosphere. ------------------------------------------------------------------- Note added 8 May 2019: It has come to my attention that the numbers in these files followed the convention of the "J" language of using the underscore,"_", for the minus sign,"-". I have now changed this by applying the vi command :%s/_/-/g to these files.