Polarization and limb darkening of plane-parallel atmospheres for 12 wavelengths between 3400A and 6000A. These results were extracted from MARCS model atmospheres with abundances 1/10 solar and 1 km/sec microturbulence. Each file is from one atmosphere: Notation: P35g40 --> T_eff= 3,500K, log g= 4.0, and also P425g45 --> T_eff= 4,250K, log g= 4.5. There are 39 rows in each file, each with 159 numbers. The first row is 159 values of $/mu$. The second row are the corresponding values of $\theta = \acos(\mu)$ in radians, while the third row are the values of $\theta$ in degrees. The polarization is highest for \mu near zero (i.e., radiation emerging nearly parallel to the surface of the stellar atmosphere), and varies rapidly as \mu goes to zero, so I have spaced the values of \mu more closely there. The next 3 rows (4,5,6) are values of I(\mu), Q(\mu) and the polarization p(\mu)= Q(\mu)/I(\mu) for a wavelength of 6000A. The following sets of three rows are I, Q and p for different wavelengths. The 12 wavelengths are: 6000A 5500 5200 5000 4800 4600 4400 4200 4000 3800 3600 3400A Note: The Planck function was normalized to unity at an optical depth ~2/3, so the absolute scale of the Stokes I & Q are arbitrary.