  The GMRT reionization effort aims to map out the large scale structure of the
Universe during the epoch of reionization (EoR). Removal of polarized Galactic
emission is a difficult part of any 21 cm EoR program, and we present new upper
limits to diffuse polarized foregrounds at 150 MHz. We find no high
significance evidence of polarized emission in our observed field at mid
galactic latitude (J2000 08h26m+26). We find an upper limit on the
2-dimensional angular power spectrum of diffuse polarized foregrounds of [l^2
C_l/(2 PI)]^{1/2}< 3K in frequency bins of width 1 MHz at 300<l<1000. The
3-dimensional power spectrum of polarized emission, which is most directly
relevant to EoR observations, is [k^3 P_p(k)/(2 PI^2)]^{1/2}< 2K at k_perp >
0.03 h/Mpc, k < 0.1 h/Mpc. This can be compared to the expected EoR signal in
total intensity of [k^3 P(k)/ (2 PI^2) ]^{1/2} ~ 10 mK. We find polarized
structure is substantially weaker than suggested by extrapolation from higher
frequency observations, so the new low upper limits reported here reduce the
anticipated impact of these foregrounds on EoR experiments. We discuss Faraday
beam and depth depolarization models and compare predictions of these models to
our data. We report on a new technique for polarization calibration using
pulsars, as well as a new technique to remove broadband radio frequency
interference. Our data indicate that, on the edges of the main beam at GMRT,
polarization squint creates ~ 3% leakage of unpolarized power into polarized
maps at zero rotation measure. Ionospheric rotation was largely stable during
these solar minimum night time observations.
