We present spectropolarimetric observations of the peculiar Type Ib/c SN 2005bf, in MCG+00-27-005, from 3600-8550AA. The SN was observed on 2005 April 30.9, 18 days after the first B-band light-curve maximum and 6 days before the second B-band light-curve maximum. The degree of the Interstellar Polarization, determined from depolarized emission lines in the spectrum, is found to be large with $p_{max}(ISP)=1.6%$ and $theta(ISP)=149$fdg$7pm4.0$, but this may be an upper limit on the real value of the ISP. After ISP subtraction, significant polarization is observed over large wavelength regions, indicating a significant degree of global asymmetry, $gtrsim 10%$. Polarizations of 3.5% and 4% are observed for absorption components of Ca II H&K and IR triplet, and 1.3% for He I 5876AA and Fe II. On the $Q-U$ plane clear velocity-dependent loop structure is observed for the He I 5876AA line, suggestive of departures from an axial symmetry and possible clumping of the SN ejecta. Weak High Velocity components of $mathrm{Halpha}$, $mathrm{Hbeta}$ and $mathrm{Hgamma}$ are observed, with velocities of -15 000kms. The low degree of polarization observed at H$beta$ suggests that the polarization observed for the other Balmer lines ($sim 0.4%$ above the background polarization) may rather be due to blending of $mathrm{Halpha}$ and $mathrm{Hgamma}$ with polarized Si II and Fe II lines, respectively. We suggest a model in which a jet of material, that is rich in $mathrm{^{56}Ni}$, has penetrated the C-O core, but not the He mantle. The jet axis is tilted with respect to the axis of the photosphere. This accounts for the lack of significant polarization of O I 7774AA, the delayed excitation and, hence, observability of He I and, potentially, the varied geometries of He and Ca.
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