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We performed the new JVLA full polarization observations at 40-48 GHz(6.3-7.5 mm) towards the nearby ($d$ $=$147$\pm$3.4 pc) Class 0 YSO IRAS16293-2422, and compare with the previous SMA observations reported by Rao etal. (2009; 2014). We observed the quasar J1407+2827 which is weakly polarizedand can be used as a leakage term calibrator for $<$9 GHz observations, togauge the potential residual polarization leakage after calibration. We did notdetect Stokes Q, U, and V intensities from the observations of J1407+2827, andconstrain (3-$\sigma$) the residual polarization leakage after calibration tobe $\lesssim$0.3\%. We detect linear polarization from one of the two binarycomponents of our target source, IRAS\,16293-2422\,B. The derived polarizationposition angles from our observations are in excellent agreement with thosedetected from the previous observations of the SMA, implying that on thespatial scale we are probing ($\sim$50-1000 au), the physical mechanisms forpolarizing the continuum emission do not vary significantly over the wavelengthrange of $\sim$0.88-7.5 mm. We hypothesize that the observed polarizationposition angles trace the magnetic field which converges from large scale to anapproximately face-on rotating accretion flow. In this scenario, magnetic fieldis predominantly poloidal on $>$100 au scales, and becomes toroidal on smallerscales. However, this interpretation remains uncertain due to the high dustoptical depths at the central region of IRAS\,16293-2422\,B and the uncertaintemperature profile. We suggest that dust polarization at wavelengthscomparable or longer than 7\,mm may still trace interstellar magnetic field.Future sensitive observations of dust polarization in the fully optically thinregime will have paramount importance for unambiguously resolving the magneticfield configuration.

Detection of 40-48 GHz dust continuum linear polarization towards the Class 0 young stellar object IRAS 16293-2422