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Dust polarization observations at optical wavelengths help to understand thedust grain properties and trace the plane-of-the-sky component of the magneticfield. In this study, we make use of the $I$-band polarization data acquiredfrom AIMPOL along with the distances ($d$) and extinction ($A_{V}$) data tostudy the variation of polarization fraction ($P$) as a function of $A_{V}$ and$d$ towards the star-forming region, NGC 1893. We employ a broken power-law fitand Bayesian analysis on extinction ($A_{V}$) versus polarization efficiency($P$/$A_{V}$) and distance ($d$) versus rate of polarization ($P$/$d$). We findthat $P$/$A_{V}$ shows a break at an extinction of $\sim$0.9 mag, whereas $P/d$exhibits a break at a distance of $\sim$1.5 kpc. Based on these, we categorizethe dust towards NGC 1893 into two populations: (i) foreground dust confined to$A_{V}$ $<$ $\sim$1 mag and distance up to $\sim$2 kpc and (ii) Perseus spiralarm dust towards NGC 1893 characterized with $A_{V}$ $>$ $\sim$1 mag anddistance beyond $\sim$2 kpc. Foreground dust exhibits higher polarizationefficiency but a lower polarization rate, whereas Perseus dust shows a lowerpolarization efficiency but a slightly higher polarization rate. Hence, wesuggest that while polarization efficiency reveals the dust grain alignment,the rate of polarization infers about the distribution of dust grains towardsNGC 1893. Further, we also shed a light on the spatial variation of intrinsicpolarization and magnetic field orientation, and other parameters within theintra-cluster medium of NGC 1893.

Revealing the dust grain polarization properties as a function of extinction and distance towards NGC 1893