  Dust polarisation observations at optical wavelengths help understand the
dust grain properties and trace the plane-of-the-sky component of the magnetic
field. In this study, we make use of published optical polarisation data
acquired with AIMPOL along with distances ($d$) and extinction
($A_{\mathrm{V}}$) data. We study the variation of polarisation efficiency
($P/A_{\mathrm{V}}$) as a function of $A_{\mathrm{V}}$ in the diffuse
interstellar medium (ISM) and intracluster mediums (ICM) using the already
published polarisation data of six clusters. Among these clusters, NGC 2281,
NGC 1664, and NGC 1960 are old; while Stock 8, NGC 1931, and NGC 1893 are
young. We categorize stars towards each cluster into foreground, background,
and cluster members by employing two clustering algorithms GMM and DBSCAN.
Thus, classified field stars and cluster members are used to reveal the
polarisation properties of ISM and ICM dust, respectively. We find that the
dust grains located in the diffuse ISM show higher polarisation efficiencies
when compared to those located in the ICM of younger clusters.
