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We present the results based on photometric ($Swift$ UVOT), broad-bandpolarimetric ($V$ and $R$-band) and optical spectroscopic observations of theType IIn supernova (SN) 2017hcc. Our study is supplemented withspectropolarimetric data available in literature for this event. The post-peaklight curve evolution is slow ($\sim$0.2 mag 100 d$^{-1}$ in $b$-band). Thespectrum of $\sim$+27 d shows a blue continuum with narrow emission lines,typical of a Type IIn SN. Archival polarization data along with the $Gaia$ DR2distances have been utilized to evaluate the interstellar polarization (ISP)towards the SN direction which is found to be $P_{ISP}$ = 0.17 $\pm$ 0.02 percent and $\theta_{ISP}$ = 140$^{\circ}$ $\pm$ 3$^{\circ}$. To extract theintrinsic polarization of SN 2017hcc, both the observed and the literaturepolarization measurements were corrected for ISP. We noticed a significantdecline of $\sim$3.5 per cent ($V$-band) in the intrinsic level of polarizationspanning a period of $\sim$2 months. In contrast, the intrinsic polarizationangles remain nearly constant at all epochs. Our study indicates a substantialvariation in the degree of asymmetry in either the ejecta and/or thesurrounding medium of SN 2017hcc. We also estimate a mass-loss rate of $\dot M$= 0.12 M$_{\odot}$ yr$^{-1}$ (for $v_w$ = 20 km s$^{-1}$) which suggests thatthe progenitor of SN 2017hcc is most likely a Luminous Blue Variable.

On the observational behaviour of the highly polarized Type IIn supernova SN 2017hcc