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Optical, near-infrared (NIR) photometric and spectroscopic studies, alongwith the optical imaging polarimetric results for SN 2012au, are presented inthis article to constrain the nature of the progenitor and other properties.Well-calibrated multiband optical photometric data (from $-$0.2 to +413 d since$B$-band maximum) were used to compute the bolometric light curve and toperform semi-analytical light-curve modelling using the $\texttt{MINIM}$ code.A spin-down millisecond magnetar-powered model explains the observedphotometric evolution of SN 2012au reasonably. Early-time imaging polarimetricfollow-up observations ($-$2 to +31 d) and comparison with other similar casesindicate signatures of asphericity in the ejecta. Good spectral coverage of SN2012au (from $-$5 to +391 d) allows us to trace the evolution of layers of SNejecta in detail. SN 2012au exhibits higher line velocities in comparison withother SNe Ib. Late nebular phase spectra of SN 2012au indicate a Wolf$-$Rayetstar as the possible progenitor for SN 2012au, with oxygen, He-core, andmain-sequence masses of $\sim$1.62 $\pm$ 0.15 M$_\odot$, $\sim$4$-$8 M$_\odot$,and $\sim$17$-$25 M$_\odot$, respectively. There is a clear absence of a firstovertone of carbon monoxide (CO) features up to +319 d in the $K$-band regionof the NIR spectra. Overall analysis suggests that SN 2012au is one of the mostluminous slow-decaying Type Ib SNe, having comparatively higher ejecta mass($\sim$4.7$-$8.3 M$_\odot$) and kinetic energy ($\sim$[4.8 $-$ 5.4] $\times$10$^{51}$ erg). Detailed modelling using $\texttt{MESA}$ and the resultsobtained through $\texttt{STELLA}$ and $\texttt{SNEC}$ explosions also stronglysupport spin-down of a magnetar with mass of around 20 M$_\odot$ andmetallicity Z = 0.04 as a possible powering source of SN 2012au.

Photometric, polarimetric, and spectroscopic studies of the luminous, slow-decaying Type Ib SN 2012au