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We present an extensive ($\sim$ 1200 d) photometric and spectroscopicmonitoring of the Type IIn supernova (SN) 2012ab. After a rapid initial riseleading to a bright maximum (M$_{R}$ = $-$19.39 mag), the light curves show aplateau lasting about 2 months followed by a steep decline up to about 100 d.Only in the $U$ band the decline is constant in the same interval. At laterphases, the light curves remain flatter than the $^{56}$Co decline suggestingthe increasing contribution of the interaction between SN ejecta withcircumstellar material (CSM). Although heavily contaminated by emission linesof the host galaxy, the early spectral sequence (until 32 d) shows persistentnarrow emissions, indicative of slow unshocked CSM, and the emergence of broadBalmer lines of hydrogen with P-Cygni profiles over a blue continuum, arisingfrom a fast expanding SN ejecta. From about 2 months to $\sim$1200 d, theP-Cygni profiles are overcome by intermediate width emissions (FWHM $\sim 6000$\kms), produced in the shocked region due to interaction. On the red wing a redbump appears after 76 d, likely a signature of the onset of interaction of thereceding ejecta with the CSM. The presence of fast material both approachingand then receding is suggestive that we are observing the SN along the axis ofa jet-like ejection in a cavity devoid of or uninterrupted by CSM in theinnermost regions.

Photometric and spectroscopic evolution of the peculiar Type IIn SN 2012ab