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We present optical observations of the peculiar Type Ibn supernova (SN Ibn)OGLE-2012-SN-006, discovered and monitored by the OGLE-IV survey, andspectroscopically followed by PESSTO at late phases. Stringent pre-discoverylimits constrain the explosion epoch with fair precision to JD = 2456203.8 +-4.0. The rise time to the I-band light curve maximum is about two weeks. Theobject reaches the peak absolute magnitude M(I) = -19.65 +- 0.19 on JD =2456218.1 +- 1.8. After maximum, the light curve declines for about 25 dayswith a rate of 4 mag per 100d. The symmetric I-band peak resembles that ofcanonical Type Ib/c supernovae (SNe), whereas SNe Ibn usually exhibitasymmetric and narrower early-time light curves. Since 25 days past maximum,the light curve flattens with a decline rate slower than that of the 56Co to56Fe decay, although at very late phases it steepens to approach that rate. Anearly-time spectrum is dominated by a blue continuum, with only a marginalevidence for the presence of He I lines marking this SN Type. This spectrumshows broad absorptions bluewards than 5000A, likely O II lines, which aresimilar to spectral features observed in super-luminous SNe at early epochs.The object has been spectroscopically monitored by PESSTO from 90 to 180 daysafter peak, and these spectra show the typical features observed in a number ofSN 2006jc-like events, including a blue spectral energy distribution andprominent and narrow (v(FWHM) ~ 1900 km/s) He I emission lines. This suggeststhat the ejecta are interacting with He-rich circumstellar material. Thedetection of broad (10000 km/s) O I and Ca II features likely produced in theSN ejecta (including the [O I] 6300A,6364A doublet in the latest spectra) lendssupport to the interpretation of OGLE-2012-SN-006 as a core-collapse event.

Massive stars exploding in a He-rich circumstellar medium. V. Observations of the slow-evolving SN Ibn OGLE-2012-SN-006