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Massive stars exploding in a He-rich circumstellar medium. V. Observations of the slow-evolving SN Ibn OGLE-2012-SN-006 | | A. Pastorello
; L. Wyrzykowski
; S. Valenti
; J. L. Prieto
; S. Kozlowski
; A. Udalski
; N. Elias-Rosa
; A. Morales-Garoffolo
; J. P. Anderson
; S. Benetti
; M. Bersten
; M. T. Botticella
; E. Cappellaro
; G. Fasano
; M. Fraser
; A. Gal-Yam
; M. Gillone
; M. L. Graham
; J. Greiner
; S. Hachinger
; D. A. Howell
; C. Inserra
; J. Parrent
; A. Rau
; S. Schulze
; S. J. Smartt
; K. W. Smith
; M. Turatto
; O. Yaron
; D. R. Young
; M. Kubiak
; M. K. Szymanski
; G. Pietrzynski
; I. Soszynski
; K. Ulaczyk
; R. Poleski
; P. Pietrukowicz
; J. Skowron
; P. Mroz
; | | Date: |
17 Feb 2015 | | Abstract: | We present optical observations of the peculiar Type Ibn supernova (SN Ibn)
OGLE-2012-SN-006, discovered and monitored by the OGLE-IV survey, and
spectroscopically followed by PESSTO at late phases. Stringent pre-discovery
limits 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. The
object 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 days
with a rate of 4 mag per 100d. The symmetric I-band peak resembles that of
canonical Type Ib/c supernovae (SNe), whereas SNe Ibn usually exhibit
asymmetric 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 to
56Fe decay, although at very late phases it steepens to approach that rate. An
early-time spectrum is dominated by a blue continuum, with only a marginal
evidence for the presence of He I lines marking this SN Type. This spectrum
shows broad absorptions bluewards than 5000A, likely O II lines, which are
similar to spectral features observed in super-luminous SNe at early epochs.
The object has been spectroscopically monitored by PESSTO from 90 to 180 days
after peak, and these spectra show the typical features observed in a number of
SN 2006jc-like events, including a blue spectral energy distribution and
prominent and narrow (v(FWHM) ~ 1900 km/s) He I emission lines. This suggests
that the ejecta are interacting with He-rich circumstellar material. The
detection of broad (10000 km/s) O I and Ca II features likely produced in the
SN ejecta (including the [O I] 6300A,6364A doublet in the latest spectra) lends
support to the interpretation of OGLE-2012-SN-006 as a core-collapse event. | | Source: | arXiv, 1502.4945 | | Services: | Forum | Review | PDF | Favorites | |
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