Optical photometry and spectroscopy of the Type Ibn supernova SN 2006jc until the onset of dust formation

Anupama, G. C.; Sahu, D. K.; Gurugubelli, U. K.; Prabhu, T. P.; Tominaga, Nozomu; Tanaka, Masayuki; Nomoto, Ken’ichi

doi:10.1111/j.1365-2966.2008.14129.x

Cited by 39 publications

(36 citation statements)

References 33 publications

(88 reference statements)

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“…Given the uncertainties involved in the derivations, it is encouraging to note that these estimates are consistent with the dust masses computed for other SNe IIn (e.g., Gerardy et al 2002;Pozzo et al 2004;Meikle et al 2007;Trundle et al 2009;Andrews et al 2011;Gall et al 2011), and the Type Ibn SN 2006jc (Smith et al 2008b;Di Carlo et al 2008;Nozawa et al 2008;Mattila et al 2008;Anupama et al 2009;Sakon et al 2009). …”

Section: Discussionsupporting

confidence: 63%

MULTI-WAVELENGTH OBSERVATIONS OF THE ENDURING TYPE IIn SUPERNOVAE 2005ip AND 2006jd

Stritzinger

Taddia

Fransson

et al. 2012

ApJ

169

246

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We present an observational study of the Type IIn supernovae (SNe IIn) 2005ip and 2006jd. Broadband UV, optical, and near-IR photometry, and visual-wavelength spectroscopy of SN 2005ip complement and extend upon published observations to 6.5 years past discovery. Our observations of SN 2006jd extend from UV to mid-infrared wavelengths, and like SN 2005ip, are compared to reported X-ray measurements to understand the nature of the progenitor. Both objects display a number of similarities with the 1988Z-like subclass of SN IIn including (1) remarkably similar early-and late-phase optical spectra, (2) a variety of high-ionization coronal lines, (3) longduration optical and near-IR emission, and (4) evidence of cold and warm dust components. However, diversity is apparent, including an unprecedented late-time r-band excess in SN 2006jd. The observed differences are attributed to differences between the mass-loss history of the progenitor stars. We conclude that the progenitor of SN 2006jd likely experienced a significant mass-loss event during its pre-SN evolution akin to the great 19th century eruption of η Carinae. Contrarily, as advocated by Smith et al., the circumstellar environment of SN 2005ip is found to be more consistent with a clumpy wind progenitor.

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Section: Discussionsupporting

confidence: 63%

MULTI-WAVELENGTH OBSERVATIONS OF THE ENDURING TYPE IIn SUPERNOVAE 2005ip AND 2006jd

Stritzinger

Taddia

Fransson

et al. 2012

ApJ

169

246

View full text Add to dashboard Cite

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“…The minimal velocity of ∼800 km s −1 could be associated with the cloud shocks speed and perhaps with the velocity of the undisturbed CSM. The latter is about 620 km s −1 as indicated by the absorption minimum of narrow lines of O i 7773 Å and He i 6678 Å (Anupama et al 2009). Interestingly, the expansion velocity of CSM of SN 2000er indicated by narrow He i absorption components in early spectra is 800–900 km s −1 (Pastorello et al 2008), close to this value.…”

Section: Early Cs Interactionmentioning

confidence: 99%

Circumstellar interaction in type Ibn supernovae and SN 2006jc

Чугай

2009

Monthly Notices of the Royal Astronomical Society

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I analyse peculiar properties of light curve and continua of enigmatic Ibn supernovae, including SN 2006jc, and argue in favour of the early strong circumstellar interaction. This interaction explains the high luminosity and fast flux rise of SN 1999cq, while the cool dense shell formed in shocked ejecta can explain the smooth early continuum of SN 2000er and unusual blue continuum of SN 2006jc. The dust is shown to condense in the cool dense shell at about day 50. Monte Carlo modelling of the He I 7065 \AA line profile affected by the dust occultation supports a picture, in which the dust resides in the fragmented cool dense shell, whereas He I lines originate from circumstellar clouds shocked and fragmented in the forward shock wave.Comment: 10 pages, 6 figures, MNRAS accepte

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“…Balmer lines were not visible or extremely weak (Pastorello et al 2008b). The natural explanation is that the outbursting progenitor was not an LBV but was instead a WR star (Pastorello et al 2007a;Foley et al 2007;Immler et al 2008;Tominaga et al 2008;Anupama et al 2009).…”

Section: Sn 2010al and Type Ibn Supernovaementioning

confidence: 99%

Supernovae interacting with a circumstellar medium: New observations with X‐shooter

et al. 2011

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In this article we present new data of a sample of core-collapse supernovae showing unequivocal evidences of interaction between their ejecta and pre-existing circumstellar matter (CSM). This CSM was produced by the progenitor star through major mass loss episodes during the final stages of its life. The study of the properties of the SN ejecta and the circumstellar environment are crucial to unveil the nature of the progenitors producing interacting supernovae. In this context, the instrumental combination Very Large Telescope (VLT) plus X-shooter provides spectra covering simultaneously the optical and near-infrared domains, and with adequate resolution to constrain the main properties of the supernova and its environment, including its chemical composition, the ejection velocity and the distribution of the emitting gas.

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Optical photometry and spectroscopy of the Type Ibn supernova SN 2006jc until the onset of dust formation

Cited by 39 publications

References 33 publications

MULTI-WAVELENGTH OBSERVATIONS OF THE ENDURING TYPE IIn SUPERNOVAE 2005ip AND 2006jd

MULTI-WAVELENGTH OBSERVATIONS OF THE ENDURING TYPE IIn SUPERNOVAE 2005ip AND 2006jd

Circumstellar interaction in type Ibn supernovae and SN 2006jc

Supernovae interacting with a circumstellar medium: New observations with X‐shooter

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