Possible evidence of asymmetry in SN 2007rt, a type IIn supernova

Trundle, C.; Pastorello, A.; Benetti, S.; Kotak, R.; Valenti, S.; Agnoletto, I.; Bufano, F.; Dolci, M.; Elias‐Rosa, N.; Greiner, T.; Hunter, David J.; Keenan, F. P.; Lorenzi, V.; Maguire, K.; Taubenberger, S.

doi:10.1051/0004-6361/200911776

Cited by 29 publications

(29 citation statements)

References 70 publications

(108 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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: 72%

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

Stritzinger

Taddia

Fransson

et al. 2012

ApJ

168

246

View full text Add to dashboard Cite

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.

show abstract

Section: Discussionsupporting

confidence: 72%

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

Stritzinger

Taddia

Fransson

et al. 2012

ApJ

168

246

View full text Add to dashboard Cite

show abstract

“…P Cygni, see above) or the escape velocity from a blue supergiant. Similar ∼100 km s −1 P Cygni profiles have been seen in a number of SNe IIn, such as SNe 1997ab (Salamanca 2000), 1997eg (Salamanca et al 2002), 1998S (Fassia et al 2001) and 2007rt (Trundle et al 2009), implying that the progenitors of each of these SNe may have been in a similar state shortly before core collapse.…”

Section: Discussionsupporting

confidence: 65%

SN 2008iy: an unusual Type IIn Supernova with an enduring 400-d rise time

Miller

Silverman

Butler

et al. 2010

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present spectroscopic and photometric observations of the Type IIn supernova (SN) 2008iy. SN 2008iy showed an unprecedentedly long rise time of ∼400 d, making it the first known SN to take significantly longer than 100 d to reach peak optical luminosity. The peak absolute magnitude of SN 2008iy was Mr≈−19.1 mag, and the total radiated energy over the first ∼700 d was ∼2 × 1050 erg. Spectroscopically, SN 2008iy is very similar to the Type IIn SN 1988Z at late times and, like SN 1988Z, it is a luminous X‐ray source (both SNe had an X‐ray luminosity LX > 1041 erg s−1). SN 2008iy has a growing near‐infrared excess at late times similar to several other SNe IIn. The Hα emission‐line profile of SN 2008iy shows a narrow P Cygni absorption component, implying a pre‐SN wind speed of ∼100 km s−1. We argue that the luminosity of SN 2008iy is powered via the interaction of the SN ejecta with a dense, clumpy circumstellar medium. The ∼400‐d rise time can be understood if the number density of clumps increases with distance over a radius ∼1.7 × 1016 cm from the progenitor. This scenario is possible if the progenitor experienced an episodic phase of enhanced mass loss <1 century prior to explosion or if the progenitor wind speed increased during the decades before core collapse. We favour the former scenario, which is reminiscent of the eruptive mass‐loss episodes observed for luminous blue variable (LBV) stars. The progenitor wind speed and increased mass‐loss rates serve as further evidence that at least some, and perhaps all, Type IIn SNe experience LBV‐like eruptions shortly before core collapse. We also discuss the host galaxy of SN 2008iy, a subluminous dwarf galaxy, and offer a few reasons why the recent suggestion that unusual, luminous SNe preferentially occur in dwarf galaxies may be the result of observational biases.

show abstract

“…There is also weak evidence of He ii λ4686, He i λ7281, and [O ii] λλ7320, 7330. In general, SN 2010jl is spectroscopically very similar to other well studied type IIn events, such as SN 2007rt (Trundle et al 2009 and references therein).…”

Section: Flux Spectrumsupporting

confidence: 58%

Asymmetries in the type IIn SN 2010jl

Patat

Taubenberger

Benetti

et al. 2011

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We study possible signs of asymmetry in the luminous type IIn SN 2010jl, to obtain independent information about its explosion geometry. Methods. We performed optical linear spectropolarimetry of SN 2010jl two weeks after the discovery, in the spectral range 3700-8800 Å.Results. The object exhibits a continuum polarization at a very significant and almost constant level (1.7-2.0%). Distinctive line depolarization is seen at the positions of the strongest emission features, such as Hα and Hβ. This implies that the line forming region is well above the photosphere. The continuum polarization level (1.7-2.0%) indicates a substantial asphericity, of axial ratio ≤0.7. The almost complete depolarization seen at Hα is indicative of a very low level of interstellar polarization (≤0.3%). This rules out the presence of relevant amounts of dust in the progenitor environment at the time of our observations. From a polarimetric point of view, SN 2010jl appears to be very similar to the two other well-studied type IIn SNe 1997eg and 1998S, establishing a strong link between members of this class of objects.

show abstract

Possible evidence of asymmetry in SN 2007rt, a type IIn supernova

Cited by 29 publications

References 70 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

SN 2008iy: an unusual Type IIn Supernova with an enduring 400-d rise time

Asymmetries in the type IIn SN 2010jl

Contact Info

Product

Resources

About