Publications (2)0 Total impact
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Maximilian Stritzinger,
Francesco Taddia,
Claes Fransson,
Ori D. Fox,
Nidia Morrell,
M. M. Phillips,
Jesper Sollerman, J. P. Anderson,
Luis Boldt,
Peter J. Brown, [......],
Carlos Contreras,
Gaston Folatelli,
S. M. Habergham,
Mario Hamuy,
Jens Hjorth,
Phil A. James,
Wojtek Krzeminski,
Seppo Mattila,
Sven E. Persson,
Miguel Roth
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ABSTRACT: We present an observational study of the Type IIn supernovae (SNe IIn) 2005ip
and 2006jd. Broad-band 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: (i) remarkably similar early- and late-phase
optical spectra, (ii) a variety of high ionization coronal lines, (iii)
long-duration optical and near-IR emission and, (iv) 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
\eta Carinae. Contrarily, as advocated by Smith et al. (2009), we find the
circumstellar environment of SN 2005ip to be more consistent with a clumpy wind
progenitor.
06/2012;
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Giuliano Pignata,
Maximilian Stritzinger,
Alicia Soderberg,
Paolo Mazzali,
M. M. Phillips,
Nidia Morrell, J. P. Anderson,
Luis Boldt,
Abdo Campillay,
Carlos Contreras, [......],
Miguel Roth,
Francisco Salgado Emily M. Levesque,
Armin Rest,
J. Adam Crain,
Andrew C. Foster,
Joshua B. Haislip,
Kevin M. Ivarsen,
Aaron P. LaCluyze,
Melissa C. Nysewander,
Daniel E. Reichart
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ABSTRACT: Ultraviolet, optical, and near-infrared photometry and optical spectroscopy of the broad-lined Type Ic supernova (SN) 2009bb are presented, following the flux evolution from -10 to +285 days past B-band maximum. Thanks to the very early discovery, it is possible to place tight constraints on the SN explosion epoch. The expansion velocities measured from near maximum spectra are found to be only slightly smaller than those measured from spectra of the prototype broad-lined SN 1998bw associated with GRB 980425. Fitting an analytical model to the pseudo-bolometric light curve of SN 2009bb suggests that 4.1+-1.9 Msun of material was ejected with 0.22 +-0.06 Msun of it being 56Ni. The resulting kinetic energy is 1.8+-0.7x10^52 erg. This, together with an absolute peak magnitude of MB=-18.36+-0.44, places SN 2009bb on the energetic and luminous end of the broad-lined Type Ic (SN Ic) sequence. Detection of helium in the early time optical spectra accompanied with strong radio emission, and high metallicity of its environment makes SN 2009bb a peculiar object. Similar to the case for GRBs, we find that the bulk explosion parameters of SN 2009bb cannot account for the copious energy coupled to relativistic ejecta, and conclude that another energy reservoir (a central engine) is required to power the radio emission. Nevertheless, the analysis of the SN 2009bb nebular spectrum suggests that the failed GRB detection is not imputable to a large angle between the line-of-sight and the GRB beamed radiation. Therefore, if a GRB was produced during the SN 2009bb explosion, it was below the threshold of the current generation of gamma-ray instruments. Comment: Accepted for publication in ApJ
11/2010;
