Carnegie Supernova Project: Observations of Type IIn supernovae ⋆

By F. Taddia, M. Stritzinger, J. Sollerman, M. Phillips, Joseph P. Anderson, L. Boldt, A. Campillay, S. Castellón, C. Contreras, G. Folatelli and 9 more. 2013

166 citations recorded by the source corpus.

Supernovae (SNe) are the final stage in the life of massive stars. Their explosion unbinds the progenitor star revealing its inner layers. The SN ejecta interact with the circumstellar material (CSM), providing further information on the progenitor star.In this work we present the study of rare SN subtypes, aiming to investigate their observational and physical properties and those of their progenitor stars.These studies include the analysis of SN samples as well as that of single objects.Two main SN classes are discussed: radioactively-powered events and SNe interacting with their CSM.Within the first group, we investigated the rare (~1% of core-collapse SNe) family of SN 1987A-like events. These SNe are found to be the explosion of compact, hydrogen-rich blue supergiant (BSG) stars, and to occur mainly in moderately low metallicity environs. We also studied a sample of 20 stripped-envelope (SE) SNe, which are also powered by the decay of radioactive 56Ni. These SNe are the result of the core-collapse of massive, hydrogen or even helium-poor stars stripped of their outer envelopes by line-driven winds and/or by the accretion onto companion stars.We investigated the differences among the early-time light curves of the subtypes forming the SE SN group (IIb, Ib, Ic, Ic-BL) and found that in all of them the 56Ni is strongly mixed out in the ejecta. This result suggests that the difference between helium-poor and helium-rich SNe is due to an actual lack of helium in SNe Ic and Ic-BL rather than to a different degree of 56Ni mixing.Our work on CSM-interacting SNe include the study of a sample of SNe IIn, i.e. core-collapse SNe interacting with hydrogen-rich CSM, and the analysis of SN 2008J, a particularly rare event which we interpreted as the interaction of a thermonuclear SN Ia with a thick hydrogen-rich CSM. Spectral analysis of the SN IIn sample suggests that these SNe are likely to be the explosion of luminous blue variable stars (LBVs), although other channels are not excluded.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/186af62958505243fdbc124bcb784a8f10c6a508

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. A. Filippenko
2. N. Smith
3. S. Valenti
4. V. Morozova
5. A. Piro
6. Weidong Li
7. S. Smartt
8. Stan Woosley

In Electrical and Electronic Engineering

1. N. Smith
2. A. Filippenko
3. Weidong Li
4. Stan Woosley
5. D. DePoy

In Instrumentation

1. N. Smith
2. Stan Woosley
3. Weidong Li
4. A. Filippenko
5. W. Freedman
6. C. Burns
7. M. Hamuy
8. S. E. Persson

Citations in the corpus

• CHARACTERIZING THE V-BAND LIGHT-CURVES OF HYDROGEN-RICH TYPE II SUPERNOVAE (2014, background): “…IIn show narrow emission lines within their spectra (Schlegel 1990), but present a large diversity of photometric and spectral properties (see e.g. Kiewe et al. 2012; Taddia et al. 2013), which clouds interpretations of their progenitor systems and how they link to the ‘normal’ SNe II population.”
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “The mass-loss rates indicated by the CSM suggest that viable progenitors could be LBVs (Gal-Yam et al. 2007, Taddia et al. 2013) as well as extreme RSGs or YHGs (Smith et al. 2009) (see Fig 3).”
• Pulsational Pair-instability Supernovae (2016, background): “Still, observations hint that luminous blue stars, LBVs in particular, may be the immediate precursors of some unusual Type IIn supernovae Gal-Yam & Leonard (2009); Mauerhan et al. (2013); Smith et al. (2007); Taddia et al. (2013).”
• The Carnegie Supernova Project. I. Third Photometry Data Release of Low-redshift Type Ia Supernovae and Other White Dwarf Explosions (2017, background): “Photometry of seven SNeIIn has already been presented by Stritzinger et al. (2012) and Taddia et al. (2013).”
• Unifying Type II Supernova Light Curves with Dense Circumstellar Material (2016, background): “This can manifests itself in narrow optical emission lines (Filippenko 1997; Pastorello et al. 2008; Kiewe et al. 2012; Taddia et al. 2013), X-ray or radio emission (Campana et al. 2006; Corsi et al. 2014), or a rapid rise at ultraviolet wavelengths (Ofek et al. 2010; Gezari et al. 2015; Tanaka et…”