The Type IIn Supernova SN 2010bt: The Explosion of a Star in Outburst

@article{EliasRosa2018TheTI,
  title={The Type IIn Supernova SN 2010bt: The Explosion of a Star in Outburst},
  author={Nancy Elias-Rosa and Schuyler D. van Dyk and Stefano Benetti and Enrico Cappellaro and Nathan Smith and Rubina Kotak and Massimo Turatto and Alexei V. Filippenko and Giuliano Pignata and Ori D. Fox and Llu{\'i}s Galbany and Santiago Gonz{\'a}lez-Gait{\'a}n and Matteo Miluzio and Libert A. G. Monard and Mattias Ergon},
  journal={The Astrophysical Journal},
  year={2018},
  volume={860}
}
It is well known that massive stars (M > 8 M☉) evolve up to the collapse of the stellar core, resulting in most cases in a supernova (SN) explosion. Their heterogeneity is related mainly to different configurations of the progenitor star at the moment of the explosion and to their immediate environments. We present photometry and spectroscopy of SN 2010bt, which was classified as a Type IIn SN from a spectrum obtained soon after discovery and was observed extensively for about 2 months. After… 
Radiation hydrodynamical simulations of eruptive mass loss from progenitors of Type Ibn/IIn supernovae
Observations suggest that some massive stars experience violent and eruptive mass loss associated with significant brightening that cannot be explained by hydrostatic stellar models. This event
The complex multi-component outflow of the Seyfert galaxy NGC 7130 (Corrigendum)
Active galactic nuclei (AGN) are a key ingredient for understanding galactic evolution, as their activity is coupled to the host galaxy properties through feedback processes. AGN-driven outflows are
High-resolution spectroscopy of SN 2017hcc and its blueshifted line profiles from post-shock dust formation
SN2017hcc was remarkable for being a nearby and strongly polarized superluminous TypeIIn supernova (SN). We obtained high-resolution echelle spectra that we combine with other spectra to investigate
A Diversity of Wave-driven Presupernova Outbursts
Many core-collapse supernova (SN) progenitors show indications of enhanced pre-SN mass loss and outbursts, some of which could be powered by wave energy transport within the progenitor star.
Wind-envelope interaction as the origin of the slow cyclic brightness variations of luminous blue variables
Luminous blue variables (LBVs) are hot, very luminous massive stars displaying large quasi-periodic variations in brightness, radius, and photospheric temperature on timescales of years to decades.
CHIPS: Complete History of Interaction-powered Supernovae
We present the public release of the Complete History of Interaction-Powered Supernovae (CHIPS) code, which is suited to model a variety of transients that arise from interaction with a dense
Type IIn Supernova Light Curves Powered by Forward and Reverse Shocks
We present a bolometric light-curve model of Type IIn supernovae powered by supernova ejecta colliding with a circumstellar medium. We estimate the conversion efficiency of the ejecta’s kinetic
MUSE-AO view of the starburst–AGN connection: NGC 7130
We present the discovery of a small kinematically decoupled core of 0.″2 (60 pc) in radius as well as an outflow jet in the archetypical AGN–starburst “composite” galaxy NGC 7130 from integral field

References

SHOWING 1-10 OF 77 REFERENCES
A MASSIVE PROGENITOR OF THE LUMINOUS TYPE IIn SUPERNOVA 2010jl
The bright, nearby, recently discovered supernova (SN) 2010jl is a luminous Type IIn SN. Here, we report archival Hubble Space Telescope (HST) observations of its host galaxy UGC 5189A taken roughly
On the Progenitor of SN 2005gl and the Nature of Type IIn Supernovae
We present a study of the Type IIn supernova (SN) 2005gl, in the relatively nearby (d ≈ 66 Mpc) galaxy NGC 266. Photometry and spectroscopy of the SN indicate that it is a typical member of its
A massive hypergiant star as the progenitor of the supernova SN 2005gl
TLDR
It is reported that the previously proposed object was indeed the progenitor star of SN 2005gl, likely a luminous blue variable that standard stellar evolution predicts should not have exploded in that state.
A Panchromatic View of the Restless SN 2009ip Reveals the Explosive Ejection of a Massive Star Envelope
The double explosion of SN 2009ip in 2012 raises questions about our understanding of the late stages of massive star evolution. Here we present a comprehensive study of SN 2009ip during its
The Unprecedented Third Outburst of SN 2009ip: A Luminous Blue Variable Becomes a Supernova
Some reports of supernova (SN) discoveries turn out not to be true core-collapse explosions. One such case was SN 2009ip, which was recognized to be a luminous blue variable (LBV) eruption. This
Coronal lines and dust formation in SN 2005ip: Not the brightest, but the hottest Type IIn supernova
We present optical photometry and spectroscopy of SN 2005ip for the first 3 yr after discovery, showing an underlying Type II-L supernova (SN) interacting with a steady wind to yield an unusual Type
Clues to the nature of SN 2009ip - II. The continuing photometric and spectroscopic evolution to 1000 days
The 2012 brightening of SN 2009ip was dominated by emission from the interaction of ejecta with the surrounding circumstellar material (CSM) produced by episodic mass loss from the progenitor,
Supernova 1998S at 14 years postmortem: continuing circumstellar interaction and dust formation
We report late-time spectroscopic observations of the Type IIn supernova (SN) 1998S, taken 14 years after explosion using the Large Binocular Telescope. The optical spectrum exhibits strong, broad
Optical and infrared photometry of the Type IIn SN 1998S: days 11–146
We present contemporaneous optical and infrared (IR) photometric observations of the Type IIn SN 1998S covering the period between 11 and 146 d after discovery. The IR data constitute the first ever
Carnegie Supernova Project: Observations of Type IIn supernovae ⋆
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
...
...