April 3, 2017 report
New slowly evolving Type Ibn supernova discovered
Type Ibn supernovae are explosions whose spectra are characterized by low-velocity helium emission lines. They are thought to be the core-collapse explosions of massive stars whose ejecta interact with helium-rich circumstellar material. They have also relatively high peak luminosities and are blue at peak.
Type Ibn supernovae are usually fast evolving with a short rise to peak brightness (less than two weeks) and a subsequent fast decline. However, a group of researchers led by Emir Karamehmetoglu of the Stockholm University in Sweden has found a new Type Ibn supernova that exhibits an unprecedentedly long rise time and a much broader light curve compared to other supernovae in this class.
Karamehmetoglu's team discovered OGLE-2014-SN-131 on November 11, 2014 using the OGLE-IV Transient Detection System. Afterward, the researchers conducted follow-up photometric observations of this supernova with the OGLE telescope at the Las Campanas Observatory in Chile and with the Gamma-Ray Burst Optical/Near-Infrared Detector (GROND) mounted on the 2.2m MPG/ESO telescope at La Silla, also in Chile. Moreover, they performed spectroscopic observations of OGLE-2014-SN-131 with the ESO New Technology Telescope (NTT) at La Silla and with the Very Large Telescope (VLT) at Cerro Paranal in Chile.
These observations show that OGLE-2014-SN-131 spectroscopically resembles other Type Ibn supernovae such as SN 2010al and showcases also peak luminosity and post-peak colors similar to other events in this class. Notably, however, the light curve of OGLE-2014-SN-131 is broader and longer-rising than any other Type Ibn supernova.
"Spectroscopy and multi-band photometry of OGLE14-131 have been presented. Identification of prominent He I emission lines classifies this SN as a Type Ibn. While, spectroscopically, OGLE14-131 is identified as a normal SN Ibn, when compared to other Type Ibn SNe, its broad light curve shows the longest rise time ever observed for this SN class," the authors write.
The researchers try to explain this record-long rise time, noting that it requires higher ejecta and circumstellar material masses for the progenitor when compared to typical supernova Ibn progenitors. Therefore, they concluded that the most likely progenitor scenario for OGLE-2014-SN-131 is a massive Wolf–Rayet star.
"To explain the unusually long rise time, the broad light curve, the light curve decline, and the spectra characterized by narrow emission lines, we favor a powering mechanism where the SN ejecta are interacting with a dense curcumstellar material. The progenitor of OGLE-2014-SN-131 was likely a Wolf-Rayet star with a mass greater than that of a typical SN Ibn progenitor, which expelled the circumstellar material that the SN is interacting with," the team wrote in the paper.
The astronomers added that given the fact that OGLE-2014-SN-131 has an unusually massive progenitor for a Type Ibn supernova, we should expect a low number of similar slowly evolving events as such massive stars should be relatively rare.
Type Ibn supernovae (SNe Ibn) are thought to be the core-collapse explosions of massive stars whose ejecta interact with He-rich circumstellar material (CSM). We report the discovery of a SN Ibn, with the longest rise-time ever observed, OGLE-2014-SN-131. We discuss the potential powering mechanisms and the progenitor nature of this peculiar stripped-envelope (SE), circumstellar-interacting SN. Optical photometry and spectroscopy were obtained with multiple telescopes including VLT, NTT, and GROND. We compare light curves and spectra with those of other known SNe Ibn and Ibc. CSM velocities are derived from the spectral analysis. The SN light curve is modeled under different assumptions about its powering mechanism (56Ni decay, CSM-interaction, magnetar) in order to estimate the SN progenitor parameters. OGLE-2014-SN-131 spectroscopically resembles SNe Ibn such as SN 2010al. Its peak luminosity and post-peak colors are also similar to those of other SNe Ibn. However, it shows an unprecedentedly long rise-time and a much broader light curve compared to other SNe Ibn. Its bolometric light curve can be reproduced by magnetar and CSM-interaction models, but not by a 56Ni-decay powering model. To explain the unusually long rise-time, the broad light curve, the light curve decline, and the spectra characterized by narrow emission lines, we favor a powering mechanism where the SN ejecta are interacting with a dense CSM. The progenitor of OGLE-2014-SN-131 was likely a Wolf-Rayet star with a mass greater than that of a typical SN Ibn progenitor, which expelled the CSM that the SN is interacting with.
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