Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 867, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/2041-8213/aaeb2e
Keywords
supernovae: general; supernovae: individual (SN 2017ens)
Categories
Funding
- Alexander von Humboldt Foundation
- Royal Society-Science Foundation Ireland University Research Fellowship
- Sofia Kovalevskaja Award (Alexander von Humboldt Foundation)
- TABASGO Foundation
- Miller Institute for Basic Research in Science (U.C. Berkeley)
- Australian Research Council [FT170100243, FT160100028]
- KAW Foundation
- European Research Council [291222]
- STFC [ST/P000312/1]
- Polish National Science Centre [OPUS 2015/17/B/ST9/03167]
- UK STFC through an Ernest Rutherford Fellowship
- Horizon 2020 ERC [758638]
- US NSF [AST-1311862]
- EU/FP7-ERC grant [615929]
- MoST (Taiwan) [105-2112-M-008-002-MY3, 104-2923-M-008-004-MY5, 106-2112-M-008-007]
- PRIN-INA F2017 Toward the SKA and CTA era: discovery, localization, and physics of transient sources
- EU via ERC [725161]
- Quantum Universe I-Core program
- ISF
- BSF Transformative program
- Kimmel award
- MoST [105-2112-M-008-024-MY3]
- W. M. Keck Foundation
- DFG [HA 1850/28-1]
- Christopher R. Redlich fund
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1720756] Funding Source: National Science Foundation
- STFC [ST/R000484/1, ST/F007159/1, ST/P000312/1, ST/L00061X/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/P000312/1] Funding Source: researchfish
Ask authors/readers for more resources
We present observations of supernova (SN) 2017ens, discovered by the ATLAS survey and identified as a hot blue object through the GREAT program. The redshift z = 0.1086 implies a peak brightness of M-g = -21.1 mag, placing the object within the regime of superluminous supernovae. We observe a dramatic spectral evolution, from initially being blue and featureless, to later developing features similar to those of the broadlined Type Ic SN 1998bw, and finally showing 2000 km s(-1) wide H alpha and H beta emission. Relatively narrow Balmer emission (reminiscent of a SN IIn) is present at all times. We also detect coronal lines, indicative of a dense circumstellar medium. We constrain the progenitor wind velocity to similar to 50-60 km s(-1) based on P-Cygni profiles, which is far slower than those present in Wolf-Rayet stars. This may suggest that the progenitor passed through a luminous blue variable phase, or that the wind is instead from a binary companion red supergiant star. At late times we see the similar to 2000 km s(-1) wide H alpha emission persisting at high luminosity (similar to 3 x 10(40) erg s(-1)) for at least 100 day, perhaps indicative of additional mass loss at high velocities that could have been ejected by a pulsational pair instability.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available