Journal
ASTROPHYSICAL JOURNAL
Volume 769, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/769/1/39
Keywords
galaxies: clusters: general; galaxies: star formation; stars: winds, outflows; supernovae: general; supernovae: individual (PS1-12sk)
Categories
Funding
- National Science Foundation [NSF PHY11-25915, AST-1009749]
- David and Lucile Packard Foundation Fellowship for Science and Engineering
- NSF STS postdoctoral fellowship
- National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]
- NSF [AST-1211196]
- NASA
- US National Science Foundation (NSF)
- National Aeronautics and Space Administration
- Science and Technology Facilities Council [ST/I001123/1, ST/G009465/1] Funding Source: researchfish
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0907903, 1211196, 1238877] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1009749] Funding Source: National Science Foundation
- STFC [ST/I001123/1, ST/G009465/1] Funding Source: UKRI
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We report on our discovery and observations of the Pan-STARRS1 supernova (SN) PS1-12sk, a transient with properties that indicate atypical star formation in its host galaxy cluster or pose a challenge to popular progenitor system models for this class of explosion. The optical spectra of PS1-12sk classify it as a Type Ibn SN (SN Ibn; cf. SN 2006jc), dominated by intermediate-width (3 x 10(3) km s(-1)) and time variable He I emission. Our multi-wavelength monitoring establishes the rise time dt similar to 9-23 days and shows an NUV-NIR spectral energy distribution with temperature greater than or similar to 17x10(3) K and a peak magnitude of M-z = -18.88 +/- 0.02 mag. SN Ibn spectroscopic properties are commonly interpreted as the signature of a massive star (17-100M(circle dot)) explosion within an He-enriched circumstellar medium. However, unlike previous SNe Ibn, PS1-12sk is associated with an elliptical brightest cluster galaxy, CGCG 208-042 (z = 0.054) in cluster RXC J0844.9+4258. The expected probability of an event like PS1-12sk in such environments is low given the measured infrequency of core-collapse SNe in red-sequence galaxies compounded by the low volumetric rate of SN Ibn. Furthermore, we find no evidence of star formation at the explosion site to sensitive limits (Sigma(H alpha) less than or similar to 2 x 10(-3) M-circle dot yr(-1) kpc(-2)). We therefore discuss white dwarf binary systems as a possible progenitor channel for SNe Ibn. We conclude that PS1-12sk represents either a fortuitous and statistically unlikely discovery, evidence for a top-heavy initial mass function in galaxy cluster cooling flow filaments, or the first clue suggesting an alternate progenitor channel for SNe Ibn.
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