| dc.contributor |
Massachusetts Institute of Technology. Program in Science, Technology and Society |
|
| dc.contributor |
Friedman, Andrew Samuel |
|
| dc.creator |
Friedman, Andrew Samuel |
|
| dc.date |
2015-01-29T18:37:38Z |
|
| dc.date |
2015-01-29T18:37:38Z |
|
| dc.date |
2013-05 |
|
| dc.date |
2013-02 |
|
| dc.date.accessioned |
2023-03-01T18:05:56Z |
|
| dc.date.available |
2023-03-01T18:05:56Z |
|
| dc.identifier |
0004-637X |
|
| dc.identifier |
1538-4357 |
|
| dc.identifier |
http://hdl.handle.net/1721.1/93202 |
|
| dc.identifier |
Sanders, N. E., A. M. Soderberg, R. J. Foley, R. Chornock, D. Milisavljevic, R. Margutti, M. R. Drout, et al. “PS1-12sk IS A PECULIAR SUPERNOVA FROM A He-RICH PROGENITOR SYSTEM IN A BRIGHTEST CLUSTER GALAXY ENVIRONMENT.” The Astrophysical Journal 769, no. 1 (May 2, 2013): 39. |
|
| dc.identifier.uri |
http://localhost:8080/xmlui/handle/CUHPOERS/278739 |
|
| dc.description |
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 × 10[superscript 3] km s[superscript –1]) and time variable He I emission. Our multi-wavelength monitoring establishes the rise time dt ~ 9-23 days and shows an NUV-NIR spectral energy distribution with temperature [> over ~] 17 × 10[superscript 3] K and a peak magnitude of M[subscript z] = –18.88 ± 0.02 mag. SN Ibn spectroscopic properties are commonly interpreted as the signature of a massive star (17-100 M ☉) 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 (Σ[subscript Hα] [< over ~] 2 × 10[superscript –3] M[subscript ☉] yr[superscript –1] kpc[superscript –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. |
|
| dc.description |
National Science Foundation (U.S.). Science, Technology, and Society (Postdoctoral Fellowship) |
|
| dc.description |
National Science Foundation (U.S.) (Grant AST-1009749) |
|
| dc.format |
application/pdf |
|
| dc.language |
en_US |
|
| dc.publisher |
IOP Publishing |
|
| dc.relation |
http://dx.doi.org/10.1088/0004-637x/769/1/39 |
|
| dc.relation |
Astrophysical Journal |
|
| dc.rights |
Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. |
|
| dc.source |
American Astronomical Society |
|
| dc.title |
PS1-12sk IS A PECULIAR SUPERNOVA FROM A He-RICH PROGENITOR SYSTEM IN A BRIGHTEST CLUSTER GALAXY ENVIRONMENT |
|
| dc.type |
Article |
|
| dc.type |
http://purl.org/eprint/type/JournalArticle |
|