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iPTF 16hgs: A Double-peaked Ca-rich Gap Transient in a Metal-poor, Star-forming Dwarf Galaxy
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Number of Authors: 212018 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 866, no 1, article id 72Article in journal (Refereed) Published
Abstract [en]

Calcium-rich gap transients represent an intriguing new class of faint and fast-evolving supernovae that exhibit strong [Ca II] emission in their nebular phase spectra. In this paper, we present the discovery and follow-up observations of a faint and fast-evolving transient, iPTF 16hgs, that exhibited a double-peaked light curve. Exhibiting a Type Ib spectrum in the photospheric phase and an early transition to a [Ca II] dominated nebular phase, iPTF 16hgs shows properties consistent with the class of Ca-rich gap transients, with two important exceptions. First, while the second peak of the light curve is similar to other Ca-rich gap transients, the first blue and fast-fading peak (declining over approximate to 2 days) is unique to this source. Second, we find that iPTF 16hgs occurred in the outskirts (projected offset of approximate to 6 kpc approximate to 1.9 R-eff) of a low-metallicity (approximate to 0.4 Z(circle dot)), star-forming, dwarf spiral galaxy. Deep limits from late-time radio observations suggest a low-density environment for the source. If iPTF 16hgs shares explosion physics with the class of Ca-rich gap transients, the first peak can be explained by the presence of 0.01 M-circle dot of Ni-56 in the outer layers the ejecta, reminiscent of some models of He-shell detonations on WDs. However, if iPTF 16hgs is physically unrelated to the class, the first peak is consistent with shock cooling emission (of an envelope with a mass of approximate to 0.08 M-circle dot and radius of approximate to 13 R-circle dot) in a core-collapse explosion of a highly stripped massive star in a close binary system.

Place, publisher, year, edition, pages
2018. Vol. 866, no 1, article id 72
Keywords [en]
supernovae: general, supernovae: individual (iPTF 16hgs), surveys
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Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-161969DOI: 10.3847/1538-4357/aadf8eISI: 000447585000008OAI: oai:DiVA.org:su-161969DiVA, id: diva2:1264930
Available from: 2018-11-21 Created: 2018-11-21 Last updated: 2019-12-04Bibliographically approved

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Lunnan, Ragnhild
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Department of AstronomyThe Oskar Klein Centre for Cosmo Particle Physics (OKC)
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