Details

Autor(en) / Beteiligte

• De, Kishalay
• Kasliwal, Mansi M.
• Cantwell, Therese
• Cao, Yi
• Cenko, S. Bradley
• Gal-Yam, Avishay
• Johansson, Joel
• Kong, Albert
• Kulkarni, Shrinivas R.
• Lunnan, Ragnhild
• Masci, Frank
• Matuszewski, Matt
• Mooley, Kunal P.
• Neill, James D.
• Nugent, Peter E.
• Ofek, Eran O.
• Perrott, Yvette
• Rebbapragada, Umaa D.
• Rubin, Adam
• Sullivan, Donal O'
• Yaron, Ofer

Titel

iPTF 16hgs: A Double-peaked Ca-rich Gap Transient in a Metal-poor, Star-forming Dwarf Galaxy

Ist Teil von

• The Astrophysical journal, 2018-10, Vol.866 (1), p.72

Ort / Verlag

Philadelphia: The American Astronomical Society

Erscheinungsjahr

2018

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• 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 2 days) is unique to this source. Second, we find that iPTF 16hgs occurred in the outskirts (projected offset of 6 kpc 1.9 Reff) of a low-metallicity ( 0.4 Z ), 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 of 56Ni 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 0.08 M and radius of 13 R ) in a core-collapse explosion of a highly stripped massive star in a close binary system.