Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 449, Issue 2, Pages 1876-1896Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv354
Keywords
circumstellar matter; stars: evolution; supernovae: general; supernovae: individual: PTF11iqb; stars: winds, outflows
Categories
Funding
- W.M. Keck Foundation
- NSF [AST-1210599, AST-1312221, AST-1211916, AST-1009571, AST-1210311]
- Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ)
- Israeli Ministry of Science
- Israel Science Foundation
- Minerva
- I-CORE Program of the Planning and Budgeting Committee
- EU/FP7 via ERC [307260]
- Quantum Universe I-Core program by the Israeli Committee
- ISF
- WIS-UK 'making connections'
- Kimmel and ARCHES awards
- Gary & Cynthia Bengier
- Richard & Rhoda Goldman Fund
- Christopher R. Redlich Fund
- TABASGO Foundation
- NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]
- Marie Curie Intra-European Fellowship, within the 7th European Community Framework Programme (FP7)
- Royal Society
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1210311, 1009987] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1009571, 1210599, 1211916, 1302771] Funding Source: National Science Foundation
Ask authors/readers for more resources
The supernova (SN) PTF11iqb was initially classified as a Type IIn event caught very early after explosion. It showed narrowWolf-Rayet (WR) spectral features on day 2 (as in SN 1998S and SN 2013cu), but the narrow emission weakened quickly and the spectrum morphed to resemble Types II-L and II-P. At late times, H alpha exhibited a complex, multipeaked profile reminiscent of SN 1998S. In terms of spectroscopic evolution, we find that PTF11iqb was a near twin of SN 1998S, although with somewhat weaker interaction with circumstellar material (CSM) at early times, and stronger interaction at late times. We interpret the spectral changes as caused by early interaction with asymmetric CSM that is quickly (by day 20) enveloped by the expanding SN ejecta photosphere, but then revealed again after the end of the plateau when the photosphere recedes. The light curve can be matched with a simple model for CSM interaction (with a mass-loss rate of roughly 10(-4) M-circle dot yr(-1)) added to the light curve of a normal SN II-P. The underlying plateau requires a progenitor with an extended hydrogen envelope like a red supergiant at the moment of explosion, consistent with the slow wind speed (<80 km s(-1)) inferred from narrow H alpha emission. The cool supergiant progenitor is significant because PTF11iqb showed WR features in its early spectrum - meaning that the presence of such WR features does not necessarily indicate a WR-like progenitor. Overall, PTF11iqb bridges SNe IIn with weaker pre-SN mass-loss seen in SNe II-L and II-P, implying a continuum between these types.
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