@article{d43c06e114ec47199df090a421dbf332,
title = "SN 2010jp (PTF10aaxi): A jet in a Type II supernova",
abstract = "We present photometry and spectroscopy of the peculiar Type II supernova (SN) SN 2010jp, also named PTF10aaxi. The light curve exhibits a linear decline with a relatively low peak absolute magnitude of only -15.9 (unfiltered), and a low radioactive decay luminosity at late times, which suggests a low synthesized nickel mass of M ( 56 Ni) ≲ 0.003 M ⊙. Spectra of SN 2010jp display an unprecedented triple-peaked Hα line profile, showing (1) a narrow (full width at half-maximum >rsim800kms -1) central component that suggests shock interaction with dense circumstellar material (CSM); (2) high-velocity blue and red emission features centred at -12600 and +15400kms -1, respectively; and (3) very broad wings extending from -22000 to +25000kms -1. These features persist over multiple epochs during the \textasciitilde{}100 d after explosion. We propose that this line profile indicates a bipolar jet-driven explosion, with the central component produced by normal SN ejecta and CSM interaction at mid and low latitudes, while the high-velocity bumps and broad-line wings arise in a non-relativistic bipolar jet. Two variations of the jet interpretation seem plausible: (1) a fast jet mixes 56Ni to high velocities in polar zones of the H-rich envelope; or (2) the reverse shock in the jet produces blue and red bumps in Balmer lines when a jet interacts with dense CSM. Jet-driven Type II SNe are predicted for collapsars resulting from a wide range of initial masses above 25M ⊙, especially at subsolar metallicity. This seems consistent with the SN host environment, which is either an extremely low-luminosity dwarf galaxy or the very remote parts of an interacting pair of star-forming galaxies. It also seems consistent with the apparently low 56Ni mass that may accompany black hole formation. We speculate that the jet survives to produce observable signatures because the star's H envelope was very low mass, having been mostly stripped away by the previous eruptive mass-loss indicated by the Type IIn features in the spectrum.",
keywords = "Circumstellar matter, ISM: jets and outflows, Supernovae: general, Supernovae: individual: SN 2010jp",
author = "Nathan Smith and Cenko, \{S. Bradley\} and Nat Butler and Bloom, \{Joshua S.\} and Kasliwal, \{Mansi M.\} and Assaf Horesh and Kulkarni, \{Shrinivas R.\} and Law, \{Nicholas M.\} and Nugent, \{Peter E.\} and Ofek, \{Eran O.\} and Dovi Poznanski and Quimby, \{Robert M.\} and Branimir Sesar and Sagi Ben-Ami and Iair Arcavi and Avishay Gal-Yam and David Polishook and Dong Xu and Ofer Yaron and Frail, \{Dale A.\} and Mark Sullivan",
note = "Richard and Rhoda Goldman Fund; NASA/Swift [NNX10AI21G, GO-7100028]; TABASGO Foundation; NSF [AST-0908886]; NASA; Office of Science of the US Department of Energy [DE-AC02-05CH11231]; Israeli Science Foundation; Binational Science Foundation; FP7 Marie Curie IRG Fellowship; Benoziyo Center for Astrophysics; Lord Sieff of Brimpton Memorial Fund; National Science Foundation (NSF-CDI) [0941742]; W. M. Keck FoundationWe thank P. Challis and R. Kirshner for assistance with the MMT observations in 2010 November, and for providing the reduced spectrum from that night. SBC acknowledges generous financial assistance from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, NASA/Swift grants NNX10AI21G and GO-7100028, the TABASGO Foundation, and NSF grant AST-0908886. DP and EOO are supported by Einstein fellowships from NASA. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources and data storage for this project. The Weizmann-PTF partnership is supported in part by grants from the Israeli Science Foundation to AG. Collaborative Caltech-WIS work is supported by a grant from the Binational Science Foundation to AG and SRK. The work of AG is further supported by an FP7 Marie Curie IRG Fellowship and the Benoziyo Center for Astrophysics, and by the Lord Sieff of Brimpton Memorial Fund. JSB was partially supported by a grant from the National Science Foundation (NSF-CDI \# 0941742). Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has",
year = "2012",
month = feb,
doi = "10.1111/j.1365-2966.2011.20104.x",
language = "الإنجليزيّة",
volume = "420",
pages = "1135--1144",
journal = "MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "2",
}