Analysis of broad-lined Type Ic supernovae from the (intermediate) Palomar Transient Factory

Creators: Taddia, F.; Sollerman, J.; Fremling, C.; Barbarino, C.; Karamehmetoglu, E.; Arcavi, I.; Cenko, S. B.; Filippenko, A. V.; Gal-Yam, A.; Hiramatsu, D.; Hosseinzadeh, G.; Howell, D. A.; Kulkarni, S. R.; Laher, R.; Lunnan, R.; Masci, F.; Nugent, P. E.; Nyholm, A.; Perley, D. A.; Quimby, R.; Silverman, J. M.

Abstract

We study 34 Type Ic supernovae that have broad spectral features (SNe Ic-BL). This is the only SN type found in association with long-duration gamma-ray bursts (GRBs). We obtained our photometric data with the Palomar Transient Factory (PTF) and its continuation, the intermediate PTF (iPTF). This is the first large, homogeneous sample of SNe Ic-BL from an untargeted survey. Furthermore, given the high observational cadence of iPTF, most of these SNe Ic-BL were discovered soon after explosion. We present K-corrected Bgriz light curves of these SNe, obtained through photometry on template-subtracted images. We analyzed the shape of the r-band light curves, finding a correlation between the decline parameter Δm_(15) and the rise parameter Δm_(−10). We studied the SN colors and, based on g − r, we estimated the host-galaxy extinction for each event. Peak r-band absolute magnitudes have an average of −18.6 ± 0.5 mag. We fit each r-band light curve with that of SN 1998bw (scaled and stretched) to derive the explosion epochs. We computed the bolometric light curves using bolometric corrections, r-band data, and g − r colors. Expansion velocities from Fe II were obtained by fitting spectral templates of SNe Ic. Bolometric light curves and velocities at peak were fitted using the semianalytic Arnett model to estimate ejecta mass M_(ej), explosion energy E_K and ^(56)Ni mass M(^(56)Ni) for each SN. We find average values of M_(ej) = 4 ± 3 M⊙, EK = (7 ± 6)×10^(51) erg, and M(^(56)Ni)=0.31 ± 0.16 M⊙. The parameter distributions were compared to those presented in the literature and are overall in agreement with them. We also estimated the degree of ^(56)Ni mixing using scaling relations derived from hydrodynamical models and we find that all the SNe are strongly mixed. The derived explosion parameters imply that at least 21% of the progenitors of SNe Ic-BL are compatible with massive (> 28 M⊙), possibly single stars, whereas at least 64% might come from less massive stars in close binary systems.

Additional Information

© 2019 ESO. Article published by EDP Sciences. Received 15 October 2018; Accepted 12 November 2018; Published online 10 January 2019. The Oskar Klein Centre is funded by the Swedish Research Council. F.T. and J.S. gratefully acknowledge support from the Knut and Alice Wallenberg Foundation. D.A.H. and G.H. are supported by National Science Foundation (NSF) grant AST-1313484. A.V.F. is grateful for financial assistance from NSF grant AST-1211916, the TABASGO Foundation, the Christopher R. Redlich Fund, and the Miller Institute for Basic Research in Science (U.C. Berkeley). A.G.-Y. is supported by the EU via ERC grant No. 725161, the Quantum Universe I-Core program, the ISF, the BSF Transformative program and by a Kimmel award. The intermediate Palomar Transient Factory project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin, Milwaukee, the Oskar Klein Center, the Weizmann Institute of Science, the TANGO Program of the University System of Taiwan, and the Kavli Institute for the Physics and Mathematics of the Universe. LANL participation in iPTF is supported by the US Department of Energy as a part of the Laboratory Directed Research and Development program. We acknowledge contributions from the full PTF and iPTF collaborations that made it possible to discover and monitor the SE SNe analyzed in this work. This work was supported by the GROWTH project funded by NSF under grant AST-1545949. We thank the staff at the various observatories at which data were collected. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias. The data presented herein were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. This work is partly based on observations made with DOLoRes@TNG. Our results made use of the Discovery Channel Telescope (DCT) at Lowell Observatory. Lowell is a private, nonprofit institution dedicated to astrophysical research and public appreciation of astronomy, and it operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University, and Yale University. The upgrade of the DeVeny optical spectrograph has been funded by a generous grant from John and Ginger Giovale. This work makes use of the Las Cumbres Observatory network and the LCO Supernova Key Project. Research at Lick Observatory is partially supported by a generous gift from Google. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). 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 Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We thank Mark Sullivan for contributing spectral data obtained under his observing programs. We acknowledge the large number of observers and those responsible for data reduction who helped acquire the spectroscopic database over the years. Among others, these include S. Adams, C. Badenes, S. Ben-Ami, N. Blagorodnova, J. S. Bloom, J. Botyanszki, K. Burdge, Y. Cao, J. Choi, N. Chotard, K. I. Clubb, D. Cook, N. Cucchiara, A. De Cia, A. Drake, G. Duggan, M. Fraser, M. L. Graham, T. Hashimoto, A. Ho, I. Hook, A. Horesh, E. Hsiao, T. Hung, M. Kandrashoff, M. Kasliwal, E. Kirby, I. Kleiser, S. Knezevic, T. Kupfer, K. Maguire, T. Matheson, A. A. Miller, K. P. Mooley, E. Ofek, Y.-C. Pan, D. Polishook, D. Poznanski, V. Ravi, J. Rex, A. Rubin, B. Sesar, I. Shivvers, A. Sternberg, N. Suzuki, D. Tal, C. Theissen, J. van Roestel. P. Vreeswijk, E. Walker, A. Waszczak, D. Xu, O. Yaron, and B. Zackay. We also thank the staff at the observatories where data were obtained. We acknowledge Umaa Rebbapragada and her group for the work with the machine-learning algorithm that allowed iPTF to discover transients. We thank Maryam Modjaz for the productive discussion on the SN classification.

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