Optical observations of the luminous Type IIn Supernova 2010jl for over 900 d

Creators: Jencson, J. E.; Prieto, J. L.; Kochanek, C. S.; Shappee, B. J.; Stanek, K. Z.; Pogge, R. W.

Abstract

The luminous Type IIn Supernova (SN) 2010jl shows strong evidence for the interaction of the SN ejecta with dense circumstellar material (CSM). We present observations of SN 2010jl for t ∼ 900 d after its earliest detection, including a sequence of optical spectra ranging from t = 55 to 909 d. We also supplement our late time spectra and the photometric measurements in the literature with an additional epoch of new, late time BVRI photometry. Combining available photometric and spectroscopic data, we derive a semi-bolometric optical light curve and calculate a total radiated energy in the optical for SN 2010jl of ∼3.5 × 10^(50) erg, confirming the result of Fransson et al. We also examine the evolution of the Hα emission line profile in detail and find evidence for asymmetry in the profile for t ≳ 775 d that is not easily explained by any of the proposed scenarios for this fascinating event. Finally, we discuss the interpretations from the literature of the optical and near-infrared light curves, and propose that the most likely explanation of their evolution is the formation of new dust in the dense, pre-existing CSM wind after ∼300 d.

Additional Information

© 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2015 November 26. Received 2015 November 25; in original form 2015 May 5. First published online December 31, 2015. We thank the referee, Nathan Smith, for his helpful comments and suggestions. We would also like to thank Matthew Penny and Dale Mudd for their helpful discussion and assistance in data acquisition and analysis. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144469. BS is supported by NASA through the Hubble Fellowship grant HST-HF-51348.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Support for JLP is in part by FONDECYT through the grant 1151445 and by the Ministry of Economy, Development, and Tourisms Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. This work is based on observations obtained at the MDM Observatory, operated by Dartmouth College, Columbia University, Ohio State University, Ohio University, and the University of Michigan. OSMOS has been generously funded by the National Science Foundation (AST-0705170) and the Center for Cosmology and AstroParticle Physics at The Ohio State University. Based on observations obtained with the APO 3.5-metre telescope, which is owned and operated by the Astrophysical Research Consortium. The LBT is an international collaboration among institutions in the United States, Italy and Germany. LBT Corporation partners are: The Ohio State University, and The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota and University of Virginia; The University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University. This paper used data obtained with the MODS spectrographs built with funding from NSF grant AST-9987045 and the NSF Telescope System Instrumentation Program (TSIP), with additional funds from the Ohio Board of Regents and the Ohio State University Office of Research. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. This research has made use of the NASA/IPAC Extragalactic Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.

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Published - MNRAS-2016-Jencson-2622-35.pdf

Submitted - 1505.01186v2.pdf

Supplemental Material - table3.txt

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