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450 d of Type II SN 2013ej in optical and near-infrared

Yuan, Fang and Jerkstrand, A. and Valenti, S. and Sollerman, J. and Seitenzahl, I. R. and Pastorello, A. and Schulze, S. and Chen, T.-W. and Childress, M. J. and Fraser, M. and Fremling, C. and Kotak, R. and Ruiter, A. J. and Schmidt, B. P. and Smartt, S. J. and Taddia, F. and Terreran, G. and Tucker, B. E. and Barbarino, C. and Benetti, S. and Elias-Rosa, N. and Gal-Yam, A. and Howell, D. A. and Inserra, C. and Kankare, E. and Lee, M. Y. and Li, K. L. and Maguire, K. and Margheim, S. and Mehner, A. and Ochner, P. and Sullivan, M. and Tomasella, L. and Young, D. R. (2016) 450 d of Type II SN 2013ej in optical and near-infrared. Monthly Notices of the Royal Astronomical Society, 461 (2). pp. 2003-2018. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20190529-082821644

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Abstract

We present optical and near-infrared photometric and spectroscopic observations of SN 2013ej, in galaxy M74, from 1 to 450 d after the explosion. SN 2013ej is a hydrogen-rich supernova, classified as a Type IIL due to its relatively fast decline following the initial peak. It has a relatively high peak luminosity (absolute magnitude MV = −17.6) but a small ^(56)Ni production of ∼0.023 M⊙. Its photospheric evolution is similar to other Type II SNe, with shallow absorption in the H_α profile typical for a Type IIL. During transition to the radioactive decay tail at ∼100 d, we find the SN to grow bluer in B − V colour, in contrast to some other Type II supernovae. At late times, the bolometric light curve declined faster than expected from ^(56)Co decay and we observed unusually broad and asymmetric nebular emission lines. Based on comparison of nebular emission lines most sensitive to the progenitor core mass, we find our observations are best matched to synthesized spectral models with a M_(ZAMS) = 12–15 M⊙progenitor. The derived mass range is similar to but not higher than the mass estimated for Type IIP progenitors. This is against the idea that Type IIL are from more massive stars. Observations are consistent with the SN having a progenitor with a relatively low-mass envelope.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stw1419DOIArticle
ORCID:
AuthorORCID
Valenti, S.0000-0001-8818-0795
Sollerman, J.0000-0003-1546-6615
Schulze, S.0000-0001-6797-1889
Chen, T.-W.0000-0002-1066-6098
Fremling, C.0000-0002-4223-103X
Kotak, R.0000-0001-5455-3653
Schmidt, B. P.0000-0001-6589-1287
Smartt, S. J.0000-0002-8229-1731
Taddia, F.0000-0002-2387-6801
Barbarino, C.0000-0002-3821-6144
Benetti, S.0000-0002-3256-0016
Elias-Rosa, N.0000-0002-1381-9125
Gal-Yam, A.0000-0002-3653-5598
Howell, D. A.0000-0003-4253-656X
Inserra, C.0000-0002-3968-4409
Kankare, E.0000-0001-8257-3512
Li, K. L.0000-0001-8229-2024
Maguire, K.0000-0002-9770-3508
Mehner, A.0000-0002-9564-3302
Sullivan, M.0000-0001-9053-4820
Additional Information:© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 June 10. Received 2016 June 10; in original form 2016 April 18. Published: 15 June 2016. The authors would like to thank Melissa Graham for scheduling the LCOGT observations. This paper is based on observations collected at the European Organization for Astronomical Research in the Southern hemisphere, Chile as part of PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects Survey) ESO programme ID 188.D-3003. The paper is partially based on observations collected at Copernico and Schmidt telescopes (Asiago, Italy) of the INAF – Osservatorio Astronomico di Padova. Some observations have been obtained also with the 1.22 m telescope + B&C spectrograph operated in Asiago by the Department of Physics and Astronomy of the University of Padova. This paper is partly based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil). This research was made possible through the use of the APASS, funded by the Robert Martin Ayers Sciences Fund. 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. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. IRS was supported by the ARC Laureate Grant FL0992131. SB, AP, NER and GT are partially supported by the PRIN-INAF 2014 project ‘Transient Universe: unveiling new types of stellar explosions with PESSTO’. SSchulze acknowledges support from CONICYT-Chile FONDECYT 3140534, Basal-CATA PFB-06/2007, and Project IC120009 ‘Millennium Institute of Astrophysics (MAS)’ of Initiative Científica Milenio del Ministerio de Economía, Fomento y Turismo. This work was partly supported by the European Union FP7 programme through ERC grant number 320360. KM acknowledges support from the STFC through an Ernest Rutherford Fellowship. MS acknowledges support from STFC grant ST/L000679/1 and EU/FP7-ERC grant no. [615929]. AGY is supported by the EU/FP7 via ERC grant no. 307260, the Quantum Universe I- CORE Program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF); by Minerva and ISF grants; by the Weizmann-UK making connections programme; and by Kimmel and ARCHES awards.
Group:Palomar Transient Factory
Funders:
Funding AgencyGrant Number
Robert Martin Ayers Sciences FundUNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Australian Research CouncilCE110001020
Australian Research CouncilFL0992131
Istituto Nazionale di Astrofisica (INAF)PRIN-INAF 2014
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)3140534
Basal-CATAPFB-06/2007
Iniciativa Científica Milenio del Ministerio de Economía, Fomento y TurismoIC120009
European Research Council (ERC)320360
Science and Technology Facilities Council (STFC)ST/L000679/1
European Research Council (ERC)615929
European Research Council (ERC)307260
I-CORE Program of the Planning and Budgeting CommitteeUNSPECIFIED
Israel Science FoundationUNSPECIFIED
MinervaUNSPECIFIED
Weizmann-UKUNSPECIFIED
Kimmel AwardUNSPECIFIED
ARCHES AwardUNSPECIFIED
Subject Keywords:supernovae: general, supernovae: individual: SN 2013ej
Issue or Number:2
Record Number:CaltechAUTHORS:20190529-082821644
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190529-082821644
Official Citation:Fang Yuan, A. Jerkstrand, S. Valenti, J. Sollerman, I. R. Seitenzahl, A. Pastorello, S. Schulze, T.-W. Chen, M. J. Childress, M. Fraser, C. Fremling, R. Kotak, A. J. Ruiter, B. P. Schmidt, S. J. Smartt, F. Taddia, G. Terreran, B. E. Tucker, C. Barbarino, S. Benetti, N. Elias-Rosa, A. Gal-Yam, D. A. Howell, C. Inserra, E. Kankare, M. Y. Lee, K. L. Li, K. Maguire, S. Margheim, A. Mehner, P. Ochner, M. Sullivan, L. Tomasella, D. R. Young, 450 d of Type II SN 2013ej in optical and near-infrared, Monthly Notices of the Royal Astronomical Society, Volume 461, Issue 2, 11 September 2016, Pages 2003–2018, https://doi.org/10.1093/mnras/stw1419
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:95844
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:30 May 2019 21:19
Last Modified:09 Mar 2020 13:18

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