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

450 d of Type II SN 2013ej in optical and near-infrared
450 d of Type II SN 2013ej in optical and near-infrared
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 56Ni production of ?0.023 M?. Its photospheric evolution is similar to other Type II SNe, with shallow absorption in the H? 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 56Co 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 MZAMS = 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
0035-8711
2003-2018
Yuan, Fang
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Jerkstrand, A.
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Valenti, S.
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Sollerman, J.
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Seitenzahl, I.R.
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Pastorello, A.
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Schulze, S.
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Chen, T.-W.
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Childress, Michael
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Fraser, M.
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Fremling, C.
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Kotak, R.
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Ruiter, A.J.
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Schmidt, B.P.
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Smartt, S.J.
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Taddia, F.
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Terreran, G.
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Tucker, B.E.
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Barbarino, C.
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Benetti, S.
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Elias-Rosa, N.
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Gal-Yam, A.
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Howell, D.A.
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Inserra, C.
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Kankare, E.
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Lee, M.Y.
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Li, K.L.
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Maguire, K.
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Margheim, S.
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Mehner, A.
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Ochner, P.
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Sullivan, Mark
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Tomasella, L.
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Young, D.R.
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Yuan, Fang
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Jerkstrand, A.
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Valenti, S.
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Sollerman, J.
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Seitenzahl, I.R.
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Pastorello, A.
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Schulze, S.
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Chen, T.-W.
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Childress, Michael
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Fraser, M.
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Fremling, C.
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Kotak, R.
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Ruiter, A.J.
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Schmidt, B.P.
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Smartt, S.J.
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Taddia, F.
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Terreran, G.
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Tucker, B.E.
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Barbarino, C.
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Benetti, S.
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Elias-Rosa, N.
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Gal-Yam, A.
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Howell, D.A.
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Inserra, C.
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Kankare, E.
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Lee, M.Y.
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Li, K.L.
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Maguire, K.
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Margheim, S.
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Mehner, A.
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Ochner, P.
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Sullivan, Mark
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Tomasella, L.
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Young, D.R.
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Yuan, Fang, Jerkstrand, A., Valenti, S., Sollerman, J., Seitenzahl, I.R., Pastorello, A., Schulze, S., Chen, T.-W., Childress, Michael, Fraser, M., Fremling, C., Kotak, R., Ruiter, A.J., Schmidt, B.P., Smartt, S.J., Taddia, F., Terreran, G., Tucker, B.E., Barbarino, C., Benetti, S., Elias-Rosa, N., Gal-Yam, A., Howell, D.A., Inserra, C., Kankare, E., Lee, M.Y., Li, K.L., Maguire, K., Margheim, S., Mehner, A., Ochner, P., Sullivan, Mark, 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), 2003-2018. (doi:10.1093/mnras/stw1419).

Record type: Article

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 56Ni production of ?0.023 M?. Its photospheric evolution is similar to other Type II SNe, with shallow absorption in the H? 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 56Co 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 MZAMS = 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

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Accepted/In Press date: 10 June 2016
e-pub ahead of print date: 15 June 2016
Published date: 11 September 2016
Organisations: Quantum, Light & Matter Group

Identifiers

Local EPrints ID: 401417
URI: https://eprints.soton.ac.uk/id/eprint/401417
ISSN: 0035-8711
PURE UUID: d0a5023d-8189-4db6-baa2-c3735e65bff9
ORCID for Mark Sullivan: ORCID iD orcid.org/0000-0001-9053-4820

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Date deposited: 17 Oct 2016 12:10
Last modified: 06 Jun 2018 12:27

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Contributors

Author: Fang Yuan
Author: A. Jerkstrand
Author: S. Valenti
Author: J. Sollerman
Author: I.R. Seitenzahl
Author: A. Pastorello
Author: S. Schulze
Author: T.-W. Chen
Author: Michael Childress
Author: M. Fraser
Author: C. Fremling
Author: R. Kotak
Author: A.J. Ruiter
Author: B.P. Schmidt
Author: S.J. Smartt
Author: F. Taddia
Author: G. Terreran
Author: B.E. Tucker
Author: C. Barbarino
Author: S. Benetti
Author: N. Elias-Rosa
Author: A. Gal-Yam
Author: D.A. Howell
Author: C. Inserra
Author: E. Kankare
Author: M.Y. Lee
Author: K.L. Li
Author: K. Maguire
Author: S. Margheim
Author: A. Mehner
Author: P. Ochner
Author: Mark Sullivan ORCID iD
Author: L. Tomasella
Author: D.R. Young

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