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SN 2013ai: A Link between Hydrogen-rich and Hydrogen-poor Core-collapse Supernovae

SN 2013ai: A Link between Hydrogen-rich and Hydrogen-poor Core-collapse Supernovae
SN 2013ai: A Link between Hydrogen-rich and Hydrogen-poor Core-collapse Supernovae
We present a study of the optical and near-infrared (NIR) spectra of SN 2013ai along with its light curves. These data range from discovery until 380 days after explosion. SN 2013ai is a fast declining Type II supernova (SN II) with an unusually long rise time, 18.9 ± 2.7 days in the V-band, and a bright V-band peak absolute magnitude of -18.7 ± 0.06 mag. The spectra are dominated by hydrogen features in the optical and NIR. The spectral features of SN 2013ai are unique in their expansion velocities, which, when compared to large samples of SNe II, are more than 1,000 km s-1 faster at 50 days past explosion. In addition, the long rise time of the light curve more closely resembles SNe IIb rather than SNe II. If SN 2013ai is coeval with a nearby compact cluster, we infer a progenitor zero-age main-sequence mass of ∼17 M⊙. After performing light-curve modeling, we find that SN 2013ai could be the result of the explosion of a star with little hydrogen mass, a large amount of synthesized 56Ni, 0.3-0.4 M⊙, and an explosion energy of 2.5-3.0 × 1051 erg. The density structure and expansion velocities of SN 2013ai are similar to those of the prototypical SN IIb, SN 1993J. However, SN 2013ai shows no strong helium features in the optical, likely due to the presence of a dense core that prevents the majority of γ-rays from escaping to excite helium. Our analysis suggests that SN 2013ai could be a link between SNe II and stripped-envelope SNe.
Core-collapse supernovae, Type II supernovae, Late stellar evolution, 304, 1731, 911
0004-637X
145
Pessi, P. J.
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Fraser, M.
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Ertini, K.
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Martinez, L.
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Hoeflich, P.
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Hsiao, E. Y.
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Folatelli, G.
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Ashall, C.
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Bersten, M.
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Englert, B.
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Benetti, S.
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Bunzel, A.
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Contreras, C.
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Elias-Rosa, N.
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Falco, E.
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Galbany, L.
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Kirshner, R. P.
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Lyman, J. D.
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Marion, G. H.
e00f4507-089f-43e6-b791-6bce3cac57fc
Mattila, S.
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Maund, J.
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Morrell, N.
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Serón, J.
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Stritzinger, M.
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Shahbandeh, M.
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Sullivan, M.
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Suntzeff, N. B.
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Pessi, P. J.
7865aa7b-1065-403e-84c0-243c5b0e5888
Fraser, M.
525afe70-c2ed-49e4-b46d-3fe44dd2de68
Ertini, K.
96ae688d-eed9-4457-b5a2-f0c47f419cf6
Martinez, L.
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Hoeflich, P.
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Hsiao, E. Y.
39b3f954-767b-4652-b436-6d59716dd348
Folatelli, G.
5780b2cf-ab97-4b6f-8c52-78019a77009b
Ashall, C.
01b8c4e1-a4d5-4509-a0b7-e77a1b9d721b
Bersten, M.
390ca848-c9a7-402b-80a9-06508d4431fb
Englert, B.
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Benetti, S.
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Bunzel, A.
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Contreras, C.
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Elias-Rosa, N.
e2b41fee-d211-459d-a991-0234d77296cf
Falco, E.
f38f4792-a192-4ad9-afc8-73b5261c7f74
Galbany, L.
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Kirshner, R. P.
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Lyman, J. D.
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Marion, G. H.
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Mattila, S.
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Maund, J.
7f0be564-fe90-4fe8-bdb5-d57ff3a83139
Morrell, N.
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Serón, J.
349784b7-3169-4ebd-a4c9-27f98bb82311
Stritzinger, M.
403de4a3-a146-4e92-88bd-06e04d917bd5
Shahbandeh, M.
daa338f7-f826-485a-8e99-4e94ecf0d220
Sullivan, M.
2f31f9fa-8e79-4b35-98e2-0cb38f503850
Suntzeff, N. B.
99635c46-d717-4204-86cc-5153237cbb37

Pessi, P. J., Fraser, M., Ertini, K., Martinez, L., Hoeflich, P., Hsiao, E. Y., Folatelli, G., Ashall, C., Bersten, M., Englert, B., Benetti, S., Bunzel, A., Contreras, C., Elias-Rosa, N., Falco, E., Galbany, L., Kirshner, R. P., Lyman, J. D., Marion, G. H., Mattila, S., Maund, J., Morrell, N., Serón, J., Stritzinger, M., Shahbandeh, M., Sullivan, M. and Suntzeff, N. B. (2021) SN 2013ai: A Link between Hydrogen-rich and Hydrogen-poor Core-collapse Supernovae. The Astrophysical Journal, 909 (2), 145. (doi:10.3847/1538-4357/abdd36).

Record type: Article

Abstract

We present a study of the optical and near-infrared (NIR) spectra of SN 2013ai along with its light curves. These data range from discovery until 380 days after explosion. SN 2013ai is a fast declining Type II supernova (SN II) with an unusually long rise time, 18.9 ± 2.7 days in the V-band, and a bright V-band peak absolute magnitude of -18.7 ± 0.06 mag. The spectra are dominated by hydrogen features in the optical and NIR. The spectral features of SN 2013ai are unique in their expansion velocities, which, when compared to large samples of SNe II, are more than 1,000 km s-1 faster at 50 days past explosion. In addition, the long rise time of the light curve more closely resembles SNe IIb rather than SNe II. If SN 2013ai is coeval with a nearby compact cluster, we infer a progenitor zero-age main-sequence mass of ∼17 M⊙. After performing light-curve modeling, we find that SN 2013ai could be the result of the explosion of a star with little hydrogen mass, a large amount of synthesized 56Ni, 0.3-0.4 M⊙, and an explosion energy of 2.5-3.0 × 1051 erg. The density structure and expansion velocities of SN 2013ai are similar to those of the prototypical SN IIb, SN 1993J. However, SN 2013ai shows no strong helium features in the optical, likely due to the presence of a dense core that prevents the majority of γ-rays from escaping to excite helium. Our analysis suggests that SN 2013ai could be a link between SNe II and stripped-envelope SNe.

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Accepted/In Press date: 14 January 2021
Published date: 12 March 2021
Keywords: Core-collapse supernovae, Type II supernovae, Late stellar evolution, 304, 1731, 911

Identifiers

Local EPrints ID: 468345
URI: http://eprints.soton.ac.uk/id/eprint/468345
ISSN: 0004-637X
PURE UUID: 37cfe5d3-6a82-41bb-b547-ba56e6c51a6d
ORCID for M. Sullivan: ORCID iD orcid.org/0000-0001-9053-4820

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Date deposited: 10 Aug 2022 18:15
Last modified: 17 Mar 2024 03:30

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Contributors

Author: P. J. Pessi
Author: M. Fraser
Author: K. Ertini
Author: L. Martinez
Author: P. Hoeflich
Author: E. Y. Hsiao
Author: G. Folatelli
Author: C. Ashall
Author: M. Bersten
Author: B. Englert
Author: S. Benetti
Author: A. Bunzel
Author: C. Contreras
Author: N. Elias-Rosa
Author: E. Falco
Author: L. Galbany
Author: R. P. Kirshner
Author: J. D. Lyman
Author: G. H. Marion
Author: S. Mattila
Author: J. Maund
Author: N. Morrell
Author: J. Serón
Author: M. Stritzinger
Author: M. Shahbandeh
Author: M. Sullivan ORCID iD
Author: N. B. Suntzeff

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