Strong near-infrared carbon in the Type Ia supernova iPTF13ebh

E. Y. Hsiao; C. R. Burns; C. Contreras; P. Höflich; D. Sand; G. H. Marion; M. M. Phillips; M. Stritzinger; S. González-Gaitán; R. E. Mason; G. Folatelli; E. Parent; C. Gall; R. Amanullah; G. C. Anupama; I. Arcavi; D. P.K. Banerjee; Y. Beletsky; G. A. Blanc; J. S. Bloom; P. J. Brown; A. Campillay; Y. Cao; A. De Cia; T. Diamond; W. L. Freedman; C. Gonzalez; A. Goobar; S. Holmbo; D. A. Howell; J. Johansson; M. M. Kasliwal; R. P. Kirshner; K. Krisciunas; S. R. Kulkarni; K. Maguire; P. A. Milne; N. Morrell; P. E. Nugent; E. O. Ofek; D. Osip; P. Palunas; D. A. Perley; S. E. Persson; A. L. Piro; M. Rabus; M. Roth; J. M. Schiefelbein; S. Srivastav; M. Sullivan; N. B. Suntzeff; J. Surace; P. R. Woźniak; O. Yaron

doi:10.1051/0004-6361/201425297

Strong near-infrared carbon in the Type Ia supernova iPTF13ebh

E. Y. Hsiao, C. R. Burns, C. Contreras, P. Höflich, D. Sand, G. H. Marion, M. M. Phillips, M. Stritzinger, S. González-Gaitán, R. E. Mason, G. Folatelli, E. Parent, C. Gall, R. Amanullah, G. C. Anupama, I. Arcavi, D. P.K. Banerjee, Y. Beletsky, G. A. Blanc, J. S. BloomP. J. Brown, A. Campillay, Y. Cao, A. De Cia, T. Diamond, W. L. Freedman, C. Gonzalez, A. Goobar, S. Holmbo, D. A. Howell, J. Johansson, M. M. Kasliwal, R. P. Kirshner, K. Krisciunas, S. R. Kulkarni, K. Maguire, P. A. Milne, N. Morrell, P. E. Nugent, E. O. Ofek, D. Osip, P. Palunas, D. A. Perley, S. E. Persson, A. L. Piro, M. Rabus, M. Roth, J. M. Schiefelbein, S. Srivastav, M. Sullivan, N. B. Suntzeff, J. Surace, P. R. Woźniak, O. Yaron

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Abstract

We present near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2.3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR C i lines, and the C iλ1.0693 μm line is the strongest ever observed in a SN Ia. Interestingly, no strong optical C ii counterparts were found, even though the optical spectroscopic time series began early and is densely cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR C i compared to the weaker optical C ii appears to be general in SNe Ia. iPTF13ebh is a fast decliner with Δm₁₅(B) = 1.79 ± 0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a "transitional" event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest that composition and density of the inner core are similar to that of 91bg-like events, and that it has a deep-reaching carbon burning layer that is not observed in more slowly declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the Si iiλ0.6355 μm line, implying a long dark phase of ∼4 days.

Original language	English
Article number	A9
Journal	Astronomy and Astrophysics
Volume	578
DOIs	https://doi.org/10.1051/0004-6361/201425297
State	Published - 1 Jun 2015
Externally published	Yes

Funding

Funders	Funder number
Australian Research Council
Comisión Nacional de Investigación Científica y Tecnológica
Danish Agency for Science and Higher Education
Danmarks Grundforskningsfond
U.S. Department of Energy
National Research Council
Ministerio de Ciencia, Tecnología e Innovación Productiva
Ministério da Ciência, Tecnologia e Inovação
Laboratory Directed Research and Development
National Science Foundation	1008343, 1009987, 1313484
Office of Science	DE-AC02-05CH11231
Ministerio de Economía, Fomento y Turismo, Chile	IC12009
Fondo Nacional de Desarrollo Científico y Tecnológico	3130680

Keywords

Infrared: general
Supernovae: general
Supernovae: individual: iPTF13ebh

Access to Document

10.1051/0004-6361/201425297

Cite this

Hsiao, E. Y., Burns, C. R., Contreras, C., Höflich, P., Sand, D., Marion, G. H., Phillips, M. M., Stritzinger, M., González-Gaitán, S., Mason, R. E., Folatelli, G., Parent, E., Gall, C., Amanullah, R., Anupama, G. C., Arcavi, I., Banerjee, D. P. K., Beletsky, Y., Blanc, G. A., ... Yaron, O. (2015). Strong near-infrared carbon in the Type Ia supernova iPTF13ebh. Astronomy and Astrophysics, 578, Article A9. https://doi.org/10.1051/0004-6361/201425297

@article{2dbd9ca6067343dbbdb7d673dba552b2,

title = "Strong near-infrared carbon in the Type Ia supernova iPTF13ebh",

abstract = "We present near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2.3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR C i lines, and the C iλ1.0693 μm line is the strongest ever observed in a SN Ia. Interestingly, no strong optical C ii counterparts were found, even though the optical spectroscopic time series began early and is densely cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR C i compared to the weaker optical C ii appears to be general in SNe Ia. iPTF13ebh is a fast decliner with Δm15(B) = 1.79 ± 0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a {"}transitional{"} event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest that composition and density of the inner core are similar to that of 91bg-like events, and that it has a deep-reaching carbon burning layer that is not observed in more slowly declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the Si iiλ0.6355 μm line, implying a long dark phase of ∼4 days.",

keywords = "Infrared: general, Supernovae: general, Supernovae: individual: iPTF13ebh",

author = "Hsiao, {E. Y.} and Burns, {C. R.} and C. Contreras and P. H{\"o}flich and D. Sand and Marion, {G. H.} and Phillips, {M. M.} and M. Stritzinger and S. Gonz{\'a}lez-Gait{\'a}n and Mason, {R. E.} and G. Folatelli and E. Parent and C. Gall and R. Amanullah and Anupama, {G. C.} and I. Arcavi and Banerjee, {D. P.K.} and Y. Beletsky and Blanc, {G. A.} and Bloom, {J. S.} and Brown, {P. J.} and A. Campillay and Y. Cao and {De Cia}, A. and T. Diamond and Freedman, {W. L.} and C. Gonzalez and A. Goobar and S. Holmbo and Howell, {D. A.} and J. Johansson and Kasliwal, {M. M.} and Kirshner, {R. P.} and K. Krisciunas and Kulkarni, {S. R.} and K. Maguire and Milne, {P. A.} and N. Morrell and Nugent, {P. E.} and Ofek, {E. O.} and D. Osip and P. Palunas and Perley, {D. A.} and Persson, {S. E.} and Piro, {A. L.} and M. Rabus and M. Roth and Schiefelbein, {J. M.} and S. Srivastav and M. Sullivan and Suntzeff, {N. B.} and J. Surace and Wo{\'z}niak, {P. R.} and O. Yaron",

note = "Publisher Copyright: {\textcopyright} 2015 ESO.",

year = "2015",

month = jun,

day = "1",

doi = "10.1051/0004-6361/201425297",

language = "אנגלית",

volume = "578",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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Hsiao, EY, Burns, CR, Contreras, C, Höflich, P, Sand, D, Marion, GH, Phillips, MM, Stritzinger, M, González-Gaitán, S, Mason, RE, Folatelli, G, Parent, E, Gall, C, Amanullah, R, Anupama, GC, Arcavi, I, Banerjee, DPK, Beletsky, Y, Blanc, GA, Bloom, JS, Brown, PJ, Campillay, A, Cao, Y, De Cia, A, Diamond, T, Freedman, WL, Gonzalez, C, Goobar, A, Holmbo, S, Howell, DA, Johansson, J, Kasliwal, MM, Kirshner, RP, Krisciunas, K, Kulkarni, SR, Maguire, K, Milne, PA, Morrell, N, Nugent, PE, Ofek, EO, Osip, D, Palunas, P, Perley, DA, Persson, SE, Piro, AL, Rabus, M, Roth, M, Schiefelbein, JM, Srivastav, S, Sullivan, M, Suntzeff, NB, Surace, J, Woźniak, PR & Yaron, O 2015, 'Strong near-infrared carbon in the Type Ia supernova iPTF13ebh', Astronomy and Astrophysics, vol. 578, A9. https://doi.org/10.1051/0004-6361/201425297

TY - JOUR

T1 - Strong near-infrared carbon in the Type Ia supernova iPTF13ebh

AU - Hsiao, E. Y.

AU - Burns, C. R.

AU - Contreras, C.

AU - Höflich, P.

AU - Sand, D.

AU - Marion, G. H.

AU - Phillips, M. M.

AU - Stritzinger, M.

AU - González-Gaitán, S.

AU - Mason, R. E.

AU - Folatelli, G.

AU - Parent, E.

AU - Gall, C.

AU - Amanullah, R.

AU - Anupama, G. C.

AU - Arcavi, I.

AU - Banerjee, D. P.K.

AU - Beletsky, Y.

AU - Blanc, G. A.

AU - Bloom, J. S.

AU - Brown, P. J.

AU - Campillay, A.

AU - Cao, Y.

AU - De Cia, A.

AU - Diamond, T.

AU - Freedman, W. L.

AU - Gonzalez, C.

AU - Goobar, A.

AU - Holmbo, S.

AU - Howell, D. A.

AU - Johansson, J.

AU - Kasliwal, M. M.

AU - Kirshner, R. P.

AU - Krisciunas, K.

AU - Kulkarni, S. R.

AU - Maguire, K.

AU - Milne, P. A.

AU - Morrell, N.

AU - Nugent, P. E.

AU - Ofek, E. O.

AU - Osip, D.

AU - Palunas, P.

AU - Perley, D. A.

AU - Persson, S. E.

AU - Piro, A. L.

AU - Rabus, M.

AU - Roth, M.

AU - Schiefelbein, J. M.

AU - Srivastav, S.

AU - Sullivan, M.

AU - Suntzeff, N. B.

AU - Surace, J.

AU - Woźniak, P. R.

AU - Yaron, O.

PY - 2015/6/1

Y1 - 2015/6/1

N2 - We present near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2.3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR C i lines, and the C iλ1.0693 μm line is the strongest ever observed in a SN Ia. Interestingly, no strong optical C ii counterparts were found, even though the optical spectroscopic time series began early and is densely cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR C i compared to the weaker optical C ii appears to be general in SNe Ia. iPTF13ebh is a fast decliner with Δm15(B) = 1.79 ± 0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a "transitional" event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest that composition and density of the inner core are similar to that of 91bg-like events, and that it has a deep-reaching carbon burning layer that is not observed in more slowly declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the Si iiλ0.6355 μm line, implying a long dark phase of ∼4 days.

AB - We present near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2.3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR C i lines, and the C iλ1.0693 μm line is the strongest ever observed in a SN Ia. Interestingly, no strong optical C ii counterparts were found, even though the optical spectroscopic time series began early and is densely cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR C i compared to the weaker optical C ii appears to be general in SNe Ia. iPTF13ebh is a fast decliner with Δm15(B) = 1.79 ± 0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a "transitional" event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest that composition and density of the inner core are similar to that of 91bg-like events, and that it has a deep-reaching carbon burning layer that is not observed in more slowly declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the Si iiλ0.6355 μm line, implying a long dark phase of ∼4 days.

KW - Infrared: general

KW - Supernovae: general

KW - Supernovae: individual: iPTF13ebh

UR - http://www.scopus.com/inward/record.url?scp=84930505473&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201425297

DO - 10.1051/0004-6361/201425297

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AN - SCOPUS:84930505473

SN - 0004-6361

VL - 578

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A9

ER -

Strong near-infrared carbon in the Type Ia supernova iPTF13ebh

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