Strong near-infrared carbon in the Type Ia supernova iPTF13ebh

EY Hsiao; CR Burns; C Contreras; P Hoflich; D Sand; GH Marion; MM Phillips; M Stritzinger; S Gonzalez-Gaitan; RE Mason; G Folatelli; E Parent; C Gall; R Amanullah; GC Anupama; Iair Arcavi; DPK Banerjee; Y Beletsky; GA Blanc; JS Bloom; PJ Brown; A Campillay; Y Cao; Cia, Annalisa De Cia; T Diamond; WL Freedman; C Gonzalez; A Goobar; S Holmbo; DA Howell; J Johansson; MM Kasliwal; RP Kirshner; K Krisciunas; SR Kulkarni; K Maguire; PA Milne; N Morrell; PE Nugent; EO Ofek; D Osip; P Palunas; DA Perley; SE Persson; AL Piro; M Rabus; M Roth; JM Schiefelbein; S Srivastav; M Sullivan; NB Suntzeff; J Surace; PR Wozniak; Ofer Yaron; P. Höflich; P. R. Woźniak

doi:https://doi.org/10.1051/0004-6361/201425297

Strong near-infrared carbon in the Type Ia supernova iPTF13ebh

EY Hsiao, CR Burns, C Contreras, P Hoflich, D Sand, GH Marion, MM Phillips, M Stritzinger, S Gonzalez-Gaitan, RE Mason, G Folatelli, E Parent, C Gall, R Amanullah, GC Anupama, Iair Arcavi, DPK Banerjee, Y Beletsky, GA Blanc, JS BloomPJ Brown, A Campillay, Y Cao, Cia, Annalisa De Cia, T Diamond, WL Freedman, C Gonzalez, A Goobar, S Holmbo, DA Howell, J Johansson, MM Kasliwal, RP Kirshner, K Krisciunas, SR Kulkarni, K Maguire, PA Milne, N Morrell, PE Nugent, EO Ofek, D Osip, P Palunas, DA Perley, SE Persson, AL Piro, M Rabus, M Roth, JM Schiefelbein, S Srivastav, M Sullivan, NB Suntzeff, J Surace, PR Wozniak, Ofer Yaron, P. Höflich, P. R. Woźniak

Department of Particle Physics and Astrophysics

Weizmann Institute of Science

Research output: Contribution to journal › Article › peer-review

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 & Astrophysics
Volume	578
DOIs	https://doi.org/10.1051/0004-6361/201425297
State	Published - 1 Jun 2015

Keywords

Infrared: general
Supernovae: general
Supernovae: individual: iPTF13ebh

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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https://doi.org/10.1051/0004-6361/201425297

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Hsiao, EY., Burns, CR., Contreras, C., Hoflich, P., Sand, D., Marion, GH., Phillips, MM., Stritzinger, M., Gonzalez-Gaitan, S., Mason, RE., Folatelli, G., Parent, E., Gall, C., Amanullah, R., Anupama, GC., Arcavi, I., Banerjee, DPK., Beletsky, Y., Blanc, GA., ... Woźniak, P. R. (2015). Strong near-infrared carbon in the Type Ia supernova iPTF13ebh. Astronomy & Astrophysics, 578, Article A9. https://doi.org/10.1051/0004-6361/201425297

@article{c7f31345e76e44c1aed46c3af38f6caa,

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 = "EY Hsiao and CR Burns and C Contreras and P Hoflich and D Sand and GH Marion and MM Phillips and M Stritzinger and S Gonzalez-Gaitan and RE Mason and G Folatelli and E Parent and C Gall and R Amanullah and GC Anupama and Iair Arcavi and DPK Banerjee and Y Beletsky and GA Blanc and JS Bloom and PJ Brown and A Campillay and Y Cao and {De Cia}, {Cia, Annalisa} and T Diamond and WL Freedman and C Gonzalez and A Goobar and S Holmbo and DA Howell and J Johansson and MM Kasliwal and RP Kirshner and K Krisciunas and SR Kulkarni and K Maguire and PA Milne and N Morrell and PE Nugent and EO Ofek and D Osip and P Palunas and DA Perley and SE Persson and AL Piro and M Rabus and M Roth and JM Schiefelbein and S Srivastav and M Sullivan and NB Suntzeff and J Surace and PR Wozniak and Ofer Yaron and P. H{\"o}flich and Wo{\'z}niak, {P. R.}",

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

year = "2015",

month = jun,

day = "1",

doi = "https://doi.org/10.1051/0004-6361/201425297",

language = "الإنجليزيّة",

volume = "578",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Hsiao, EY, Burns, CR, Contreras, C, Hoflich, P, Sand, D, Marion, GH, Phillips, MM, Stritzinger, M, Gonzalez-Gaitan, 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, CA, 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, Wozniak, PR, Yaron, O, Höflich, P & Woźniak, PR 2015, 'Strong near-infrared carbon in the Type Ia supernova iPTF13ebh', Astronomy & 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, EY

AU - Burns, CR

AU - Contreras, C

AU - Hoflich, P

AU - Sand, D

AU - Marion, GH

AU - Phillips, MM

AU - Stritzinger, M

AU - Gonzalez-Gaitan, S

AU - Mason, RE

AU - Folatelli, G

AU - Parent, E

AU - Gall, C

AU - Amanullah, R

AU - Anupama, GC

AU - Arcavi, Iair

AU - Banerjee, DPK

AU - Beletsky, Y

AU - Blanc, GA

AU - Bloom, JS

AU - Brown, PJ

AU - Campillay, A

AU - Cao, Y

AU - De Cia, Cia, Annalisa

AU - Diamond, T

AU - Freedman, WL

AU - Gonzalez, C

AU - Goobar, A

AU - Holmbo, S

AU - Howell, DA

AU - Johansson, J

AU - Kasliwal, MM

AU - Kirshner, RP

AU - Krisciunas, K

AU - Kulkarni, SR

AU - Maguire, K

AU - Milne, PA

AU - Morrell, N

AU - Nugent, PE

AU - Ofek, EO

AU - Osip, D

AU - Palunas, P

AU - Perley, DA

AU - Persson, SE

AU - Piro, AL

AU - Rabus, M

AU - Roth, M

AU - Schiefelbein, JM

AU - Srivastav, S

AU - Sullivan, M

AU - Suntzeff, NB

AU - Surace, J

AU - Wozniak, PR

AU - Yaron, Ofer

AU - Höflich, P.

AU - Woźniak, P. R.

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 - https://doi.org/10.1051/0004-6361/201425297

DO - https://doi.org/10.1051/0004-6361/201425297

M3 - مقالة

SN - 0004-6361

VL - 578

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A9

ER -

Strong near-infrared carbon in the Type Ia supernova iPTF13ebh

Abstract

Keywords

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