Comprehensive observations of the bright and energetic Type Iax SN 2012Z: Interpretation as a Chandrasekhar mass white dwarf explosion ∗

M. D. Stritzinger, S. Valenti, P. Hoeflich, E. Baron, M. M. Phillips, F. Taddia, R. J. Foley, E. Y. Hsiao, S. W. Jha, C. McCully, V. Pandya, J. D. Simon, S. Benetti, P. J. Brown, C. R. Burns, A. Campillay, C. Contreras, F. Förster, S. Holmbo, G. H. MarionN. Morrell, G. Pignata

Resultado de la investigación: Article

10 Citas (Scopus)

Resumen

We present ultraviolet through near-infrared (NIR) broadband photometry, and visual-wavelength and NIR spectroscopy of the Type Iax supernova (SN) 2012Z. The data set consists of both early- and late-time observations, including the first late phase NIR spectrum obtained for a spectroscopically classified SN Iax. Simple model calculations of its bolometric light curve suggest SN 2012Z produced ∼0.3 M of 56Ni, ejected about a Chandrasekhar mass of material, and had an explosion energy of ∼1051 erg, making it one of the brightest (MB = -18.3 mag) and most energetic SN Iax yet observed. The late phase (+269d) NIRspectrum of SN 2012Z is found to broadly resemble similar epoch spectra of normal SNe Ia; however, like other SNe Iax, corresponding visual-wavelength spectra differ substantially from all supernova types. Constraints from the distribution of intermediate mass elements, e.g., silicon and magnesium, indicate that the outer ejecta did not experience significant mixing during or after burning, and the late phase NIR line profiles suggests most of the 56Ni is produced during high density burning. The various observational properties of SN 2012Z are found to be consistent with the theoretical expectations of a Chandrasekhar mass white dwarf progenitor that experiences a pulsational delayed detonation, which produced several tenths of a solar mass of 56Ni during the deflagration burning phase and little (or no) 56Ni during the detonation phase. Within this scenario only a moderate amount of Rayleigh-Taylor mixing occurs both during the deflagration and fallback phase of the pulsation, and the layered structure of the intermediate mass elements is a product of the subsequent denotation phase. The fact that the SNe Iax population does not follow a tight brightness-decline relation similar to SNe Ia can then be understood in the framework of variable amounts of mixing during pulsational rebound and variable amounts of 56Ni production during the early subsonic phase of expansion.

Idioma originalEnglish
Número de artículoA6
PublicaciónAstronomy and Astrophysics
Volumen573
DOI
EstadoPublished - 1 ene 2015

Huella dactilar

supernovae
explosions
explosion
energetics
near infrared
deflagration
detonation
wavelength
ejecta
infrared spectroscopy
erg
silicon
magnesium
wavelengths
light curve
photometry
brightness
infrared spectra
time measurement
broadband

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Stritzinger, M. D. ; Valenti, S. ; Hoeflich, P. ; Baron, E. ; Phillips, M. M. ; Taddia, F. ; Foley, R. J. ; Hsiao, E. Y. ; Jha, S. W. ; McCully, C. ; Pandya, V. ; Simon, J. D. ; Benetti, S. ; Brown, P. J. ; Burns, C. R. ; Campillay, A. ; Contreras, C. ; Förster, F. ; Holmbo, S. ; Marion, G. H. ; Morrell, N. ; Pignata, G. / Comprehensive observations of the bright and energetic Type Iax SN 2012Z : Interpretation as a Chandrasekhar mass white dwarf explosion ∗. En: Astronomy and Astrophysics. 2015 ; Vol. 573.
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title = "Comprehensive observations of the bright and energetic Type Iax SN 2012Z: Interpretation as a Chandrasekhar mass white dwarf explosion ∗",
abstract = "We present ultraviolet through near-infrared (NIR) broadband photometry, and visual-wavelength and NIR spectroscopy of the Type Iax supernova (SN) 2012Z. The data set consists of both early- and late-time observations, including the first late phase NIR spectrum obtained for a spectroscopically classified SN Iax. Simple model calculations of its bolometric light curve suggest SN 2012Z produced ∼0.3 M™ of 56Ni, ejected about a Chandrasekhar mass of material, and had an explosion energy of ∼1051 erg, making it one of the brightest (MB = -18.3 mag) and most energetic SN Iax yet observed. The late phase (+269d) NIRspectrum of SN 2012Z is found to broadly resemble similar epoch spectra of normal SNe Ia; however, like other SNe Iax, corresponding visual-wavelength spectra differ substantially from all supernova types. Constraints from the distribution of intermediate mass elements, e.g., silicon and magnesium, indicate that the outer ejecta did not experience significant mixing during or after burning, and the late phase NIR line profiles suggests most of the 56Ni is produced during high density burning. The various observational properties of SN 2012Z are found to be consistent with the theoretical expectations of a Chandrasekhar mass white dwarf progenitor that experiences a pulsational delayed detonation, which produced several tenths of a solar mass of 56Ni during the deflagration burning phase and little (or no) 56Ni during the detonation phase. Within this scenario only a moderate amount of Rayleigh-Taylor mixing occurs both during the deflagration and fallback phase of the pulsation, and the layered structure of the intermediate mass elements is a product of the subsequent denotation phase. The fact that the SNe Iax population does not follow a tight brightness-decline relation similar to SNe Ia can then be understood in the framework of variable amounts of mixing during pulsational rebound and variable amounts of 56Ni production during the early subsonic phase of expansion.",
keywords = "Supernovae: general, Supernovae: individual: SN 2005hk, Supernovae: individual: SN 2012Z",
author = "Stritzinger, {M. D.} and S. Valenti and P. Hoeflich and E. Baron and Phillips, {M. M.} and F. Taddia and Foley, {R. J.} and Hsiao, {E. Y.} and Jha, {S. W.} and C. McCully and V. Pandya and Simon, {J. D.} and S. Benetti and Brown, {P. J.} and Burns, {C. R.} and A. Campillay and C. Contreras and F. F{\"o}rster and S. Holmbo and Marion, {G. H.} and N. Morrell and G. Pignata",
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Stritzinger, MD, Valenti, S, Hoeflich, P, Baron, E, Phillips, MM, Taddia, F, Foley, RJ, Hsiao, EY, Jha, SW, McCully, C, Pandya, V, Simon, JD, Benetti, S, Brown, PJ, Burns, CR, Campillay, A, Contreras, C, Förster, F, Holmbo, S, Marion, GH, Morrell, N & Pignata, G 2015, 'Comprehensive observations of the bright and energetic Type Iax SN 2012Z: Interpretation as a Chandrasekhar mass white dwarf explosion ∗', Astronomy and Astrophysics, vol. 573, A6. https://doi.org/10.1051/0004-6361/201424168

Comprehensive observations of the bright and energetic Type Iax SN 2012Z : Interpretation as a Chandrasekhar mass white dwarf explosion ∗. / Stritzinger, M. D.; Valenti, S.; Hoeflich, P.; Baron, E.; Phillips, M. M.; Taddia, F.; Foley, R. J.; Hsiao, E. Y.; Jha, S. W.; McCully, C.; Pandya, V.; Simon, J. D.; Benetti, S.; Brown, P. J.; Burns, C. R.; Campillay, A.; Contreras, C.; Förster, F.; Holmbo, S.; Marion, G. H.; Morrell, N.; Pignata, G.

En: Astronomy and Astrophysics, Vol. 573, A6, 01.01.2015.

Resultado de la investigación: Article

TY - JOUR

T1 - Comprehensive observations of the bright and energetic Type Iax SN 2012Z

T2 - Interpretation as a Chandrasekhar mass white dwarf explosion ∗

AU - Stritzinger, M. D.

AU - Valenti, S.

AU - Hoeflich, P.

AU - Baron, E.

AU - Phillips, M. M.

AU - Taddia, F.

AU - Foley, R. J.

AU - Hsiao, E. Y.

AU - Jha, S. W.

AU - McCully, C.

AU - Pandya, V.

AU - Simon, J. D.

AU - Benetti, S.

AU - Brown, P. J.

AU - Burns, C. R.

AU - Campillay, A.

AU - Contreras, C.

AU - Förster, F.

AU - Holmbo, S.

AU - Marion, G. H.

AU - Morrell, N.

AU - Pignata, G.

PY - 2015/1/1

Y1 - 2015/1/1

N2 - We present ultraviolet through near-infrared (NIR) broadband photometry, and visual-wavelength and NIR spectroscopy of the Type Iax supernova (SN) 2012Z. The data set consists of both early- and late-time observations, including the first late phase NIR spectrum obtained for a spectroscopically classified SN Iax. Simple model calculations of its bolometric light curve suggest SN 2012Z produced ∼0.3 M™ of 56Ni, ejected about a Chandrasekhar mass of material, and had an explosion energy of ∼1051 erg, making it one of the brightest (MB = -18.3 mag) and most energetic SN Iax yet observed. The late phase (+269d) NIRspectrum of SN 2012Z is found to broadly resemble similar epoch spectra of normal SNe Ia; however, like other SNe Iax, corresponding visual-wavelength spectra differ substantially from all supernova types. Constraints from the distribution of intermediate mass elements, e.g., silicon and magnesium, indicate that the outer ejecta did not experience significant mixing during or after burning, and the late phase NIR line profiles suggests most of the 56Ni is produced during high density burning. The various observational properties of SN 2012Z are found to be consistent with the theoretical expectations of a Chandrasekhar mass white dwarf progenitor that experiences a pulsational delayed detonation, which produced several tenths of a solar mass of 56Ni during the deflagration burning phase and little (or no) 56Ni during the detonation phase. Within this scenario only a moderate amount of Rayleigh-Taylor mixing occurs both during the deflagration and fallback phase of the pulsation, and the layered structure of the intermediate mass elements is a product of the subsequent denotation phase. The fact that the SNe Iax population does not follow a tight brightness-decline relation similar to SNe Ia can then be understood in the framework of variable amounts of mixing during pulsational rebound and variable amounts of 56Ni production during the early subsonic phase of expansion.

AB - We present ultraviolet through near-infrared (NIR) broadband photometry, and visual-wavelength and NIR spectroscopy of the Type Iax supernova (SN) 2012Z. The data set consists of both early- and late-time observations, including the first late phase NIR spectrum obtained for a spectroscopically classified SN Iax. Simple model calculations of its bolometric light curve suggest SN 2012Z produced ∼0.3 M™ of 56Ni, ejected about a Chandrasekhar mass of material, and had an explosion energy of ∼1051 erg, making it one of the brightest (MB = -18.3 mag) and most energetic SN Iax yet observed. The late phase (+269d) NIRspectrum of SN 2012Z is found to broadly resemble similar epoch spectra of normal SNe Ia; however, like other SNe Iax, corresponding visual-wavelength spectra differ substantially from all supernova types. Constraints from the distribution of intermediate mass elements, e.g., silicon and magnesium, indicate that the outer ejecta did not experience significant mixing during or after burning, and the late phase NIR line profiles suggests most of the 56Ni is produced during high density burning. The various observational properties of SN 2012Z are found to be consistent with the theoretical expectations of a Chandrasekhar mass white dwarf progenitor that experiences a pulsational delayed detonation, which produced several tenths of a solar mass of 56Ni during the deflagration burning phase and little (or no) 56Ni during the detonation phase. Within this scenario only a moderate amount of Rayleigh-Taylor mixing occurs both during the deflagration and fallback phase of the pulsation, and the layered structure of the intermediate mass elements is a product of the subsequent denotation phase. The fact that the SNe Iax population does not follow a tight brightness-decline relation similar to SNe Ia can then be understood in the framework of variable amounts of mixing during pulsational rebound and variable amounts of 56Ni production during the early subsonic phase of expansion.

KW - Supernovae: general

KW - Supernovae: individual: SN 2005hk

KW - Supernovae: individual: SN 2012Z

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U2 - 10.1051/0004-6361/201424168

DO - 10.1051/0004-6361/201424168

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JO - Astronomy and Astrophysics

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