SN 2009ipà la PESSTO: No evidence for core collapse yet

Morgan Fraser, Cosimo Inserra, Anders Jerkstrand, Rubina Kotak, Giuliano Pignata, Stefano Benetti, Maria Teresa Botticella, Filomena Bufano, Michael Childress, Seppo Mattila, Andrea Pastorello, Stephen J. Smartt, Massimo Turatto, Fang Yuan, Joe P. Anderson, Daniel D.R. Bayliss, Franz Erik Bauer, Ting Wan Chen, Francisco Förster Burón, Avishay Gal-YamJoshua B. Haislip, Cristina Knapic, Laurent Le Guillou, Sebastián Marchi, Paolo Mazzali, Marco Molinaro, Justin P. Moore, Daniel Reichart, Riccardo Smareglia, Ken W. Smith, Assaf Sternberg, Mark Sullivan, Katalin Takáts, Brad E. Tucker, Stefano Valenti, Ofer Yaron, David R. Young, George Zhou

Resultado de la investigación: Article

72 Citas (Scopus)

Resumen

We present ultraviolet, optical and near-infrared observations of the interacting transient SN 2009ip, covering the period from the start of the outburst in 2012 October until the end of the 2012 observing season. The transient reached a peak magnitude of MV =-17.7mag, with a total integrated luminosity of 1.9 × 1049 erg over the period of 2012 August-December. The light curve fades rapidly, dropping by 4.5 mag from the V-band peak in 100 d. The optical and near-infrared spectra are dominated by narrow emission lines with broad electron scattering wings, signalling a dense circumstellar environment, together with multiple components of broad emission and absorption in H and He at velocities in the range 0.5-1.2 × 104 km s-1. We see no evidence for nucleosynthesized material in SN 2009ip, even in late-time pseudonebular spectra. We set a limit of<0.02Mȯ on themass of any possible synthesized 56Ni from the late-time light curve. A simple model for the narrow Balmer lines is presented and used to derive number densities for the circumstellar medium in the range ~109-1010 cm. Our near-infrared data do not show any excess at longer wavelengths, and we see no other signs of dust formation. Our last data, taken in 2012 December, show that SN 2009ip has spectroscopically evolved to something quite similar to its appearance in late 2009, albeit with higher velocities. It is possible that neither of the eruptive and high-luminosity events of SN 2009ip were induced by a core collapse. We show that the peak and total integrated luminosity can be due to the efficient conversion of kinetic energy from colliding ejecta, and that around 0.05-0.1 Mȯ of material moving at 0.5-1 × 104 km s-1 could comfortably produce the observed luminosity. We discuss the possibility that these shells were ejected by the pulsational pair instability mechanism, in which case the progenitor star may still exist, and will be observed after the current outburst fades. The long-term monitoring of SN 2009ip, due to its proximity, has given the most extensive data set yet gathered of a high-luminosity interacting transient and its progenitor. It is possible that some purported Type IIn supernovae are in fact analogues of the 2012b event and that pre-explosion outbursts have gone undetected.

Idioma originalEnglish
Páginas (desde-hasta)1312-1337
Número de páginas26
PublicaciónMonthly Notices of the Royal Astronomical Society
Volumen433
N.º2
DOI
EstadoPublished - 1 jul 2013

Huella dactilar

luminosity
outburst
near infrared
light curve
ejecta
extremely high frequencies
wings
erg
kinetic energy
supernovae
explosions
proximity
explosion
electron scattering
coverings
infrared spectra
dust
scattering
shell
analogs

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Fraser, M., Inserra, C., Jerkstrand, A., Kotak, R., Pignata, G., Benetti, S., ... Zhou, G. (2013). SN 2009ipà la PESSTO: No evidence for core collapse yet. Monthly Notices of the Royal Astronomical Society, 433(2), 1312-1337. https://doi.org/10.1093/mnras/stt813
Fraser, Morgan ; Inserra, Cosimo ; Jerkstrand, Anders ; Kotak, Rubina ; Pignata, Giuliano ; Benetti, Stefano ; Botticella, Maria Teresa ; Bufano, Filomena ; Childress, Michael ; Mattila, Seppo ; Pastorello, Andrea ; Smartt, Stephen J. ; Turatto, Massimo ; Yuan, Fang ; Anderson, Joe P. ; Bayliss, Daniel D.R. ; Bauer, Franz Erik ; Chen, Ting Wan ; Burón, Francisco Förster ; Gal-Yam, Avishay ; Haislip, Joshua B. ; Knapic, Cristina ; Le Guillou, Laurent ; Marchi, Sebastián ; Mazzali, Paolo ; Molinaro, Marco ; Moore, Justin P. ; Reichart, Daniel ; Smareglia, Riccardo ; Smith, Ken W. ; Sternberg, Assaf ; Sullivan, Mark ; Takáts, Katalin ; Tucker, Brad E. ; Valenti, Stefano ; Yaron, Ofer ; Young, David R. ; Zhou, George. / SN 2009ipà la PESSTO : No evidence for core collapse yet. En: Monthly Notices of the Royal Astronomical Society. 2013 ; Vol. 433, N.º 2. pp. 1312-1337.
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title = "SN 2009ip{\`a} la PESSTO: No evidence for core collapse yet",
abstract = "We present ultraviolet, optical and near-infrared observations of the interacting transient SN 2009ip, covering the period from the start of the outburst in 2012 October until the end of the 2012 observing season. The transient reached a peak magnitude of MV =-17.7mag, with a total integrated luminosity of 1.9 × 1049 erg over the period of 2012 August-December. The light curve fades rapidly, dropping by 4.5 mag from the V-band peak in 100 d. The optical and near-infrared spectra are dominated by narrow emission lines with broad electron scattering wings, signalling a dense circumstellar environment, together with multiple components of broad emission and absorption in H and He at velocities in the range 0.5-1.2 × 104 km s-1. We see no evidence for nucleosynthesized material in SN 2009ip, even in late-time pseudonebular spectra. We set a limit of<0.02Mȯ on themass of any possible synthesized 56Ni from the late-time light curve. A simple model for the narrow Balmer lines is presented and used to derive number densities for the circumstellar medium in the range ~109-1010 cm. Our near-infrared data do not show any excess at longer wavelengths, and we see no other signs of dust formation. Our last data, taken in 2012 December, show that SN 2009ip has spectroscopically evolved to something quite similar to its appearance in late 2009, albeit with higher velocities. It is possible that neither of the eruptive and high-luminosity events of SN 2009ip were induced by a core collapse. We show that the peak and total integrated luminosity can be due to the efficient conversion of kinetic energy from colliding ejecta, and that around 0.05-0.1 Mȯ of material moving at 0.5-1 × 104 km s-1 could comfortably produce the observed luminosity. We discuss the possibility that these shells were ejected by the pulsational pair instability mechanism, in which case the progenitor star may still exist, and will be observed after the current outburst fades. The long-term monitoring of SN 2009ip, due to its proximity, has given the most extensive data set yet gathered of a high-luminosity interacting transient and its progenitor. It is possible that some purported Type IIn supernovae are in fact analogues of the 2012b event and that pre-explosion outbursts have gone undetected.",
author = "Morgan Fraser and Cosimo Inserra and Anders Jerkstrand and Rubina Kotak and Giuliano Pignata and Stefano Benetti and Botticella, {Maria Teresa} and Filomena Bufano and Michael Childress and Seppo Mattila and Andrea Pastorello and Smartt, {Stephen J.} and Massimo Turatto and Fang Yuan and Anderson, {Joe P.} and Bayliss, {Daniel D.R.} and Bauer, {Franz Erik} and Chen, {Ting Wan} and Bur{\'o}n, {Francisco F{\"o}rster} and Avishay Gal-Yam and Haislip, {Joshua B.} and Cristina Knapic and {Le Guillou}, Laurent and Sebasti{\'a}n Marchi and Paolo Mazzali and Marco Molinaro and Moore, {Justin P.} and Daniel Reichart and Riccardo Smareglia and Smith, {Ken W.} and Assaf Sternberg and Mark Sullivan and Katalin Tak{\'a}ts and Tucker, {Brad E.} and Stefano Valenti and Ofer Yaron and Young, {David R.} and George Zhou",
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language = "English",
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Fraser, M, Inserra, C, Jerkstrand, A, Kotak, R, Pignata, G, Benetti, S, Botticella, MT, Bufano, F, Childress, M, Mattila, S, Pastorello, A, Smartt, SJ, Turatto, M, Yuan, F, Anderson, JP, Bayliss, DDR, Bauer, FE, Chen, TW, Burón, FF, Gal-Yam, A, Haislip, JB, Knapic, C, Le Guillou, L, Marchi, S, Mazzali, P, Molinaro, M, Moore, JP, Reichart, D, Smareglia, R, Smith, KW, Sternberg, A, Sullivan, M, Takáts, K, Tucker, BE, Valenti, S, Yaron, O, Young, DR & Zhou, G 2013, 'SN 2009ipà la PESSTO: No evidence for core collapse yet', Monthly Notices of the Royal Astronomical Society, vol. 433, n.º 2, pp. 1312-1337. https://doi.org/10.1093/mnras/stt813

SN 2009ipà la PESSTO : No evidence for core collapse yet. / Fraser, Morgan; Inserra, Cosimo; Jerkstrand, Anders; Kotak, Rubina; Pignata, Giuliano; Benetti, Stefano; Botticella, Maria Teresa; Bufano, Filomena; Childress, Michael; Mattila, Seppo; Pastorello, Andrea; Smartt, Stephen J.; Turatto, Massimo; Yuan, Fang; Anderson, Joe P.; Bayliss, Daniel D.R.; Bauer, Franz Erik; Chen, Ting Wan; Burón, Francisco Förster; Gal-Yam, Avishay; Haislip, Joshua B.; Knapic, Cristina; Le Guillou, Laurent; Marchi, Sebastián; Mazzali, Paolo; Molinaro, Marco; Moore, Justin P.; Reichart, Daniel; Smareglia, Riccardo; Smith, Ken W.; Sternberg, Assaf; Sullivan, Mark; Takáts, Katalin; Tucker, Brad E.; Valenti, Stefano; Yaron, Ofer; Young, David R.; Zhou, George.

En: Monthly Notices of the Royal Astronomical Society, Vol. 433, N.º 2, 01.07.2013, p. 1312-1337.

Resultado de la investigación: Article

TY - JOUR

T1 - SN 2009ipà la PESSTO

T2 - No evidence for core collapse yet

AU - Fraser, Morgan

AU - Inserra, Cosimo

AU - Jerkstrand, Anders

AU - Kotak, Rubina

AU - Pignata, Giuliano

AU - Benetti, Stefano

AU - Botticella, Maria Teresa

AU - Bufano, Filomena

AU - Childress, Michael

AU - Mattila, Seppo

AU - Pastorello, Andrea

AU - Smartt, Stephen J.

AU - Turatto, Massimo

AU - Yuan, Fang

AU - Anderson, Joe P.

AU - Bayliss, Daniel D.R.

AU - Bauer, Franz Erik

AU - Chen, Ting Wan

AU - Burón, Francisco Förster

AU - Gal-Yam, Avishay

AU - Haislip, Joshua B.

AU - Knapic, Cristina

AU - Le Guillou, Laurent

AU - Marchi, Sebastián

AU - Mazzali, Paolo

AU - Molinaro, Marco

AU - Moore, Justin P.

AU - Reichart, Daniel

AU - Smareglia, Riccardo

AU - Smith, Ken W.

AU - Sternberg, Assaf

AU - Sullivan, Mark

AU - Takáts, Katalin

AU - Tucker, Brad E.

AU - Valenti, Stefano

AU - Yaron, Ofer

AU - Young, David R.

AU - Zhou, George

PY - 2013/7/1

Y1 - 2013/7/1

N2 - We present ultraviolet, optical and near-infrared observations of the interacting transient SN 2009ip, covering the period from the start of the outburst in 2012 October until the end of the 2012 observing season. The transient reached a peak magnitude of MV =-17.7mag, with a total integrated luminosity of 1.9 × 1049 erg over the period of 2012 August-December. The light curve fades rapidly, dropping by 4.5 mag from the V-band peak in 100 d. The optical and near-infrared spectra are dominated by narrow emission lines with broad electron scattering wings, signalling a dense circumstellar environment, together with multiple components of broad emission and absorption in H and He at velocities in the range 0.5-1.2 × 104 km s-1. We see no evidence for nucleosynthesized material in SN 2009ip, even in late-time pseudonebular spectra. We set a limit of<0.02Mȯ on themass of any possible synthesized 56Ni from the late-time light curve. A simple model for the narrow Balmer lines is presented and used to derive number densities for the circumstellar medium in the range ~109-1010 cm. Our near-infrared data do not show any excess at longer wavelengths, and we see no other signs of dust formation. Our last data, taken in 2012 December, show that SN 2009ip has spectroscopically evolved to something quite similar to its appearance in late 2009, albeit with higher velocities. It is possible that neither of the eruptive and high-luminosity events of SN 2009ip were induced by a core collapse. We show that the peak and total integrated luminosity can be due to the efficient conversion of kinetic energy from colliding ejecta, and that around 0.05-0.1 Mȯ of material moving at 0.5-1 × 104 km s-1 could comfortably produce the observed luminosity. We discuss the possibility that these shells were ejected by the pulsational pair instability mechanism, in which case the progenitor star may still exist, and will be observed after the current outburst fades. The long-term monitoring of SN 2009ip, due to its proximity, has given the most extensive data set yet gathered of a high-luminosity interacting transient and its progenitor. It is possible that some purported Type IIn supernovae are in fact analogues of the 2012b event and that pre-explosion outbursts have gone undetected.

AB - We present ultraviolet, optical and near-infrared observations of the interacting transient SN 2009ip, covering the period from the start of the outburst in 2012 October until the end of the 2012 observing season. The transient reached a peak magnitude of MV =-17.7mag, with a total integrated luminosity of 1.9 × 1049 erg over the period of 2012 August-December. The light curve fades rapidly, dropping by 4.5 mag from the V-band peak in 100 d. The optical and near-infrared spectra are dominated by narrow emission lines with broad electron scattering wings, signalling a dense circumstellar environment, together with multiple components of broad emission and absorption in H and He at velocities in the range 0.5-1.2 × 104 km s-1. We see no evidence for nucleosynthesized material in SN 2009ip, even in late-time pseudonebular spectra. We set a limit of<0.02Mȯ on themass of any possible synthesized 56Ni from the late-time light curve. A simple model for the narrow Balmer lines is presented and used to derive number densities for the circumstellar medium in the range ~109-1010 cm. Our near-infrared data do not show any excess at longer wavelengths, and we see no other signs of dust formation. Our last data, taken in 2012 December, show that SN 2009ip has spectroscopically evolved to something quite similar to its appearance in late 2009, albeit with higher velocities. It is possible that neither of the eruptive and high-luminosity events of SN 2009ip were induced by a core collapse. We show that the peak and total integrated luminosity can be due to the efficient conversion of kinetic energy from colliding ejecta, and that around 0.05-0.1 Mȯ of material moving at 0.5-1 × 104 km s-1 could comfortably produce the observed luminosity. We discuss the possibility that these shells were ejected by the pulsational pair instability mechanism, in which case the progenitor star may still exist, and will be observed after the current outburst fades. The long-term monitoring of SN 2009ip, due to its proximity, has given the most extensive data set yet gathered of a high-luminosity interacting transient and its progenitor. It is possible that some purported Type IIn supernovae are in fact analogues of the 2012b event and that pre-explosion outbursts have gone undetected.

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U2 - 10.1093/mnras/stt813

DO - 10.1093/mnras/stt813

M3 - Article

AN - SCOPUS:84880436172

VL - 433

SP - 1312

EP - 1337

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

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