Constraints on the Progenitor System and the Environs of Sn 2014j From Deep Radio Observations

Pérez-Torres, M. Á.; Lundqvist, Peter; Beswick, R. J.; Björnsson, C. I.; Muxlow, T. W. B.; Paragi, Z.; Ryder, S. D.; Alberdi, A.; Fransson, Claes; Marcaide, J. M.; Martí-Vidal, Iván; Ros, E.; Argo, M. K.; Guirado, J. C.

doi:10.1088/0004-637x/792/1/38

Cited by 96 publications

(146 citation statements)

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“…This type of companion are indeed ruled out by several authors as possible progenitors in SN 2014J, e.g. Pérez-Torres et al (2014), with the most sensitive study in the radio band of a Type Ia SN, or Margutti et al (2014) in the X-ray band. The former reported non-detection from the observations performed with eMERLIN and EVN.…”

Section: Introductionmentioning

confidence: 80%

Very-high-energy gamma-ray observations of the Type Ia supernova SN 2014J with the MAGIC telescopes

Fernández-Barral¹,

Fruck²,

Blanch³

et al. 2017

AIP Conference Proceedings

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Context. In this work we present data from observations with the MAGIC telescopes of SN 2014J detected in January 21 2014, the closest Type Ia supernova since Imaging Air Cherenkov Telescopes started to operate. Aims. We probe the possibility of very-high-energy (VHE; E ≥ 100 GeV) gamma rays produced in the early stages of Type Ia supernova explosions. Methods. We performed follow-up observations after this supernova explosion for 5 days, between January 27 and February 2 in 2014. We search for gamma-ray signal in the energy range between 100 GeV and several TeV from the location of SN 2014J using data from a total of ∼ 5.5 hours of observations. Prospects for observing gamma-rays of hadronic origin from SN 2014J in the near future are also being addressed. Results. No significant excess was detected from the direction of SN 2014J. Upper limits at 95% confidence level on the integral flux, assuming a power-law spectrum, dF/dE ∝ E −Γ , with a spectral index of Γ = 2.6, for energies higher than 300 GeV and 700 GeV, are established at 1.3 × 10 −12 and 4.1 × 10 −13 photons cm −2 s −1 , respectively. Conclusions. For the first time, upper limits on the VHE emission of a Type Ia supernova are established. The energy fraction isotropically emitted into TeV gamma rays during the first ∼ 10 days after the supernova explosion for energies greater than 300 GeV is limited to 10 −6 of the total available energy budget (∼ 10 51 erg). Within the assumed theoretical scenario, the MAGIC upper limits on the VHE emission suggest that SN 2014J will not be detectable in the future by any current or planned generation of Imaging Atmospheric Cherenkov Telescopes.

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Section: Introductionmentioning

confidence: 80%

Very-high-energy gamma-ray observations of the Type Ia supernova SN 2014J with the MAGIC telescopes

Fernández-Barral¹,

Fruck²,

Blanch³

et al. 2017

AIP Conference Proceedings

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“…In the present study I examine some properties of the type Ia SN 2014J, concentrating on the medium around it. I take into account limits on the pre-explosion progenitor (Kelly et al 2014;Nielsen et al 2014;Lundqvist et al 2015) and its mass loss (Pérez-Torres et al 2014), and the properties of the absorption potassium lines (Ritchey et al 2014), and their time-variability (Graham et al 2015). ¿From radio observations Pérez-Torres et al (2014) limit the mass loss rate from the progenitor of SN 2014J to < 7.0 × 10 −10 M⊙ yr −1 for a wind speed of 100 km s −1 .…”

Section: Introductionmentioning

confidence: 99%

“…I take into account limits on the pre-explosion progenitor (Kelly et al 2014;Nielsen et al 2014;Lundqvist et al 2015) and its mass loss (Pérez-Torres et al 2014), and the properties of the absorption potassium lines (Ritchey et al 2014), and their time-variability (Graham et al 2015). ¿From radio observations Pérez-Torres et al (2014) limit the mass loss rate from the progenitor of SN 2014J to < 7.0 × 10 −10 M⊙ yr −1 for a wind speed of 100 km s −1 . This contradicts many cases of the SD scenario, but not those with a long delay to explosion (Di Stefano et al 2011;Justham 2011).…”

Section: Introductionmentioning

confidence: 99%

“…¿From radio observations Pérez-Torres et al (2014) limit the mass loss rate from the progenitor of SN 2014J to < 7.0 × 10 −10 M⊙ yr −1 for a wind speed of 100 km s −1 . This contradicts many cases of the SD scenario, but not those with a long delay to explosion (Di Stefano et al 2011;Justham 2011). Pérez-Torres et al (2014 consider the DD scenario to be the alternative to the SD scenario; without explanation they ignore the other three scenarios listed above, and the presence of dense circum-stellar matter (CSM) in some cases of the DD scenario Raskin et al 2014;Levanon et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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The circumstellar matter of supernova 2014J and the core-degenerate scenario

Soker

2015

Monthly Notices of the Royal Astronomical Society

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I show that the circumstellar matter (CSM) of the type Ia supernova 2014J is too massive and its momentum too large to be accounted for by any but the core-degenerate (CD) scenario for type Ia supernovae. Assuming the absorbing gas is of CSM origin, the several shells responsible of the absorption potassium lines are accounted for by a mass loss episode from a massive asymptotic giant branch star during a common envelope phase with a white dwarf companion. The time-varying potassium lines can be accounted for by ionization of neutral potassium and the Na-from-dust absorption (NaDA) model. Before explosion some of the potassium resides in the gas phase and some in dust. Weakening in absorption strength is caused by potassium-ionizing radiation of the supernova, while release of atomic potassium from dust increases the absorption. I conclude that if the absorbing gas originated from the progenitor of SN 2014J, then a common envelope phase took place about 15,000 years ago, leading to the merging of the core with the white dwarf companion, i.e., the core-degenerate scenario. Else, the absorbing material is of interstellar medium origin.

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“…By mid-march, SN 2014J had faded below 12.0 mag, but it was still well placed in the sky for good-quality observations. It has been observed by many telescopes and in different wavelength regions (Telesco, C. M. et al, 2015;Foley, R. J. et al, 2014;Ashall et al 2014;Margutti et al 2014;Pérez-Torres, M. A. et al, 2014), however, none of them have obtained observations with a very detailed time series of optical spectra with higher resolution.…”

Section: Introductionmentioning

confidence: 99%

Time series of high-resolution spectra of SN 2014J observed with the TIGRE telescope

Jack¹,

Mittag²,

Schröder³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a time series of high resolution spectra of the Type Ia supernova 2014J, which exploded in the nearby galaxy M82. The spectra were obtained with the HEROŚ echelle spectrograph installed at the 1.2 m TIGRE telescope. We present a series of 33 spectra with a resolution of R ≈ 20, 000, which covers the important bright phases in the evolution of SN 2014J during the period from January 24 to April 1 of 2014. The spectral evolution of SN 2014J is derived empirically. The expansion velocities of the Si II P-Cygni features were measured and show the expected decreasing behaviour, beginning with a high velocity of 14,000 km/s on January 24. The Ca II infrared triplet feature shows a high velocity component with expansion velocities of > 20, 000 km/s during the early evolution apart from the normal component showing similar velocities as Si II. Further broad P-Cygni profiles are exhibited by the principal lines of Ca II, Mg II and Fe II. The TIGRE SN 2014J spectra also resolve several very sharp Na I D doublet absorption components. Our analysis suggests interesting substructures in the interstellar medium of the host galaxy M82, as well as in our Milky Way, confirming other work on this SN. We were able to identify the interstellar absorption of M82 in the lines of Ca II H & K at 3933 and 3968Å as well as K I at 7664 and 7698Å. Furthermore, we confirm several Diffuse Interstellar Bands, at wavelengths of 6196, 6283, 6376, 6379 and 6613Å and give their measured equivalent widths.

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Constraints on the Progenitor System and the Environs of Sn 2014j From Deep Radio Observations

Cited by 96 publications

References 65 publications

Very-high-energy gamma-ray observations of the Type Ia supernova SN 2014J with the MAGIC telescopes

Very-high-energy gamma-ray observations of the Type Ia supernova SN 2014J with the MAGIC telescopes

The circumstellar matter of supernova 2014J and the core-degenerate scenario

Time series of high-resolution spectra of SN 2014J observed with the TIGRE telescope

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