A Deep Search for Prompt Radio Emission From Thermonuclear Supernovae With the Very Large Array

Chomiuk, Laura; Söderberg, A. M.; Chevalier, Roger A.; Bruzewski, S.; Foley, R. J.; Parrent, J.; Strader, Jay; Badenes, Carles; Fransson, Claes; Kamble, A.; Margutti, R.; Rupen, M. P.; Simon, Joshua D.

doi:10.3847/0004-637x/821/2/119

Cited by 115 publications

(185 citation statements)

References 187 publications

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“…Hubble Space Telescope (HST) pre-explosion images of NGC 4424 revealed no source at the location of the SN down to limits of M V ∼−6.0 and M I ∼−5.4 mags and excluded most supergiants as potential binary companions (Graur & Maoz 2012). Chomiuk et al (2012) did not detect the SN in the radio and constrained any possible circumstellar material to either lie at distances >10 16 cm or be distributed in thin shells <10 15 cm wide.…”

Section: Introductionmentioning

confidence: 99%

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

Graur

Zurek

Shara

et al. 2016

ApJ

103

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Seitenzahl et al. have predicted that roughly three years after its explosion, the light we receive from a Type Ia supernova (SN Ia) will come mostly from reprocessing of electrons and X-rays emitted by the radioactive decay chain 57 Co→ 57 Fe, instead of positrons from the decay chain 56 Co→ 56 Fe that dominates the SN light at earlier times. Using the Hubble Space Telescope, we followed the light curve of the SN Ia SN 2012cg out to 1055 days after maximum light. Our measurements are consistent with the light curves predicted by the contribution of energy from the reprocessing of electrons and X-rays emitted by the decay of 57 Co, offering evidence that 57 Co is produced in SN Ia explosions. However, the data are also consistent with a light echo ∼14 mag fainter than SN 2012cg at peak. Assuming no light-echo contamination, the mass ratio of 57 Ni and 56 Ni produced by the explosion, a strong constraint on any SN Ia explosion models, is 0.043 0.011 0.012 -+ , roughly twice Solar. In the context of current explosion models, this value favors a progenitor white dwarf with a mass near the Chandrasekhar limit.

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Section: Introductionmentioning

confidence: 99%

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

Graur

Zurek

Shara

et al. 2016

ApJ

103

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“…Spectropolarimetry of heavily reddened SNe Ia (Patat et al 2015), and the lack of infrared thermal emission (Johansson et al 2013(Johansson et al , 2016) from some of the same events, point to the absence of dust in the CS environments. In addition, strong limits from X-ray (Margutti et al 2014) and radio (Panagia et al 2006;Chomiuk et al 2016) observations point to very low mass-loss rates from the progenitor systems. Nevertheless, there are observations suggesting the existence of outflowing matter from SNe Ia.…”

Section: Introductionmentioning

confidence: 99%

Time-varying sodium absorption in the Type Ia supernova 2013gh

Ferretti

Amanullah

Goobar

et al. 2016

A&A

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Context. Temporal variability of narrow absorption lines in high-resolution spectra of Type Ia supernovae (SNe Ia) is studied to search for circumstellar matter. Time series which resolve the profiles of absorption lines such as Na I D or Ca II H&K are expected to reveal variations due to photoionisation and subsequent recombination of the gases. The presence, composition, and geometry of circumstellar matter may hint at the elusive progenitor system of SNe Ia and could also affect the observed reddening law. Aims. To date, there are few known cases of time-varying Na I D absorption in SNe Ia, all of which occurred during relatively late phases of the supernova (SN) evolution. Photoionisation, however, is predicted to occur during the early phases of SNe Ia, when the supernovae peak in the ultraviolet. We attempt, therefore, to observe early-time absorption-line variations by obtaining high-resolution spectra of SNe before maximum light. Methods. We have obtained photometry and high-resolution spectroscopy of SNe Ia 2013gh and iPTF 13dge, to search for absorptionline variations. Furthermore, we study interstellar absorption features in relation to the observed photometric colours of the SNe. Results. Both SNe display deep Na I D and Ca II H&K absorption features. Furthermore, small but significant variations are detected in a feature of the Na I D profile of SN 2013gh. The variations are consistent with either geometric effects of rapidly moving or patchy gas clouds or photoionisation of Na I gas at R ≈ 10 19 cm from the explosion. Conclusions. Our analysis indicates that it is necessary to focus on early phases to detect photoionisation effects of gases in the circumstellar medium of SNe Ia. Different absorbers such as Na I and Ca II can be used to probe for matter at different distances from the SNe. The nondetection of variations during early phases makes it possible to put limits on the abundance of the species at those distances.

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“…The number of subclasses has grown with the number of available spectra, with recent reviews distinguishing almost 10 (Chomiuk et al 2016;Taubenberger 2017).…”

Section: Introductionmentioning

confidence: 99%

Spectral Sequences of Type Ia Supernovae. I. Connecting Normal and Subluminous SNe Ia and the Presence of Unburned Carbon

Heringer

Kerkwijk

Kerzendorf

2017

ApJ

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Type Ia supernovae (SNe Ia)are generally agreed to arise from thermonuclear explosions of carbon-oxygen white dwarfs. The actual path to explosion, however, remains elusive, with numerous plausible parent systems and explosion mechanisms suggested. Observationally, SNe Ia have multiple subclasses, distinguished by their light curves and spectra. This raises the question of whether these indicate that multiple mechanisms occur in nature or that explosions have a large but continuous range of physical properties. We revisit the idea that normal and 91bg-like SNe can be understood as part of a spectral sequence in which changes in temperature dominate. Specifically, we find that a single ejecta structure is sufficient to provide reasonable fits of both the normal SN Ia SN2011fe and the 91bg-like SN2005bl, provided that the luminosity and thus temperature of the ejecta are adjusted appropriately. This suggests that the outer layers of the ejecta are similar, thus providing some support for a common explosion mechanism. Our spectral sequence also helps to shed light on the conditions under which carbon can be detected in premaximum SNIa spectra-we find that emission from iron can "fill in" the carbon trough in cool SNeIa. This may indicate that the outer layers of the ejecta of events in which carbon is detected are relatively metal-poor compared to events in which carbon is not detected.

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A Deep Search for Prompt Radio Emission From Thermonuclear Supernovae With the Very Large Array

Cited by 115 publications

References 187 publications

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

Time-varying sodium absorption in the Type Ia supernova 2013gh

Spectral Sequences of Type Ia Supernovae. I. Connecting Normal and Subluminous SNe Ia and the Presence of Unburned Carbon

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A Deep Search for Prompt Radio Emission From Thermonuclear Supernovae With the Very Large Array

Cited by 115 publications

References 187 publications

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF 57Co

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF 57Co

Time-varying sodium absorption in the Type Ia supernova 2013gh

Spectral Sequences of Type Ia Supernovae. I. Connecting Normal and Subluminous SNe Ia and the Presence of Unburned Carbon

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Product

Resources

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LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co