A Search for Radio Emission from Type Ia Supernovae

Panagia, N.; Dyk, Schuyler D. Van; Weiler, K. W.; Sramek, R. A.; Stockdale, C. J.; Murata, Kimberly P.

doi:10.1086/504710

Cited by 107 publications

(163 citation statements)

References 53 publications

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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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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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“…Such an assumption is necessary because the correlation between wind density and radio luminosity for SNe Ia cannot be calculated from theory at this point. In the absence of theoretical or observational support for such an assumption the very low mass-loss rates claimed by Panagia et al (2006) cannot yet be considered definitive ). The radio non-detections may therefore still permit the symbiotic scenario.…”

Section: Discussionmentioning

confidence: 98%

“…from the WD to be consistent with our Hα nondetections. For a 1.4 M ⊙ primary and a 1.0 M ⊙ secondary, this corresponds to an orbital period of 20 yr. Panagia et al (2006) rely on the assumption that SN Ia radio light curves behave identically to those of SNe Ib/c. Such an assumption is necessary because the correlation between wind density and radio luminosity for SNe Ia cannot be calculated from theory at this point.…”

Section: Discussionmentioning

confidence: 99%

Constraining the Type Ia Supernova Progenitor: The Search for Hydrogen in Nebular Spectra

Leonard

2007

AIP Conference Proceedings

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Despite intense scrutiny, the progenitor system(s) that gives rise to Type Ia supernovae remains unknown. The favored theory invokes a carbon-oxygen white dwarf accreting hydrogen-rich material from a close companion until a thermonuclear runaway ensues that incinerates the white dwarf. However, simulations resulting from this single-degenerate, binary channel demand the presence of low-velocity Hα emission in spectra taken during the late nebular phase, since a portion of the companion's envelope becomes entrained in the ejecta. This hydrogen has never been detected, but has only rarely been sought. Here we present results from a campaign to obtain deep, nebular-phase spectroscopy of nearby Type Ia supernovae, and include multi-epoch observations of two events: SN 2005am (slightly subluminous) and SN 2005cf (normally bright). No Hα emission is detected in the spectra of either object. An upper limit of 0.01 M ⊙ of solar abundance material in the ejecta is established from the models of Mattila et al. (2005) which, when coupled with the mass-stripping simulations of Marietta et al. (2000) and Meng et al. (2007), effectively rules out progenitor systems for these supernovae with secondaries close enough to the white dwarf to be experiencing Roche lobe overflow at the time of explosion. Alternative explanations for the absence of Hα emission, along with suggestions for future investigations necessary to confidently exclude them as possibilities, are critically evaluated.

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“…We choose a value of u w = 10 km s −1 , which is typical of the winds of evolved intermediate-mass stars (e.g. Panagia et al 2006).…”

Section: The Gas Bubblementioning

confidence: 99%

“…No direct detection has been made at this point, but upper limits are reaching interesting values. Using the VLA, Panagia et al (2006) found upper limits of ∼10 −6 M yr −1 based on observations of 27 SNe Ia. Their analysis is extrapolated from the assumption that the process behind radio emission from SNe Ia are similar to those of SNe Ib/c.…”

Section: Upper Limitsmentioning

confidence: 99%

Obscuration of supersoft X-ray sources by circumbinary material

Nielsen

Dominik

Nelemans

et al. 2012

A&A

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Context. The progenitors of Type Ia supernovae are usually assumed to be either a single white dwarf accreting from a non-degenerate companion (the single-degenerate channel) or the result of two merging white dwarfs (the double degenerate channel). However, no consensus currently exists as to which progenitor scenario is the correct one, or whether the observed Type Ia supernovae rate is produced by a combination of both channels. Unlike a double degenerate progenitor, a single-degenerate progenitor is expected to emit supersoft X-rays for a prolonged period of time (∼1 Myr) as a result of the burning of accreted matter on the surface of the white dwarf. An argument against the single-degenerate channel as a significant producer of Type Ia supernovae has been the lack of observed supersoft X-ray sources and the lower-than-expected integrated soft X-ray flux from elliptical galaxies. Aims. We wish to determine whether it is possible to obscure the supersoft X-ray emission from a nuclear-burning white dwarf in an accreting single-degenerate binary system. In the case of obscured systems we wish to determine their general observational characteristics. Methods. We examine the emergent X-ray emission from a canonical supersoft X-ray system surrounded by a spherically symmetric configuration of material, assuming a black-body spectrum with T bb = 50 eV and L = 10 38 erg s −1 . The circumbinary material is assumed to be of solar chemical abundances, and we leave the mechanism behind the mass-loss into the circumbinary region unspecified. Results. We find that relatively low circumstellar mass-loss rates,Ṁ = 10 −9 −10 −8 M yr −1 , at binary separations of ∼1 AU or less, will cause significant attenuation of the X-rays from the supersoft X-ray source. These circumstellar mass-loss rates are sufficient to make a canonical supersoft X-ray source in typical external galaxies unobservable in Chandra. Conclusions. If steadily accreting, nuclear-burning white dwarfs are canonical supersoft X-ray sources our analysis suggests that they can be obscured by relatively modest circumbinary mass-loss rates. This may explain the discrepancy of supersoft sources relative to the Type Ia supernova rate inferred from observations if the single-degenerate progenitor scenario contributes significantly to the Type Ia supernova rate. Recycled emissions from obscured systems may be visible in wavebands other than X-rays. It may also explain the lack of observed supersoft sources in symbiotic binary systems.

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A Search for Radio Emission from Type Ia Supernovae

Cited by 107 publications

References 53 publications

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

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

Constraining the Type Ia Supernova Progenitor: The Search for Hydrogen in Nebular Spectra

Obscuration of supersoft X-ray sources by circumbinary material

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