Abundance tomography of Type Iax SN 2011ay with tardis

Barna, Barnabás; Szalai, T.; Kromer, M.; Kerzendorf, Wolfgang; Vinkó, J.; Silverman, J. M.; Marion, G. H.; Wheeler, J. C.

doi:10.1093/mnras/stx1894

Cited by 36 publications

(42 citation statements)

References 70 publications

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“…The sample of objects is chosen to broadly represent the properties of the class. Similar to our pilot study for SN 2011ay (Barna et al 2017), we compare our findings with the results of previous spectral models, as well as with the predictions of the pure deflagration of a Chandrasekhar-mass WD with a bound remnant (the most promising explosion scenario for SNe Iax).…”

Section: Introductionsupporting

confidence: 71%

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Type Iax supernovae as a few-parameter family

Barna

Szalai

Kerzendorf

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present direct spectroscopic modeling of five Type Iax supernovae (SNe) with the one dimensional Monte Carlo radiative transfer code TARDIS. The abundance tomography technique is used to map the chemical structure and physical properties of the SN atmosphere. Through via fitting of multiple spectral epochs with self-consistent ejecta models, we can then constrain the location of some elements within the ejecta. The synthetic spectra of the best-fit models are able to reproduce the flux continuum and the main absorption features in the whole sample. We find that the mass fractions of IGEs and IMEs show a decreasing trend toward the outer regions of the atmospheres using density profiles similar to those of deflagration models in the literature. Oxygen is the only element, which could be dominant at higher velocities. The stratified abundance structure contradicts the well-mixed chemical profiles predicted by pure deflagration models. Based on the derived densities and abundances, a template model atmosphere is created for the SN Iax class and compared to the observed spectra. Free parameters are the scaling of the density profile, the velocity shift of the abundance template, and the peak luminosity. The results of this test support the idea that all SNe Iax can be described by a similar internal structure, which argues for a common origin of this class of explosions.

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Section: Introductionsupporting

confidence: 71%

“…The original spectroscopic data of SN 2011ay were published by Silverman et al (2012), while Szalai et al (2015) provided detailed photometric and spectroscopic analysis. Moreover, Barna et al (2017) published an abundance tomography analysis using TARDIS; a revision of these results is also part of the current paper.…”

Section: Sn 2011aymentioning

confidence: 98%

Type Iax supernovae as a few-parameter family

Barna

Szalai

Kerzendorf

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…(1) The weak deflagration model by Fink et al (2014) leads to a rapid decline in the post-maximum phase. However, the (2) The weak deflagration model inevitably leads to a well-mixed, non-stratified structure in the ejecta, while the layered structure has been inferred at least for some SNe Iax from the velocity evolution (SN 2012Z; Stritzinger et al 2015) and through spectral modeling (SN 2011ay; Barna et al 2017). Indeed, this feature has been suggested to be consistent with the PDD model rather than the weak deflagration model (Stritzinger et al 2015).…”

Section: Explosion Mechanismmentioning

confidence: 99%

Extended optical/NIR observations of Type Iax supernova 2014dt: Possible signatures of a bound remnant

Kawabata

Maeda

et al. 2018

Publications of the Astronomical Society of Japan

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We present optical and near-infrared observations of the nearby Type Iax supernova (SN) 2014dt from 14 to 410 days after the maximum light. The velocities of the iron absorption lines in the early phase indicated that SN 2014dt showed slower expansion than the well-observed Type Iax SNe 2002cx, 2005hk and 2012Z. In the late phase, the evolution of the light curve and that of the spectra were considerably slower. The spectral energy distribution kept roughly the same shape after ∼ 100 days, and the bolometric light curve flattened during the same period. These observations suggest the existence of an optically thick component that almost fully trapped the γ-ray energy from 56 Co decay. These findings are consistent with the predictions of the weak deflagration model, leaving a bound white dwarf remnant after the explosion.

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“…structure (Magee et al 2016(Magee et al , 2017Barna et al 2017Barna et al , 2018 and presence of helium in the ejecta (Magee et al 2019). tardis takes a model for the ejecta with arbitrary density and abundance profiles as input, along with a luminosity and time since explosion.…”

Section: Bolometric Light Curve and Explosion Parametersmentioning

confidence: 99%

The Lowest of the Low: Discovery of SN 2019gsc and the Nature of Faint Iax Supernovae

Srivastav

Smartt

Leloudas

et al. 2020

ApJL

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We present the discovery and optical follow-up of the faintest supernova-like transient known. The event (SN 2019gsc) was discovered in a star-forming host at 53 Mpc by ATLAS. A detailed multicolour light curve was gathered with Pan-STARRS1 and follow-up spectroscopy was obtained with the NOT and Gemini-North. The spectra near maximum light show narrow features at low velocities of 3000 to 4000 km s −1 , similar to the extremely low luminosity SNe 2010ae and 2008ha, and the light curve displays a similar fast decline (∆m 15 (r) = 0.91 ± 0.10 mag). SNe 2010ae and 2008ha have been classified as type Iax supernovae, and together the three either make up a distinct physical class of their own or are at the extreme low luminosity end of this diverse supernova population. The bolometric light curve is consistent with a low kinetic energy of explosion (E k ∼ 10 49 erg s −1 ), a modest ejected mass (M ej ∼ 0.2 M ) and radioactive powering by 56 Ni (M Ni ∼ 2 × 10 −3 M ). The spectra are quite well reproduced with radiative transfer models (TARDIS) and a composition dominated by carbon, oxygen, magnesium, silicon and sulphur. Remarkably, all three of these extreme Iax events are in similar low-metallicity star-forming environments. The combination of the observational constraints for all three may be best explained by deflagrations of near M Ch hybrid carbon-oxygen-neon white dwarfs which have short evolutionary pathways to formation.

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Abundance tomography of Type Iax SN 2011ay with tardis

Cited by 36 publications

References 70 publications

Type Iax supernovae as a few-parameter family

Type Iax supernovae as a few-parameter family

Extended optical/NIR observations of Type Iax supernova 2014dt: Possible signatures of a bound remnant

The Lowest of the Low: Discovery of SN 2019gsc and the Nature of Faint Iax Supernovae

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