The He-rich stripped-envelope core-collapse supernova 2008ax★

Taubenberger, S.; Navasardyan, H.; Maurer, J.; Zampieri, L.; Чугай, Н. Н.; Benetti, S.; Agnoletto, I.; Bufano, F.; Elias‐Rosa, N.; Turatto, M.; Patat, F.; Cappellaro, E.; Mazzali, P. A.; Iijima, Takashi; Valenti, S.; Harutyunyan, A.; Claudi, R.; Dolci, M.

doi:10.1111/j.1365-2966.2011.18287.x

Cited by 90 publications

(158 citation statements)

References 73 publications

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“…The distance, extinction and the references for the photometric data used for SNe 1993J and2008ax are the same as in E14. The lack of S-corrected photometry for SN 1993J complicates the comparison, whereas for SN 2008ax, the S-corrected Johnson-Cousins (JC) photometry by Taubenberger et al (2011) agrees reasonably well with the JC photometry by Tsvetkov et al (2009).…”

Section: Photometrysupporting

confidence: 65%

The Type IIb SN 2011dh: Two years of observations and modelling of the lightcurves

Ergon

Jerkstrand

Sollerman

et al. 2015

A&A

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We present optical and near-infrared (NIR) photometry and spectroscopy as well as modelling of the lightcurves of the Type IIb supernova (SN) 2011dh. Our extensive dataset, for which we present the observations obtained after day 100, spans two years, and complemented with Spitzer mid-infrared (MIR) data, we use it to build an optical-to-MIR bolometric lightcurve between days 3 and 732. To model the bolometric lightcurve before day 400 we use a grid of hydrodynamical SN models, which allows us to determine the errors in the derived quantities, and a bolometric correction determined with steady-state non-local thermodynamic equilibrium (NLTE) modelling. Using this method we find a helium core mass of 3.1 +0.7 −0.4 M for SN 2011dh, consistent within error bars with previous results obtained using the bolometric lightcurve before day 80. We compute bolometric and broad-band lightcurves between days 100 and 500 from spectral steady-state NLTE models, presented and discussed in a companion paper. The preferred 12 M (initial mass) model, previously found to agree well with the observed spectra, shows a good overall agreement with the observed lightcurves, although some discrepancies exist. Time-dependent NLTE modelling shows that after day ∼600 a steadystate assumption is no longer valid. The radioactive energy deposition in this phase is likely dominated by the positrons emitted in the decay of 56 Co, but seems insufficient to reproduce the lightcurves, and what energy source is dominating the emitted flux is unclear. We find an excess in the K and the MIR bands developing between days 100 and 250, during which an increase in the optical decline rate is also observed. A local origin of the excess is suggested by the depth of the He  20 581 Å absorption. Steady-state NLTE models with a modest dust opacity in the core (τ = 0.44), turned on during this period, reproduce the observed behaviour, but an additional excess in the Spitzer 4.5 µm band remains. Carbon-monoxide (CO) first-overtone band emission is detected at day 206, and possibly at day 89, and assuming the additional excess to be dominated by CO fundamental band emission, we find fundamental to first-overtone band ratios considerably higher than observed in SN 1987A. The profiles of the [O ] 6300 Å and Mg ] 4571 Å lines show a remarkable similarity, suggesting that these lines originate from a common nuclear burning zone (O/Ne/Mg), and using small scale fluctuations in the line profiles we estimate a filling factor of 0.07 for the emitting material. This paper concludes our extensive observational and modelling work on SN 2011dh. The results from hydrodynamical modelling, steady-state NLTE modelling, and stellar evolutionary progenitor analysis are all consistent, and suggest an initial mass of ∼12 M for the progenitor.

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Section: Photometrysupporting

confidence: 65%

The Type IIb SN 2011dh: Two years of observations and modelling of the lightcurves

Ergon

Jerkstrand

Sollerman

et al. 2015

A&A

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“…The bolometric corrections take into account contributions from the UV and IR ranges that can be significant depending on the SN color. We employed the BVRI and g r i ¢ ¢ ¢ light curves published by Pastorello et al (2008), augmented by BVRI observations of Taubenberger et al (2011). Bolometric corrections were derived using the calibrations for…”

Section: Hydrodynamical Modelsmentioning

confidence: 99%

“…He I λ5876 velocities were taken from Chornock et al (2011) and Taubenberger et al (2011), while Fe II λ5169 velocities were obtained from the latter work. Roughly after day 10 since explosion He I λ5876 velocities began to flatten as the photosphere receded beyond the bottom of the He-rich layer.…”

Section: Hydrodynamical Modelsmentioning

confidence: 99%

“…The methodology is the same that we applied in previous analyses of SNe IIb (e.g., see Bersten et al 2012;Bufano et al 2014), i.e., we first derived global parameters focusing on the explosion of H-free structures to fit the main peak of the bolometric light curve and the expansion velocities, and then we used such parameters to analyze the effect on the early light curve of a thin H-rich envelope with different extensions. In order to compare models and observations on the same time frame, we adopted an explosion date of JD = 2,454,528.80 ± 0.15 from Taubenberger et al (2011).…”

Section: Hydrodynamical Modelsmentioning

confidence: 99%

“…With the then available data, the authors selected two out of a series of possible scenarios: a W-R star that retained a small amount of hydrogen, or an interacting binary system. The light curves and spectra indicated a relatively low ejected mass and normal kinetic energy (Pastorello et al 2008;Roming et al 2009;Tsvetkov et al 2009;Maurer et al 2010;Taubenberger et al 2011;Jerkstrand et al 2015). The low mass was generally interpreted as an indication against a single massive W-R progenitor.…”

Section: Introductionmentioning

confidence: 99%

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THE PROGENITOR OF THE TYPE IIb SN 2008ax REVISITED

Folatelli

Bersten

Kuncarayakti

et al. 2015

ApJ

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Hubble Space Telescope observations of the site of the supernova (SN) SN 2008ax obtained in 2011 and 2013 reveal that the possible progenitor object detected in pre-explosion images was in fact multiple. Four point sources are resolved in the new, higher-resolution images. We identify one of the sources with the fading SN. The other three objects are consistent with single supergiant stars. We conclude that their light contaminated the previously identified progenitor candidate. After subtraction of these stars, the progenitor appears to be significantly fainter and bluer than previously measured. Post-explosion photometry at the SN location indicates that the progenitor object has disappeared. If single, the progenitor is compatible with a supergiant star of B to mid-A spectral type, while a Wolf-Rayet (W-R) star would be too luminous in the ultraviolet to account for the observations. Moreover, our hydrodynamical modeling shows that the pre-explosion mass was 4-5 M e and the radius was 30-50 R e , which is incompatible with a W-R progenitor. We present a possible interacting binary progenitor computed with our evolutionary models that reproduces all the observational evidence. A companion star as luminous as an O9-B0 main-sequence star may have remained after the explosion.

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Light Curves of Type II Supernovae

Zampieri¹

2017

Handbook of Supernovae

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The He-rich stripped-envelope core-collapse supernova 2008ax★

Cited by 90 publications

References 73 publications

The Type IIb SN 2011dh: Two years of observations and modelling of the lightcurves

The Type IIb SN 2011dh: Two years of observations and modelling of the lightcurves

THE PROGENITOR OF THE TYPE IIb SN 2008ax REVISITED

Light Curves of Type II Supernovae

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