Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae

Pessi, P. J.; Folatelli, G.; Anderson, J. P.; Bersten, Melina C.; Burns, C. R.; Contreras, C.; Davis, Scott; Englert, Berthold-Georg; Hamuy, M.; Hsiao, E. Y.; Martínez, Laureano; Morrell, N.; Phillips, M. M.; Suntzeff, Nicholas B.; Stritzinger, M. D.

doi:10.1093/mnras/stz1855

Cited by 31 publications

(33 citation statements)

References 112 publications

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“…Filippenko et al 1993). A recent study analysed the possible existence of a continuum between the SNe II and IIb in terms of their photometric properties (Pessi et al 2019). However, these latter authors found clear differences between the two subgroups.…”

Section: Introductionmentioning

confidence: 99%

Progenitor properties of type II supernovae: fitting to hydrodynamical models using Markov chain Monte Carlo methods

Martínez

Bersten

Anderson

et al. 2020

A&A

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Context. The progenitor and explosion properties of type II supernovae (SNe II) are fundamental to understanding the evolution of massive stars. Particular attention has been paid to the initial masses of their progenitors, but despite the efforts made, the range of initial masses is still uncertain. Direct imaging of progenitors in pre-explosion archival images suggests an upper initial mass cutoff of ∼18 M⊙. However, this is in tension with previous studies in which progenitor masses inferred by light-curve modelling tend to favour high-mass solutions. Moreover, it has been argued that light-curve modelling alone cannot provide a unique solution for the progenitor and explosion properties of SNe II. Aims. We develop a robust method which helps us to constrain the physical parameters of SNe II by simultaneously fitting their bolometric light curve and the evolution of the photospheric velocity to hydrodynamical models using statistical inference techniques. Methods. We created pre-supernova red supergiant models using the stellar evolution code MESA, varying the initial progenitor mass. We then processed the explosion of these progenitors through hydrodynamical simulations, where we changed the explosion energy and the synthesised nickel mass together with its spatial distribution within the ejecta. We compared the results to observations using Markov chain Monte Carlo methods. Results. We apply this method to a well-studied set of SNe with an observed progenitor in pre-explosion images and compare with results in the literature. Progenitor mass constraints are found to be consistent between our results and those derived by pre-SN imaging and the analysis of late-time spectral modelling. Conclusions. We have developed a robust method to infer progenitor and explosion properties of SN II progenitors which is consistent with other methods in the literature. Our results show that hydrodynamical modelling can be used to accurately constrain the physical properties of SNe II. This study is the starting point for a further analysis of a large sample of hydrogen-rich SNe.

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Section: Introductionmentioning

confidence: 99%

Progenitor properties of type II supernovae: fitting to hydrodynamical models using Markov chain Monte Carlo methods

Martínez

Bersten

Anderson

et al. 2020

A&A

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“…Later on, Faran et al (2014), analysing a sample of fast-declining SNe II, found that SNe IIL seem to be photometrically related to SNe IIb. More recently, Pessi et al (2019), using a larger sample of SNe (73 SNe II and 22 SNe IIb), found a lack of events that bridge the observed properties of these two classes, concluding that they form two observationally distinct families.…”

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confidence: 99%

SN 2017ivv: two years of evolution of a transitional Type II supernova

Gutiérrez

Pastorello

Jerkstrand

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the photometric and spectroscopic evolution of the type II supernova (SN II) SN 2017ivv (also known as ASASSN-17qp). Located in an extremely faint galaxy (Mr = −10.3 mag), SN 2017ivv shows an unprecedented evolution during the two years of observations. At early times, the light curve shows a fast rise (∼6 − 8 days) to a peak of ${\rm M}^{\rm max}_{g}= -17.84$ mag, followed by a very rapid decline of 7.94 ± 0.48 mag per 100 days in the V −band. The extensive photometric coverage at late phases shows that the radioactive tail has two slopes, one steeper than that expected from the decay of 56Co (between 100 and 350 days), and another slower (after 450 days), probably produced by an additional energy source. From the bolometric light curve, we estimated that the amount of ejected 56Ni is ∼0.059 ± 0.003 M⊙. The nebular spectra of SN 2017ivv show a remarkable transformation that allows the evolution to be split into three phases: (1) Hα strong phase (<200 days); (2) Hα weak phase (between 200 and 350 days); and (3) Hα broad phase (>500 days). We find that the nebular analysis favours a binary progenitor and an asymmetric explosion. Finally, comparing the nebular spectra of SN 2017ivv to models suggests a progenitor with a zero-age main-sequence mass of 15 – 17 M⊙.

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“…DES14X2fna rises to peak in the r band in 18 d, similar to ASASSN-18am and SN 2011hs and fairly typical for SNe IIb based on the sample of SN IIb rise times presented in fig. 4 of Pessi et al (2019). After rising to maximum, DES14X2fna declines at a similar rate to ASASSN-18am until ∼30 d after explosion, after which DES14X2fna begins to decline far more rapidly.…”

Section: Photometrymentioning

confidence: 71%

Understanding the extreme luminosity of DES14X2fna

Grayling

Gutiérrez

Sullivan

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present DES14X2fna, a high-luminosity, fast-declining type IIb supernova (SN IIb) at redshift z = 0.0453, detected by the Dark Energy Survey (DES). DES14X2fna is an unusual member of its class, with a light curve showing a broad, luminous peak reaching Mr ≃ −19.3 mag 20 days after explosion. This object does not show a linear decline tail in the light curve until ≃60 days after explosion, after which it declines very rapidly (4.30 ± 0.10 mag 100 d−1 in r-band). By fitting semi-analytic models to the photometry of DES14X2fna, we find that its light curve cannot be explained by a standard 56Ni decay model as this is unable to fit the peak and fast tail decline observed. Inclusion of either interaction with surrounding circumstellar material or a rapidly-rotating neutron star (magnetar) significantly increases the quality of the model fit. We also investigate the possibility for an object similar to DES14X2fna to act as a contaminant in photometric samples of SNe Ia for cosmology, finding that a similar simulated object is misclassified by a recurrent neural network (RNN)-based photometric classifier as a SN Ia in ∼1.1-2.4 per cent of cases in DES, depending on the probability threshold used for a positive classification.

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Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae

Cited by 31 publications

References 112 publications

Progenitor properties of type II supernovae: fitting to hydrodynamical models using Markov chain Monte Carlo methods

Progenitor properties of type II supernovae: fitting to hydrodynamical models using Markov chain Monte Carlo methods

SN 2017ivv: two years of evolution of a transitional Type II supernova

Understanding the extreme luminosity of DES14X2fna

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