Mass discrepancy analysis for a select sample of Type II-Plateau supernovae

Martínez, Laureano; Bersten, Melina C.

doi:10.1051/0004-6361/201834818

Cited by 41 publications

(59 citation statements)

References 92 publications

(120 reference statements)

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“…This is consistent with the red supergiant problem inferred from direct progenitor detections, discussed in section 4 (although see Anderson et al 2018 for a reportedly high-mass progenitor case in a low-metallicity environment). Studies of the SN light curve evolution, that primarily constrain the ejecta masses of the event, are in general agreement with the above studies (e.g., Valenti et al 2016;Martinez & Bersten 2019;Eldridge et al 2019).…”

Section: Predicted Discrepancy Of Inferred Initial Masses Of Type II Sn Progenitors Between Different Observational Methodssupporting

confidence: 85%

Effect of binary evolution on the inferred initial and final core masses of hydrogen-rich, Type II supernova progenitors

Zapartas

Mink

Justham

et al. 2020

A&A

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The majority of massive stars, which are the progenitors of core-collapse supernovae (SNe), are found in close binary systems. In a previous work, we modeled the fraction of hydrogen-rich, Type II SN progenitors whose evolution is affected by mass exchange with their companion, finding this to be between ≈1/3 and 1/2 for most assumptions. Here we study in more depth the impact of this binary history of Type II SN progenitors on their final pre-SN core mass distribution, using population synthesis simulations. We find that binary star progenitors of Type II SNe typically end their life with a larger core mass than they would have had if they had lived in isolation because they gained mass or merged with a companion before their explosion. The combination of the diverse binary evolutionary paths typically leads to a marginally shallower final core mass distribution. In discussing our results in the context of the red supergiant problem, that is, the reported lack of detected high luminosity progenitors, we conclude that binary evolution does not seem to significantly affect the issue. This conclusion is quite robust against our variations in the assumptions of binary physics. We also predict that inferring the initial masses of Type II SN progenitors by “age-dating” their surrounding environment systematically yields lower masses compared to methods that probe the pre-SN core mass or luminosity. A robust discrepancy between the inferred initial masses of a SN progenitor from those different techniques could indicate an evolutionary history of binary mass accretion or merging.

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Section: Predicted Discrepancy Of Inferred Initial Masses Of Type II Sn Progenitors Between Different Observational Methodssupporting

confidence: 85%

Effect of binary evolution on the inferred initial and final core masses of hydrogen-rich, Type II supernova progenitors

Zapartas

Mink

Justham

et al. 2020

A&A

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show abstract

“…Smartt et al 2009; and hydrodynamical models (e.g. Bersten, Benvenuto & Hamuy 2011;Dessart et al 2013b;Martinez & Bersten 2019). Although there remain some disagreements (e.g.…”

Section: Progenitor Massmentioning

confidence: 99%

“…Smartt et al 2009; and hydrodynamical models (e.g. Dessart et al 2013b;Martinez & Bersten 2019). However, other studies have suggested the possibility that their progenitors are more massive RSGs with large amounts of fallback material (e.g.…”

mentioning

confidence: 99%

The low-luminosity Type II SN 2016aqf: a well-monitored spectral evolution of the Ni/Fe abundance ratio

Müller-Bravo

Gutiérrez

Sullivan

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Abstract Low-luminosity type II supernovae (LL SNe II) make up the low explosion energy end of core-collapse SNe, but their study and physical understanding remain limited. We present SN 2016aqf, a LL SN II with extensive spectral and photometric coverage. We measure a V-band peak magnitude of −14.58 mag, a plateau duration of ∼100 days, and an inferred 56Ni mass of 0.008 ± 0.002 M⊙. The peak bolometric luminosity, Lbol ≈ 1041.4 erg s−1, and its spectral evolution is typical of other SNe in the class. Using our late-time spectra, we measure the [O i] λλ6300, 6364 lines, which we compare against SN II spectral synthesis models to constrain the progenitor zero-age main-sequence mass. We find this to be 12 ± 3 M⊙. Our extensive late-time spectral coverage of the [Fe ii] λ7155 and [Ni ii] λ7378 lines permits a measurement of the Ni/Fe abundance ratio, a parameter sensitive to the inner progenitor structure and explosion mechanism dynamics. We measure a constant abundance ratio evolution of $0.081^{+0.009}_{-0.010}$, and argue that the best epochs to measure the ratio are at ∼200 – 300 days after explosion. We place this measurement in the context of a large sample of SNe II and compare against various physical, light-curve and spectral parameters, in search of trends which might allow indirect ways of constraining this ratio. We do not find correlations predicted by theoretical models; however, this may be the result of the exact choice of parameters and explosion mechanism in the models, the simplicity of them and/or primordial contamination in the measured abundance ratio.

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“…MESA+STELLA progenitor and light-curve modeling. Recent work 72,98,99,100 highlights the nonuniqueness of bolometric light-curve modeling for extracting explosion characteristics (ejecta mass M ej , explosion energy E exp , and progenitor radius R) from plateau features (in particular, luminosity at day 50, L 50 , and plateau duration, t p ) without an independent prior on one of M ej , E exp , or R. Due to the presumed presence of a dense CSM and its potential influence on the early light curves and velocities, shock-cooling modeling and early expansion velocities cannot simply lift this degeneracy.…”

mentioning

confidence: 99%