Type Ic supernova of a 22 M⊙ progenitor

Teffs, Jacob; Ertl, Thomas; Mazzali, Paolo A.; Hachinger, Stephan; Janka, Thomas

doi:10.1093/mnras/staa123

Cited by 25 publications

(36 citation statements)

References 59 publications

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“…The values for the ejecta mass and kinetic energy produced by the PM13 method are much higher than those predicted by the Arnett-like model, as expected due to the contribution of the helium envelope and the effect of having similar optical opacities. However, the ejecta mass derived from the PM13 method matches the value obtained by comparing the spectra of SN 2020cpg with the spectral models of Teffs et al (2020), although the kinetic energy given by the modelling is lower than that predicted using the method from PM13.…”

Section: Re-scaled Light Curvessupporting

confidence: 58%

“…When compared to the ejecta masses of the H-rich SE-SNe, SN 2020cpg lies in the region that has been associated with an extended progenitor. As the ejecta mass obtained using the comparative method of PM13 and the spectral modelling of Teffs et al (2020) are in close agreement, we take the PM13 method as a valid replacement for the Arnett-like model to obtain the ejecta mass when dealing with SE-SNe. The PM13 method will also improve in the future as more SE-SNe undergo hydrodynamical modelling.…”

Section: Re-scaled Light Curvesmentioning

confidence: 96%

“…By comparing the spectra of SN 2020cpg with model spectra, we can gain insight on the potential elemental composition of the outer layers prior to explosion. Teffs et al (2020) calculated a set of synthetic SE-SNe models based on a single mass progenitor, with varying degrees of H/He stripping that produces several Type Ic/Ib/IIb analogue SNe. Teffs et al (2020) estimated the energy of a set of well observed Type IIb SNe by comparing synthetic and observed spectra at pre-, near-and post-peak luminosities.…”

Section: Model Comparisonsmentioning

confidence: 99%

“…The pre-and near-peak spectra of SN 2020cpg are very blue and with few strong features. The early synthetic Type IIb-like spectra in Teffs et al (2020) are typically redder due to a stronger amount of Fe-group elements mixing, producing strong line blocking in the near UV. As such, the conditions in which the early spectra of SN 2020cpg are produced are beyond the scope of this comparison and can be explored in future work.…”

Section: Model Comparisonsmentioning

confidence: 99%

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SN 2020cpg: an energetic link between Type IIb and Ib supernovae

Medler

Mazzali

Teffs

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Stripped-envelope supernovae (SE-SNe) show a wide variety of photometric and spectroscopic properties. This is due to the different potential formation channels and the stripping mechanism that allows for a large diversity within the progenitors outer envelop compositions. Here, the photometric and spectroscopic observations of SN 2020cpg covering ∼130 days from the explosion date are presented. SN 2020cpg (z = 0.037) is a bright SE-SNe with the B-band peaking at MB = −17.75 ± 0.39 mag and a maximum pseudo-bolometric luminosity of Lmax = 6.03 ± 0.01 × 1042 erg s−1. Spectroscopically, SN 2020cpg displays a weak high and low velocity H α feature during the photospheric phase of its evolution, suggesting that it contained a detached hydrogen envelope prior to explosion. From comparisons with spectral models, the mass of hydrogen within the outer envelope was constrained to be ∼ 0.1 M⊙ . From the pseudo-bolometric light curve of SN 2020cpg a 56Ni mass of MNi ∼ 0.27 ± 0.08 M⊙ was determined using an Arnett-like model. The ejecta mass and kinetic energy of SN 2020cpg were determined using an alternative method that compares the light curve of SN 2020cpg and several modelled SE-SNe, resulting in an ejecta mass of Mejc ∼ 5.5 ± 2.0 M⊙ and a kinetic energy of EK ∼ 9.0 ± 3.0 × 1051 erg. The ejected mass indicates a progenitor mass of 18 − 25 M⊙. The use of the comparative light curve method provides an alternative process to the commonly used Arnett-like model to determine the physical properties of SE-SNe.

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Section: Re-scaled Light Curvessupporting

confidence: 58%

Section: Re-scaled Light Curvesmentioning

confidence: 96%

Section: Model Comparisonsmentioning

confidence: 99%

Section: Model Comparisonsmentioning

confidence: 99%

See 2 more Smart Citations

SN 2020cpg: an energetic link between Type IIb and Ib supernovae

Medler

Mazzali

Teffs

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…The code has been used to model the light curves of many Type I SNe, both Ia and Ib/c (e.g. Mazzali et al 2017;Teffs et al 2020).…”

Section: Light Curve Modelmentioning

confidence: 99%

Modelling of SN2013dx associated with the low-redshift GRB130702A points to diversity in GRB/SN properties

Mazzali,

Pian,

Bufano

et al. 2021

Preprint

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The properties of the broad-lined type Ic supernova (SN) 2013dx, associated with the long gamma-ray burst GRB 130702A at a redshift z = 0.145, are derived via spectral modelling. SN 2013dx was similar in luminosity to other GRB/SNe, with a derived value of the mass of 56 Ni ejected in the explosion of ≈ 0.4 M . However, its spectral properties suggest a smaller explosion kinetic energy. Radiation transport models were used to derive a plausible mass and density distribution of the SN ejecta in a one-dimensional approximation. While the mass ejected in the explosion that is obtained from the modelling (M ej ≈ 9 M ) is similar to that of all other well-studied GRB/SNe, the kinetic energy is significantly smaller (E K ∼ 10 52 erg). This leads to a smaller E K /M ej ratio, ≈ 10 51 erg/M , which is reflected in the narrower appearance of the spectral lines. While the low E K does not represent a problem for the scenario in which magnetar energy aids powering the explosion and the nucleosynthesis, it is nevertheless highly unusual. SNe Ic with similar E K have never been seen in coincidence with a GRB, and no well-observed GRB/SN has shown similarly low E K and E K /M ej .

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Systematic investigation of the effect of 56Ni mixing in the early photospheric velocity evolution of stripped-envelope supernovae

Moriya

Suzuki

Takiwaki

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Mixing of 56Ni, whose nuclear decay energy is a major luminosity source in stripped-envelope supernovae, is known to affect the observational properties of stripped-envelope supernovae such as light-curve and colour evolution. Here we systematically investigate the effect of 56Ni mixing on the photospheric velocity evolution in stripped-envelope supernovae. We show that 56Ni mixing significantly affects the early photospheric velocity evolution. The photospheric velocity, which is often used to constrain the ejecta mass and explosion energy, significantly varies by just changing the degree of 56Ni mixing. In addition, the models with a small degree of 56Ni mixing show a flattening in the early photospheric velocity evolution, while the fully mixed models show a monotonic decrease. The velocity flattening appears in both helium and carbon+oxygen progenitor explosions with a variety of ejecta mass, explosion energy, and 56Ni mass. Some stripped-envelope supernovae with early photospheric velocity information do show such a flattening. We find that Type Ib SN 2007Y, which has early photospheric velocity information, has a signature of a moderate degree of 56Ni mixing in the photospheric velocity evolution and about half of the ejecta is mixed in it. The immediate spectroscopic follow-up observations of stripped-envelope supernovae shortly after the explosion providing the early photospheric evolution give an important clue to constrain 56Ni mixing in the ejecta.

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Type Ic supernova of a 22 M⊙ progenitor

Cited by 25 publications

References 59 publications

SN 2020cpg: an energetic link between Type IIb and Ib supernovae

SN 2020cpg: an energetic link between Type IIb and Ib supernovae

Modelling of SN2013dx associated with the low-redshift GRB130702A points to diversity in GRB/SN properties

Systematic investigation of the effect of 56Ni mixing in the early photospheric velocity evolution of stripped-envelope supernovae

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