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

Müller-Bravo, T. E.; Gutiérrez, C. P.; Sullivan, M.; Jerkstrand, A.; Anderson, J. P.; González–Gaitán, S.; Sollerman, J.; Arcavi, I.; Burke, J.; Galbany, L.; Gal‐Yam, A.; Gromadzki, M.; Hiramatsu, D.; Hosseinzadeh, G.; Howell, D. A.; Inserra, C.; Kankare, E.; Kozyreva, Alexandra; McCully, C.; Nicholl, M.; Smartt, S. J.; Valenti, S.; Young, D. R.

doi:10.1093/mnras/staa1932

Cited by 15 publications

(8 citation statements)

References 99 publications

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“…The method described abo v e was dev eloped to study standard SNe IIP, but it was also applied to LL SNe IIP, when possible. Spectral modelling results are so far consistent with the lack of massive progenitors ( ∼20 M ) for LL SNe IIP (M üller -Bra v o et al 2020 ). Studies on the photometric and spectroscopic evolution of larger samples (up to 15 objects) of LL SNe IIP (Pastorello et al 2004 ;Spiro et al 2014 ) found that these transients share strikingly similar features.…”

Section: Introductionsupporting

confidence: 63%

Low luminosity Type II supernovae – IV. SN 2020cxd and SN 2021aai, at the edges of the sub-luminous supernovae class

Valerin

Pumo

Pastorello

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Photometric and spectroscopic data for two Low Luminosity Type IIP Supernovae (LL SNe IIP) 2020cxd and 2021aai are presented. SN 2020cxd was discovered two days after explosion at an absolute magnitude of Mr = –14.02 ± 0.21 mag, subsequently settling on a plateau which lasts for ∼120 days. Through the luminosity of the late light curve tail, we infer a synthesized 56Ni mass of (1.8±0.5) × 10−3 M⊙. During the early evolutionary phases, optical spectra show a blue continuum (T > 8000 K) with broad Balmer lines displaying a P Cygni profile, while at later phases Ca II, Fe II, Sc II and Ba II lines dominate the spectra. Hydrodynamical modelling of the observables yields R ≃ 575 R⊙ for the progenitor star, with Mej = 7.5 M⊙ and E ≃ 0.097 foe emitted during the explosion. This low–energy event originating from a low–mass progenitor star is compatible with both the explosion of a red supergiant (RSG) star and with an Electron Capture Supernova arising from a super asymptotic giant branch star. SN 2021aai reaches a maximum luminosity of Mr = –16.57 ± 0.23 mag (correcting for AV=1.92 mag), at the end of its remarkably long plateau (∼140 days). The estimated 56Ni mass is (1.4±0.5) × 10−2 M⊙. The expansion velocities are compatible with those of other LL SNe IIP (few 103 km s−1). The physical parameters obtained through hydrodynamical modelling are R ≃ 575 R⊙, Mej = 15.5 M⊙ and E = 0.4 foe. SN 2021aai is therefore interpreted as the explosion of a RSG, with properties that bridge the class of LL SNe IIP with standard SN IIP events.

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Section: Introductionsupporting

confidence: 63%

Low luminosity Type II supernovae – IV. SN 2020cxd and SN 2021aai, at the edges of the sub-luminous supernovae class

Valerin

Pumo

Pastorello

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…ECSNe). Müller-Bravo et al (2020) performed a similar analysis for the low-luminosity Type II SN 2016aqf. They compare SN 2016afq to the models of Jerkstrand et al (2018), which we also compare SN 2018zd to in Fig.…”

Section: Nebular-phase Spectroscopymentioning

confidence: 99%

How low can you go? SN 2018zd as a low-mass Fe core-collapse supernova

Callis¹,

Fraser²,

Pastorello³

et al. 2021

Preprint

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We present spectroscopy and photometry of SN 2018zd, a Type IIP core-collapse supernova with signatures of interaction with circumstantial material in its earliest spectra. High ionization lines, the earmark of shock breakout, are not seen in the earliest spectral epoch, and are only seen in a single spectrum at 4.9 d after explosion. The strength and brevity of these features imply a confined circumstellar material shell in the immediate vicinity of the progenitor. Once the narrow emission lines disappear, SN 2018zd evolves similarly to a Type IIP SN, although the blue colour and enhanced plateau magnitude of SN 2018zd suggests an additional source of luminosity throughout the plateau phase. While SN 2018zd has previously been proposed as an electron-capture SN, we suggest that it is an Fe core-collapse from a low mass red supergiant progenitor. Differences in interpretation for SN 2018zd arise in part due to the large uncertainty on the distance to the host-galaxy NGC 2146, which we re-derive here to be 15.6 +6.1 −3.0 Mpc. We find the ejected 56 Ni mass for SN 2018zd to be 0.017 M , significantly higher than models of ECSNe predict. We also find the Ni/Fe ratio in SN 2018zd to be much lower that would be expected for an ECSN.

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“…The spectral features mentioned so far are extensively observed in LL SNe (Pastorello et al 2004;Spiro et al 2014;Müller-Bravo et al 2020;Reguitti et al 2021). The presence of a relevant amount of metals gives rise to "line blanketing", where the flux in the bluest part of the spectrum is reduced by the metal absorption lines (see e.g.…”

Section: Spectroscopic Featuresmentioning

confidence: 94%

“…Thereafter, the brightness consistently increased to 𝑀 𝑔 = -13.58 mag and 𝑀 𝑟 = -14.48 mag before finally fading from the plateau at ∼120 days. Müller-Bravo et al (2020) attributed the different behaviour of the 𝑔 band compared to the 𝑟 band to the shift of the Spectral Energy Distribution (SED) peak from the ultraviolet (UV) to the optical domain. The drop from the plateau was very sharp, with the object fading by 2.9 mag in the 𝑟 band and 3.2 mag in the 𝑔 band in just 10 days.…”

Section: Sn 2020cxd Photometric Propertiesmentioning

confidence: 99%

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Low luminosity Type II supernovae -- IV. SN 2020cxd and SN 2021aai, at the edges of the sub-luminous supernovae class

Valerin,

Pumo,

Pastorello

et al. 2022

Preprint

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Photometric and spectroscopic data for two Low Luminosity Type IIP Supernovae (LL SNe IIP) are presented. SN 2020cxd reaches a peak absolute magnitude 𝑀 𝑟 = -13.90 ± 0.05 mag two days after explosion, subsequently settling on a plateau for ∼120 days. Through the luminosity of the late light curve tail, we infer a synthesized 56 Ni mass of (1.8±0.5) × 10 −3 M . During the early evolutionary phases, optical spectra show a blue continuum (𝑇 > 8000 K) with broad Balmer lines displaying a P Cygni profile, while at later phases Ca II, Fe II, Sc II and Ba II lines dominate the spectra. Hydrodynamical modelling of the observables yields 𝑅 575 𝑅 for the progenitor star, with 𝑀 𝑒 𝑗 = 7.5 M and 𝐸 0.097 foe emitted during the explosion. This low-energy event originating from a low-mass progenitor star is compatible with both the explosion of a red supergiant (RSG) star and with an Electron Capture Supernova arising from a super asymptotic giant branch star. SN 2021aai reaches a maximum luminosity of 𝑀 𝑟 = -16.4 mag (correcting for 𝐴 𝑉 =1.9 mag), and displays a remarkably long plateau (∼140 days). The estimated 56 Ni mass is (1.4±0.5) × 10 −2 M . The expansion velocities are compatible with those of other LL SNe IIP (few 10 3 km s −1 ). The physical parameters obtained through hydrodynamical modelling are 𝑅 575 R , 𝑀 𝑒 𝑗 = 15.5 M and 𝐸 = 0.4 foe. SN 2021aai is therefore interpreted as the explosion of a RSG, with properties that bridge the class of LL SNe IIP with standard SN IIP events.

show abstract

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

Cited by 15 publications

References 99 publications

Low luminosity Type II supernovae – IV. SN 2020cxd and SN 2021aai, at the edges of the sub-luminous supernovae class

Low luminosity Type II supernovae – IV. SN 2020cxd and SN 2021aai, at the edges of the sub-luminous supernovae class

How low can you go? SN 2018zd as a low-mass Fe core-collapse supernova

Low luminosity Type II supernovae -- IV. SN 2020cxd and SN 2021aai, at the edges of the sub-luminous supernovae class

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