SN 2018hfm: a low-energy Type II supernova with prominent signatures of circumstellar interaction and dust formation

Zhang, Xinghan; Sai, Hanna; Niculescu-Duvaz, Maria; Filippenko, A. V.; Zheng, W.; Brink, Thomas G.; Lin, Han; Zhang, Jicheng; Cai, Yongzhi; Mo, Jun; Zhang, Jujia; Baron, Edward; DerKacy, James M.; Huang, Fang; Zhang, T. M.

doi:10.1093/mnras/stab3007

Cited by 11 publications

(5 citation statements)

References 85 publications

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“…With the increasing number of SNe observed early enough, the fraction of SNe showing flash ionization features is also increasing (>36%, Bruch et al 2023), indicating the presence of CSM close to the explosion site is common in Type II SNe (Morozova et al 2018). Other observational features such as narrow emission lines, high-velocity (HV) absorption features in spectra, and enhanced luminosity in light curves (Bullivant et al 2018;Singh et al 2019;Zhang et al 2022) also reveal the presence of spatially confined CSM, most probably originating from enhanced mass loss from the progenitor shortly prior to the explosion.…”

Section: Introductionmentioning

confidence: 99%

“…The evidence of CSM in Type IIP is usually seen early on with ionized lines, narrow emission lines, HV absorption features in spectra, and enhanced luminosity in light curves (Bullivant et al 2018;Singh et al 2019;Zhang et al 2022). Furthermore, it has been established that sometimes only a few of these features are present while others are missing altogether (Andrews et al 2019;Dong et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission

Teja,

Singh,

Sahu

et al. 2023

ApJ

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We present an extensive, panchromatic photometric (UV, optical, and near-IR) and low-resolution optical spectroscopic coverage of a Type IIP supernova SN 2018gj that occurred on the outskirts of the host galaxy NGC 6217. From the V-band light curve, we estimate the plateau length to be ∼ 70 ± 2 days, placing it among the very few well-sampled short plateau supernovae (SNe). With V-band peak absolute magnitude M V ≤ −17.0 ± 0.1 mag, it falls in the middle of the luminosity distribution of the Type II SNe. The color evolution is typical to other Type II SNe except for an early elbow-like feature in the evolution of V − R color owing to its early transition from the plateau to the nebular phase. Using the expanding photospheric method, we present an independent estimate of the distance to SN 2018gj. We report the spectral evolution to be typical of a Type II SNe. However, we see a persistent blueshift in emission lines until the late nebular phase, not ordinarily observed in Type II SNe. The amount of radioactive nickel (56Ni) yield in the explosion was estimated to be 0.026 ± 0.007 M ⊙. We infer from semianalytical modeling, nebular spectrum, and 1D hydrodynamical modeling that the probable progenitor was a red supergiant with a zero-age-main-sequence mass ≤13 M ⊙. In the simulated hydrodynamical model light curves, reproducing the early optical bolometric light curve required an additional radiation source, which could be the interaction with the proximal circumstellar matter.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission

Teja,

Singh,

Sahu

et al. 2023

ApJ

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“…Dust formation is common in SNe IIP (e.g. Be v an & Barlow 2016 ; Niculescu-Duvaz et al 2022 ;Zhang et al 2022 ). Newly formed dust within the ejecta of SNe can cause a deficit in the red side of the emission lines and produce blueshifted peaks.…”

Section: A P P E N D I X B : D U S T F O R M At I O Nmentioning

confidence: 99%

SN 2018hna: Adding a piece to the puzzles of the explosion of blue supergiants

Xiang

Zhang

Sai

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present extensive optical/ultraviolet observations and modelling analysis for the nearby SN 1987A-like peculiar Type II supernova (SN) 2018hna. Both photometry and spectroscopy covered phases extending to >500 days after the explosion, making it one of the best-observed SN II of this subtype. SN 2018hna is obviously bluer than SN 1987A during the photospheric phase, suggesting higher photospheric temperature, which may account for weaker Ba ii λ6142 lines in its spectra. Analysis of early-time temperature evolution suggests a radius of ∼45 R⊙ for the progenitor of SN 2018hna, consistent with a blue supergiant (BSG). By fitting the bolometric light curve with hydrodynamical models, we find that SN 2018hna has an ejecta mass of ∼(13.7–17.7) M⊙, a kinetic energy of ∼ (1.0–1.2) × 1051 erg, and a 56Ni mass of about 0.05 M⊙. Moreover, based on standard stellar evolution and the oxygen mass (0.44–0.73 M⊙) deduced from nebular [O i] lines, the progenitor of SN 2018hna is expected to have an initial main-sequence mass <16 M⊙. In principle, such a relatively low-mass star cannot end as a BSG just before core-collapse, except some unique mechanisms are involved, such as rapid rotation, restricted semiconvection, etc. On the other hand, binary scenario may be more favourable, like in the case of SN 1987A. While the much lower oxygen mass inferred for SN 2018hna may imply that its progenitor system also had much lower initial masses than that of SN 1987A.

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“…Dust formation is common in SNe IIP (e.g., Bevan & Barlow 2016;Niculescu-Duvaz et al 2022;Zhang et al 2022). Newly formed dust within the ejecta of SNe can cause a deficit in the red side of the emission lines and produce blueshifted peaks.…”

Section: Data Availabilitymentioning

confidence: 99%

SN 2018hna: Adding a Piece to the Puzzles of the Explosion of Blue Supergiants

Xiang¹,

Zhang²,

Sai³

et al. 2023

Preprint

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We present extensive optical/ultraviolet observations and modelling analysis for the nearby SN 1987A-like peculiar Type II supernova (SN) 2018hna. Both photometry and spectroscopy covered phases extending to >500 days after the explosion, making it one of the best-observed SN II of this subtype. SN 2018hna is obviously bluer than SN 1987A during the photospheric phase, suggesting higher photospheric temperature, which may account for weaker Ba 𝜆6142 lines in its spectra. Analysis of early-time temperature evolution suggests a radius of ∼45 R for the progenitor of SN 2018hna, consistent with a blue supergiant (BSG). By fitting the bolometric light curve with hydrodynamical models, we find that SN 2018hna has an ejecta mass of ∼(13.7-17.7) M , a kinetic energy of ∼ (1.0-1.2) ×10 51 erg, and a 56 Ni mass of about 0.05 M . Moreover, based on standard stellar evolution and the oxygen mass (0.44-0.73 M ) deduced from nebular [O ] lines, the progenitor of SN 2018hna is expected to have an initial main-sequence mass <16 M . In principle, such a relatively low-mass star cannot end as a BSG just before core-collapse, except some unique mechanisms are involved, such as rapid rotation, restricted semiconvection, etc. On the other hand, binary scenario may be more favourable, like in the case of SN 1987A. While the much lower oxygen mass inferred for SN 2018hna may imply that its progenitor system also had much lower initial masses than that of SN 1987A.

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SN 2018hfm: a low-energy Type II supernova with prominent signatures of circumstellar interaction and dust formation

Cited by 11 publications

References 85 publications

SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission

SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission

SN 2018hna: Adding a piece to the puzzles of the explosion of blue supergiants

SN 2018hna: Adding a Piece to the Puzzles of the Explosion of Blue Supergiants

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