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

Valerin, G.; Pumo, M. L.; Pastorello, A.; Reguitti, A.; Elias‐Rosa, N.; Gutiérrez, C. P.; Kankare, E.; Fraser, M.; Mazzali, Paolo A.; Howell, D. A.; Kotak, R.; Galbany, L.; Williams, S. C.; Cai, Yongzhi; Salmaso, I.; Pintėr, V.; Müller-Bravo, T. E.; Burke, J.; González, E. P.; Hiramatsu, D.; McCully, C.; Newsome, Megan; Pellegrino, C.

doi:10.1093/mnras/stac1182

Cited by 14 publications

(10 citation statements)

References 91 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The spectral evolution of SN 2018lab is similar to that of other LLSNe presented in previous papers (e.g., Benetti et al 2001;Pastorello et al 2004Pastorello et al , 2009Spiro et al 2014;Takáts et al 2014;Lisakov et al 2017;Valerin et al 2022). The first four spectra (7 days) exhibit a blue continuum and the slow emergence of Balmer lines and He I λ5876, as is typical of all SNe II.…”

Section: Spectral Evolutionsupporting

confidence: 84%

“…Electron-capture (EC) SNe, the result of O-Ne-Mg CC in super-asymptotic giant branch (AGB) stars, have also been used to explain the properties of some LLSNe (Hosseinzadeh et al 2018;Valerin et al 2022). Some models predict that ECSNe can appear nearly identical to LL-CCSNe (Nomoto 1984;Kitaura et al 2006;Poelarends et al 2008) and their progenitors lie in the same mass range (super-AGB stars 8-10 M e ; Kitaura et al 2006) as low-mass RSGs which undergo CC.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Circumstellar Medium Interaction in SN 2018lab, A Low-luminosity Type IIP Supernova Observed with TESS

Hosseinzadeh

Sand

Andrews

et al. 2023

ApJ

View full text Add to dashboard Cite

We present photometric and spectroscopic data of SN 2018lab, a low-luminosity Type IIP supernova (LLSN) with a V-band peak luminosity of −15.1 ± 0.1 mag. SN 2018lab was discovered by the Distance Less Than 40 Mpc (DLT40) SN survey only 0.73 days post-explosion, as determined by observations from the Transiting Exoplanet Survey Satellite (TESS). TESS observations of SN 2018lab yield a densely sampled, fast-rising, early-time light curve likely powered by ejecta–circumstellar medium (CSM) interaction. The blueshifted, broadened flash feature in the earliest spectra (<2 days) of SN 2018lab provides further evidence for ejecta–CSM interaction. The early emission features in the spectra of SN 2018lab are well described by models of a red supergiant progenitor with an extended envelope and a close-in CSM. As one of the few LLSNe with observed flash features, SN 2018lab highlights the need for more early spectra to explain the diversity of the flash feature morphology of Type II SNe.

show abstract

Section: Spectral Evolutionsupporting

confidence: 84%

Section: Introductionmentioning

confidence: 99%

Circumstellar Medium Interaction in SN 2018lab, A Low-luminosity Type IIP Supernova Observed with TESS

Hosseinzadeh

Sand

Andrews

et al. 2023

ApJ

View full text Add to dashboard Cite

show abstract

“…In particular, the light curve luminosity seems to be correlated with some spectral parameters, such as the Hα luminosity (L Hα ) and the Hα FWHM velocity (v FWHM ). They inferred a general trend according to which brighter events have higher L Hα and v FWHM (Hα ) (see the analysis in Pastorello et al (2022), in preparation; and their Fig. 17) Furthermore, the luminosity of the light curve is tightly correlated with that of the progenitor.…”

Section: Discussion and Concluding Remarksmentioning

confidence: 95%

“…5); the Hα emission line becomes quite weak, and at the same time a forest of metal lines in absorption appears (see Figs. 6 and 8), as in some low-luminosity SNe IIP (e.g., Pastorello et al 2004Pastorello et al , 2006Pastorello et al , 2009Spiro et al 2014;Hosseinzadeh et al 2018;Müller-Bravo et al 2020;Reguitti et al 2021;Valerin et al 2022;Zhang et al 2022).…”

Section: Discussion and Concluding Remarksmentioning

confidence: 96%

Observations of the luminous red nova AT 2021biy in the nearby galaxy NGC 4631

Cai¹,

Pastorello²,

Fraser³

et al. 2022

Preprint

View full text Add to dashboard Cite

We present an observational study of the luminous red nova (LRN) AT 2021biy in the nearby galaxy NGC 4631. The field of the object was routinely imaged during the pre-eruptive stage by synoptic surveys, but the transient was detected only at a few epochs from ∼ 231 days before maximum brightness. The LRN outburst was monitored with unprecedented cadence both photometrically and spectroscopically. AT 2021biy shows a short-duration blue peak, with a bolometric luminosity of ∼ 1.6 × 10 41 erg s −1 , followed by the longest plateau among LRNe to date, with a duration of 210 days. A late-time hump in the light curve was also observed, possibly produced by a shell-shell collision. AT 2021biy exhibits the typical spectral evolution of LRNe. Early-time spectra are characterised by a blue continuum and prominent H emission lines. Then, the continuum becomes redder, resembling that of a K-type star with a forest of metal absorption lines during the plateau phase. Finally, late-time spectra show a very red continuum (T BB ≈ 2050 K) with molecular features (e.g., TiO) resembling those of M-type stars. Spectropolarimetric analysis indicates that AT 2021biy has local dust properties similar to those of V838 Mon in the Milky Way Galaxy. Inspection of archival Hubble Space Telescope data taken on 2003 August 3 reveals a ∼ 20 M progenitor candidate with log (L/L ) = 5.0 dex and T eff = 5900 K at solar metallicity. The above luminosity and colour match those of a luminous yellow supergiant. Most likely, this source is a close binary, with a 17-24 M primary component.

show abstract

Section: Discussion and Concluding Remarksmentioning

confidence: 94%

Forbidden hugs in pandemic times

Cai

Pastorello

Fraser

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

We present an observational study of the luminous red nova (LRN) AT 2021biy in the nearby galaxy NGC 4631. The field of the object was routinely imaged during the pre-eruptive stage by synoptic surveys, but the transient was detected only at a few epochs from ∼231 days before maximum brightness. The LRN outburst was monitored with unprecedented cadence both photometrically and spectroscopically. AT 2021biy shows a short-duration blue peak, with a bolometric luminosity of ∼1.6 × 1041 erg s−1, followed by the longest plateau among LRNe to date, with a duration of 210 days. A late-time hump in the light curve was also observed, possibly produced by a shell-shell collision. AT 2021biy exhibits the typical spectral evolution of LRNe. Early-time spectra are characterised by a blue continuum and prominent H emission lines. Then, the continuum becomes redder, resembling that of a K-type star with a forest of metal absorption lines during the plateau phase. Finally, late-time spectra show a very red continuum (TBB ≈ 2050 K) with molecular features (e.g., TiO) resembling those of M-type stars. Spectropolarimetric analysis indicates that AT 2021biy has local dust properties similar to those of V838 Mon in the Milky Way Galaxy. Inspection of archival Hubble Space Telescope data taken on 2003 August 3 reveals a ∼20 M⊙ progenitor candidate with log (L/L⊙) = 5.0 dex and Teff = 5900 K at solar metallicity. The above luminosity and colour match those of a luminous yellow supergiant. Most likely, this source is a close binary, with a 17–24 M⊙ primary component.

show abstract

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

Cited by 14 publications

References 91 publications

Circumstellar Medium Interaction in SN 2018lab, A Low-luminosity Type IIP Supernova Observed with TESS

Circumstellar Medium Interaction in SN 2018lab, A Low-luminosity Type IIP Supernova Observed with TESS

Observations of the luminous red nova AT 2021biy in the nearby galaxy NGC 4631

Forbidden hugs in pandemic times

Contact Info

Product

Resources

About