Supernova 2018cuf: A Type IIP Supernova with a Slow Fall from Plateau

Dong, Yize; Valenti, S.; Bostroem, K. A.; Sand, David J.; Andrews, Jennifer E.; Galbany, L.; Eweis, Y.; Kwok, Lindsey A.; Hsiao, E. Y.; Davis, Scott; Brown, P. J.; Kuncarayakti, H.; Maeda, Keiichi; Rho, Jeonghee; Amaro, R.; Anderson, J. P.; Arcavi, I.; Burke, J.; Dastidar, Raya; Folatelli, G.; Haislip, J.; Hiramatsu, D.; Hosseinzadeh, G.; Howell, D. A.; Jencson, J.; Kouprianov, V. V.; Lundquist, M.; Lyman, J. D.; McCully, C.; Misra, Kuntal; Reichart, D.; Sánchez, S. F.; Smith, Nathan; Wang, Xiaofeng; Wang, Lingzhi; Wyatt, S.

doi:10.3847/1538-4357/abc417

Cited by 17 publications

(13 citation statements)

References 121 publications

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“…While the flash ionization features are ephemeral, CSM interaction can produce excess flux in the light curve of the SN up to ∼month post-explosion. Such early-time bolometric luminosity excess has been observed in many CCSNe, including the nearby and wellstudied SNe 2017eaw (Morozova et al 2020 ) and 2018cuf (Dong et al 2021 ). In some events, like SN 2017gmr (Andrews et al 2019 ), the excess flux from the CSM can be present without early-time flash ionization features.…”

Section: Introductionmentioning

confidence: 86%

“…In addition to photometric evidence, there is also spectroscopic evidence of high-velocity absorption features from hydrogen and helium caused by the continuous excitation of the outermost ejecta by ongoing CSM interactions (Chugai, Che v alier & Utrobin 2007 ) in many SNe II-P (SNe II with a luminosity plateau) (e.g. Guti érrez et al 2017 ;Dastidar et al 2019 ;Davis et al 2019 ;Tinyanont et al 2019a ;Dong et al 2021 ). Because SNe II-P are explosions of normal RSGs (see re vie w by Smartt 2009 ), the ubiquity of CSM interaction in SNe II-P indicates enhanced mass-loss in these stars towards the end of their life, perhaps due to the instability in late-stage nuclear burning (Quataert & Shiode 2012 ;Fuller 2017 ).…”

Section: Introductionmentioning

confidence: 99%

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Progenitor and close-in circumstellar medium of type II supernova 2020fqv from high-cadence photometry and ultra-rapid UV spectroscopy

Tinyanont

Ridden-Harper

Foley

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present observations of SN 2020fqv, a Virgo-cluster Type II core-collapse supernova (CCSN) with a high temporal resolution light curve from the Transiting Exoplanet Survey Satellite (TESS) covering the time of explosion; ultraviolet (UV) spectroscopy from the Hubble Space Telescope (HST) starting 3.3 days post-explosion; ground-based spectroscopic observations starting 1.1 days post-explosion; along with extensive photometric observations. Massive stars have complicated mass-loss histories leading up to their death as CCSNe, creating circumstellar medium (CSM) with which the SNe interact. Observations during the first few days post-explosion can provide important information about the mass-loss rate during the late stages of stellar evolution. Model fits to the quasi-bolometric light curve of SN 2020fqv reveal 0.23 M⊙ of CSM confined within 1450 R⊙ (1014 cm) from its progenitor star. Early spectra (<4 days post-explosion), both from HST and ground-based observatories, show emission features from high-ionization metal species from the outer, optically thin part of this CSM. We find that the CSM is consistent with an eruption caused by the injection of ∼5 × 1046 erg into the stellar envelope ∼300 days pre-explosion, potentially from a nuclear burning instability at the onset of oxygen burning. Light-curve fitting, nebular spectroscopy, and pre-explosion HST imaging consistently point to a red supergiant (RSG) progenitor with MZAMS ≈ 13.5–15 M⊙, typical for SN II progenitor stars. This finding demonstrates that a typical RSG, like the progenitor of SN 2020fqv, has a complicated mass-loss history immediately before core collapse.

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Section: Introductionmentioning

confidence: 86%

Section: Introductionmentioning

confidence: 99%

Progenitor and close-in circumstellar medium of type II supernova 2020fqv from high-cadence photometry and ultra-rapid UV spectroscopy

Tinyanont

Ridden-Harper

Foley

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…We note that it is also possible to investigate the effects of the circumstellar medium (CSM) on the early LC, through varying the constant wind density K which extends up to a radius R ext (eg. Dong et al 2020). K is dependent on both the mass loss rate of the progenitor star, as well as its wind velocity.…”

Section: Hydrodynamical Lc Modelingmentioning

confidence: 99%

PGIR 20eid (SN 2020qmp): A Type IIP Supernova at 15.6 Mpc discovered by the Palomar Gattini-IR survey

Srinivasaragavan

Sfaradi

Jencson

et al. 2022

A&A

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Aims. We present a detailed analysis of SN 2020qmp, a nearby Type II-P core-collapse supernova (CCSN), discovered by the Palomar Gattini-IR (PGIR) survey in the galaxy UGC07125 (distance of ≈ 15.6 ± 4 Mpc). We illustrate how the multiwavelength study of this event helps our general understanding of stellar progenitors and circumstellar medium (CSM) interactions in CCSNe. We highlight the importance of near-infrared (NIR) surveys for early detections of SNe in dusty environments. Methods. We analyze data from observations in various bands: radio, NIR, optical and X-rays. We use optical and NIR data for a spectroscopic and spectro-polarimetric study of the SN, and to model its lightcurve (LC). We estimate the explosion energy and zero-age main sequence (ZAMS) progenitor mass through hydrodynamical LC modeling. We also obtain an independent estimate of the ZAMS progenitor mass from the luminosity of the [O I] doublet lines (λλ6300, 6364) normalized to the decay power of 56 Co. From radio and X-ray observations, we derive the mass loss rate and microphysical parameters of the progenitor star, and investigate possible deviations from energy equipartition of magnetic fields and electrons in a standard CSM interaction model. Finally, we simulate a sample of CCSNe with plausible distributions of brightness and extinction, within 40 Mpc, and test what fraction of the sample is detectable at peak light by NIR surveys versus optical surveys. Results. SN 2020qmp displays characteristic hydrogen lines in its optical spectra, as well as a plateau in its optical LC, hallmarks of a Type II-P SN. We do not detect linear polarization during the plateau phase, with a 3σ upper limit of 0.78%. Through hydrodynamical LC modeling and an analysis of its nebular spectra, we estimate a progenitor mass of around 12 M , and an explosion energy of around 0.5 × 10 51 erg. We find that the spectral energy distribution cannot be explained by a simple CSM interaction model, assuming a constant shock velocity and steady mass-loss rate. In particular, the excess X-ray luminosity compared with the synchrotron radio luminosity suggests deviations from equipartition. Finally, we demonstrate the advantages of NIR surveys over optical surveys for the detection of dust-obscured CCSNe in the local universe. Specifically, our simulations show that the Wide-Field Infrared Transient Explorer (WINTER) will detect about 14 more CCSNe out of 75 expected in its footprint within 40 Mpc, over five years than an optical survey equivalent to the Zwicky Transient Facility (ZTF) would detect. Conclusions. We have determined or constrained the main properties of SN 2020qmp and of its progenitor, highlighting the value of multiwavelength follow up observations of nearby CCSNe. We have shown that forthcoming NIR surveys will finally enable us to do a nearly complete census of CCSNe in the local universe.

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“…RSGs have a significant mass-loss history, and it is intuitive for the CSM to be present (Mauron & Josselin 2011). However, in many cases, the CSM evades from being detected directly (Andrews et al 2019;Dong et al 2021). Nonetheless, the heating effects of such hidden CSM are at times observed in the form of enhanced luminosity (Nagao et al 2020;Haynie & Piro 2021).…”

Section: Introductionmentioning

confidence: 99%

SN 2020jfo: A Short-plateau Type II Supernova from a Low-mass Progenitor

Teja

Singh

Sahu

et al. 2022

ApJ

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We present spectroscopic and photometric observations of the Type IIP supernova, SN 2020jfo, in ultraviolet and optical wavelengths. SN 2020jfo occurred in the spiral galaxy M61 (NGC 4303), with eight observed supernovae in the past 100 yr. SN 2020jfo exhibited a short plateau lasting < 65 days, and achieved a maximum brightness in Vband of M V = −17.4 ± 0.4 mag at about 8.0 ± 0.5 days since explosion. From the bolometric light curve, we have estimated the mass of 56Ni synthesized in the explosion to be 0.033 ± 0.006 M ⊙. The observed spectral features are typical for a Type IIP supernova except for shallow Hα absorption throughout the evolution and the presence of stable 58Ni feature at 7378 Å, in the nebular phase. Using hydrodynamical modeling in the MESA + STELLA framework, an ejecta mass of ∼5 M ⊙ is estimated. Models also indicate SN 2020jfo could be the result of a red supergiant progenitor with M ZAMS ∼ 12 M ⊙. Bolometric light-curve modeling revealed the presence of a secondary radiation source for initial ∼20 days, which has been attributed to interaction with a circumstellar material of mass ∼ 0.2 M ⊙, which most likely was ejected due to enhanced mass loss about 20 yr prior to the supernova explosion.

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Supernova 2018cuf: A Type IIP Supernova with a Slow Fall from Plateau

Cited by 17 publications

References 121 publications

Progenitor and close-in circumstellar medium of type II supernova 2020fqv from high-cadence photometry and ultra-rapid UV spectroscopy

Progenitor and close-in circumstellar medium of type II supernova 2020fqv from high-cadence photometry and ultra-rapid UV spectroscopy

PGIR 20eid (SN 2020qmp): A Type IIP Supernova at 15.6 Mpc discovered by the Palomar Gattini-IR survey

SN 2020jfo: A Short-plateau Type II Supernova from a Low-mass Progenitor

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