SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

doi:10.3847/1538-4357/ab43e3

Cited by 33 publications

(40 citation statements)

References 151 publications

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“…However, dust formation could also result in a fast-declining tail, and additional effects such as a different radioactivities could affect the decline (Branch & Wheeler 2017), as well as CSM-ejecta interaction, which can contribute to the luminosity at late times (e.g. Andrews et al 2019).…”

Section: Bolometric Light Curvementioning

confidence: 99%

SN 2019hcc: a Type II supernova displaying early O ii lines

Parrag

Inserra

Schulze

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present optical spectroscopy together with ultraviolet, optical and near-infrared photometry of SN 2019hcc, which resides in a host galaxy at redshift 0.044, displaying a sub-solar metallicity. The supernova spectrum near peak epoch shows a ‘w’ shape at around 4000 Åwhich is usually associated with O ii lines and is typical of Type I superluminous supernovae. SN 2019hcc post-peak spectra show a well-developed Hα P-Cygni profile from 19 days past maximum and its light curve, in terms of its absolute peak luminosity and evolution, resembles that of a fast-declining Hydrogen-rich supernova (SN IIL). The object does not show any unambiguous sign of interaction as there is no evidence of narrow lines in the spectra or undulations in the light curve. Our tardis spectral modelling of the first spectrum shows that Carbon, Nitrogen and Oxygen (CNO) at 19000 K reproduce the ‘w’ shape and suggests that a combination of non-thermally excited CNO and metal lines at 8000 K could reproduce the feature seen at 4000 Å. The Bolometric light curve modelling reveals that SN 2019hcc could be fit with a magnetar model, showing a relatively strong magnetic field (B>3 × 1014G), which matches the peak luminosity and rise time without powering up the light curve to superluminous luminosities. The high-energy photons produced by the magnetar would then be responsible for the detected O ii lines. As a consequence, SN 2019hcc shows that a ‘w’ shape profile at around 4000 Å, usually attributed to O ii, is not only shown in superluminous supernovae and hence it should not be treated as the sole evidence of the belonging to such a supernova type.

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Section: Bolometric Light Curvementioning

confidence: 99%

SN 2019hcc: a Type II supernova displaying early O ii lines

Parrag

Inserra

Schulze

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…The photometric and spectroscopic follow-up observations of SN2018ivc were obtained and coordinated through Las Cumbres Observatory's Global Supernova Project (GSP; PI: D. A. Howell), a key project to collect densely sampled optical light curves and spectra of nearby and bright SNe (e.g., Andrews et al 2019;Szalai et al 2019).…”

Section: Observationsmentioning

confidence: 99%

Discovery and Rapid Follow-up Observations of the Unusual Type II SN 2018ivc in NGC 1068

Bostroem

Valenti

Sand

et al. 2020

ApJ

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We present the discovery and high-cadence follow-up observations of SN2018ivc, an unusual SNe II that exploded in NGC1068 (D=10.1 Mpc). The light curve of SN2018ivc declines piecewise-linearly, changing slope frequently, with four clear slope changes in the first 30 days of evolution. This rapidly changing light curve indicates that interaction between the circumstellar material and ejecta plays a significant role in the evolution. Circumstellar interaction is further supported by a strong X-ray detection. The spectra are rapidly evolving and dominated by hydrogen, helium, and calcium emission lines. We identify a rare high-velocity emission-line feature blueshifted at ∼7800 km s 1 (in Hα, Hβ, Pβ, Pγ, He I, and Ca II), which is visible from day 18 until at least day 78 and could be evidence of an asymmetric progenitor or explosion. From the overall similarity between SN2018ivc and SN1996al, the Hα equivalent width of its parent H IIregion, and constraints from pre-explosion archival Hubble Space Telescope images, we find that the progenitor of SN2018ivc could be as massive as 52 M  but is more likely <12 M . SN2018ivc demonstrates the importance of the early discovery and rapid follow-up observations of nearby supernovae to study the physics and progenitors of these cosmic explosions.

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“…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 2020). 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. Morozova et al (2018) demonstrated using light curves of 20 nearby hydrogen-rich (Type II) SNe that early-time excess flux from CSM interaction is a generic feature of this class of CCSNe.…”

Section: Introductionmentioning

confidence: 87%

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

Preprint

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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 (10 14 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 × 10 46 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 𝑀 ZAMS ≈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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SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

Cited by 33 publications

References 151 publications

SN 2019hcc: a Type II supernova displaying early O ii lines

SN 2019hcc: a Type II supernova displaying early O ii lines

Discovery and Rapid Follow-up Observations of the Unusual Type II SN 2018ivc in NGC 1068

Progenitor and Close-In Circumstellar Medium of Type II Supernova 2020fqv from High-Cadence Photometry and Ultra-Rapid UV Spectroscopy

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