Post maximum light and late time optical imaging polarimetry of type I superluminous supernova 2020znr

Poidevin, F.; Omand, C. M. B.; Pérez-Fournon, I.; Clavero, R.; Shirley, R.; Marques-Chaves, R.; Angel, C. Jimenez; Geier, S.

doi:10.48550/arxiv.2201.03887

Cited by 2 publications

(1 citation statement)

References 86 publications

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“…Both studies concluded that the inner ejecta were more aspherical than the outer ejecta. However, several other SLSNe have had detections consistent with zero polarization and thus have a spherical ejecta (e.g Leloudas et al 2015;Cikota et al 2018;Lee 2019Lee , 2020Poidevin et al 2022), implying that significant asymmetries may only appear in a minority of SLSNe. Vurm & Metzger (2021) relaxed the assumption that a magnetar's power output is 100% thermalized by the SLSN ejecta.…”

Section: Breakdown Of Assumptionsmentioning

confidence: 99%

SN 2020qlb: A hydrogen-poor superluminous supernova with well-characterized light curve undulations

West

Lunnan

Omand

et al. 2023

A&A

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Context. SN 2020qlb (ZTF20abobpcb) is a hydrogen-poor superluminous supernova (SLSN-I) that is among the most luminous (maximum M g = −22.25 mag) and that has one of the longest rise times (77 days from explosion to maximum). We estimate the total radiated energy to be > 2.1 × 10 51 erg. SN 2020qlb has a well-sampled light curve that exhibits clear near and post peak undulations, a phenomenon seen in other SLSNe, whose physical origin is still unknown. Aims. We discuss the potential power source of this immense explosion as well as the mechanisms behind its observed light curve undulations. Methods. We analyze photospheric spectra and compare them to other SLSNe-I. We construct the bolometric light curve using photometry from a large data set of observations from the Zwicky Transient Facility (ZTF), Liverpool Telescope (LT) and Neil Gehrels Swift Observatory and compare it with radioactive, circumstellar interaction and magnetar models. Model residuals and light curve polynomial fit residuals are analyzed to estimate the undulation timescale and amplitude. We also determine host galaxy properties based on imaging and spectroscopy data, including a detection of the [O III]λ4363, auroral line, allowing for a direct metallicity measurement. Results. We rule out the Arnett 56 Ni decay model for SN 2020qlb's light curve due to unphysical parameter results. Our most favored power source is the magnetic dipole spin-down energy deposition of a magnetar. Two to three near peak oscillations, intriguingly similar to those of SN 2015bn, were found in the magnetar model residuals with a timescale of 32 ± 6 days and an amplitude of 6% of peak luminosity. We rule out centrally located undulation sources due to timescale considerations; and we favor the result of ejecta interactions with circumstellar material (CSM) density fluctuations as the source of the undulations.

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Section: Breakdown Of Assumptionsmentioning

confidence: 99%

SN 2020qlb: A hydrogen-poor superluminous supernova with well-characterized light curve undulations

West

Lunnan

Omand

et al. 2023

A&A

View full text Add to dashboard Cite

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SN2020qlb: a hydrogen-poor superluminous supernova with well-characterized light curve undulations

West¹,

Lunnan²,

Omand³

et al. 2022

Preprint

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Context. SN 2020qlb (ZTF20abobpcb) is a hydrogen-poor superluminous supernova (SLSN-I) that is among the most luminous (maximum M g = −22.25 mag) and that has one of the longest rise times (77 days from explosion to maximum). We estimate the total radiated energy to be > 2.1 × 10 51 ergs. SN 2020qlb has a well-sampled light curve that exhibits clear undulations, a phenomenon seen in other SLSNe, whose physical origin is still unknown. Aims. We discuss the potential power source of this immense explosion as well as the mechanisms behind its observed light curve undulations. Methods. We analyze photospheric spectra and compare them to other SLSNe-I. We construct the bolometric light curve using photometry from a large data set of observations from the Zwicky Transient Facility (ZTF), Liverpool Telescope (LT) and Neil Gehrels Swift Observatory and compare it with radioactive, circumstellar interaction and magnetar models. Model residuals and light curve polynomial fit residuals are analyzed to estimate the undulation timescale and amplitude. We also determine host galaxy properties based on imaging and spectroscopy data, including a detection of the [O III]λ4363Å auroral line, allowing for a direct metallicity estimate. Results. We rule out the Arnett 56 Ni decay model for SN 2020qlb's light curve due to unphysical parameter results. Our most favored power source is the magnetic dipole spin-down energy deposition of a magnetar. Two to three near peak oscillations, intriguingly similar to those of SN 2015bn, were found in the magnetar model residuals with a timescale of 32 ± 6 days and an amplitude of 6% of peak luminosity. We rule out centrally located undulation sources due to timescale considerations; and we favor the result of ejecta interactions with circumstellar material (CSM) density fluctuations as the source of the undulations.

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Post maximum light and late time optical imaging polarimetry of type I superluminous supernova 2020znr

Cited by 2 publications

References 86 publications

SN 2020qlb: A hydrogen-poor superluminous supernova with well-characterized light curve undulations

SN 2020qlb: A hydrogen-poor superluminous supernova with well-characterized light curve undulations

SN2020qlb: a hydrogen-poor superluminous supernova with well-characterized light curve undulations

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