SN 2018bsz: significant dust formation in a nearby superluminous supernova

-W., Chen, T.; Brennan, S. J.; Wesson, R.; Fraser, M.; Schweyer, T.; Inserra, C.; S., Schulze,; Nicholl, M.; Anderson, J. P.; Hsiao, E. Y.; A., Jerkstrand,; E., Kankare,; Kool, E. C.; Kravtsov, T.; Kuncarayakti, H.; Leloudas, G.; Li, C. -J.; Matsuura, M.; Pursiainen, M.; Roy, R.; Ruiter, A. J.; Schady, P.; Seitenzahl, I.; Sollerman, J.; Tartaglia, L.; Wang, L.; Yates, R. M.; Yang, S.; Baade, D.; Carini, R.; Gal-Yam, A.; Galbany, L.; Gonzalez-Gaitan, S.; Gromadzki, M.; Gutiérrez, C. P.; Kotak, R.; Maguire, K.; Mazzali, P. A.; Mueller-Bravo, T. E.; Paraskeva, E.; Pessi, P. J.; Pignata, G.; Rau, A.; Young, D. R.

doi:10.48550/arxiv.2109.07942

Cited by 23 publications

(41 citation statements)

References 118 publications

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“…Radio and millimetre observations have mostly found non-detections (Law et al 2019;Murase et al 2021;Eftekhari et al 2021;Hatsukade et al 2021a), but three sources have been detected: PTF10hgi (Eftekhari et al 2019;Law et al 2019;Mondal et al 2020;Hatsukade et al 2021b), which is consistent with the magnetar model; SN2017ens (Coppejans et al 2021a), which may be either due to a magnetar or CSM shock; and 2020tcw (Coppejans et al 2021b), which was detected only months after explosion and is likely due to CSM interaction. An infrared excess in magnetar-driven supernova was predicted by Omand et al (2019) due to heating of dust formed in the supernova, and which was observed recently in SN2018bsz (Chen et al 2021).…”

Section: Introductionmentioning

confidence: 65%

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

Poidevin,

Omand,

Pérez-Fournon

et al. 2022

Preprint

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Optical imaging polarimetry was conducted on the hydrogen poor superluminous supernova SN2020znr during 3 phases after maximum light (≈ +34 days, +288 days and +289 days). After instrumental and interstellar polarization correction, all measurements are consistent with null-polarization detection. Modelling the light curve with a magnetar spin-down model shows that SN2020znr has similar magnetar and ejecta parameters to other SLSNe. A comparison of the best-fit values discussed in the literature on SN2017egm and SN2015bn, two hydrogen poor SLSNe showing an increase of polarization after maximum light, suggests that SN2020znr has higher mass ejecta that may prevent access to the geometry of the inner ejecta with optical polarimetry. The combined information provided by spectroscopy and light curve analysis of type I SLSNe may be an interesting avenue to categorize the polarization properties of this class of transients. This approach would require to expand the sample of SLSNe polarimetry data currently available with early and late time epochs new measurements.

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Section: Introductionmentioning

confidence: 65%

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

Poidevin,

Omand,

Pérez-Fournon

et al. 2022

Preprint

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show abstract

“…With the deprecation of Python 2 and popular photometry packages within IRAF, AutoPhOT provides accurate photometry with little User setup or monitoring. AutoPhOT has already been used in several scientific publications (Chen et al 2021, Fraser et al 2021, Brennan et al 2021a, Brennan et al 2021b at the time of writing.…”

Section: Conclusion and Future Developmentmentioning

confidence: 99%

The Automated Photometry Of Transients (AutoPhOT) pipeline

Brennan¹,

Fraser²

2022

Preprint

Self Cite

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We present the AUTOmated Photometry Of Transients (AutoPhOT) package, a novel automated pipeline that is designed for rapid, publication-quality photometry of transients. AutoPhOT is built from the ground up using Python 3 -with no dependencies on legacy software. Capabilities of AutoPhOT include aperture and PSF-fitting photometry, template subtraction, and calculation of limiting magnitudes through artificial source injection. AutoPhOT is also capable of calibrating photometry against either survey catalogs (e.g. SDSS, PanSTARRS), or using a custom set of local photometric standards. We demonstrate the ability of AutoPhOT to reproduce lightcurves found in the published literature. AutoPhOT's ability to recover source fluxes is consistent with commonly used software e.g. DAOPHOT, using both aperture and PSF photometry. We also demonstrate that AutoPhOT can reproduce published lightcurves for a selection of transients with minimal human intervention.

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“…This phenomenon also extends to H-poor SLSNe (SLSNe-I). For example, iPTF13ehe, iPTFesb, iPTF16bad, iPTF16eh, SN 2018bsz, and other events discussed in Hosseinzadeh et al (2021) show evidence of CSM material located ∼ 10 16 cm from their explosion sites (Yan et al 2017;Lunnan et al 2018;Anderson et al 2018;Chen et al 2021;Pursiainen et al 2022).…”

Section: Introductionmentioning

confidence: 98%

Radio Analysis of SN 2004C Reveals an Unusual CSM Density Profile as a Harbinger of Core Collapse

DeMarchi¹,

Margutti²,

Dittman³

et al. 2022

Preprint

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We present extensive multi-frequency VLA and VLBA observations of the radio-bright supernova (SN) IIb SN 2004C that span ∼40-2793 days post-explosion. We interpret the temporal evolution of the radio spectral energy distribution (SED) in the context of synchrotron self-absorbed (SSA) emission from the explosion's forward shock as it expands in the circumstellar medium (CSM) previously sculpted by the mass-loss history of the stellar progenitor. VLBA observations and modeling of the VLA data point to a blastwave with average velocity ∼ 0.06c that carries an energy of ≈10 49 erg. Our modeling further reveals a flat CSM density profile ρ CSM ∝R −0.03 ± 0.22 up to a break radius R br ≈(1.96 ± 0.10) × 10 16 cm, with a steep density gradient following ρ CSM ∝R −2.3 ± 0.5 at larger radii. We infer that the flat part of the density profile corresponds to a CSM shell with mass ∼0.021 M , and that the progenitor's effective mass-loss rate varied with time over the range (50 − 500) × 10 −5 M yr −1 for an adopted wind velocity v w =1000 km s −1 and shock microphysical parameters e = 0.1, B = 0.01. These results add to the mounting observational evidence for departures from the traditional single-wind mass-loss scenarios in evolved, massive stars in the centuries leading up to core collapse. Potentially viable scenarios include mass loss powered by gravity waves and/or interaction with a binary companion.

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SN 2018bsz: significant dust formation in a nearby superluminous supernova

Cited by 23 publications

References 118 publications

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

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

The Automated Photometry Of Transients (AutoPhOT) pipeline

Radio Analysis of SN 2004C Reveals an Unusual CSM Density Profile as a Harbinger of Core Collapse

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