Broad-lined type Ic supernova iPTF16asu: A challenge to all popular models

Wang, L. J.; Wang, X. F.; Cano, Z.; Wang, S. Q.; Liu, Liang-Duan; Dai, Z. G.; Deng, J. S.; Yu, Hai; Li, B.; Song, Liming; Qiu, Y.; Wei, J. Y.

doi:10.1093/mnras/stz2184

Cited by 27 publications

(22 citation statements)

References 96 publications

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“…SN 2018gep (ZTF 18abukavn) is an SN discovered by the Zwicky Transient Factory (ZTF; Bellm et al 2019;Graham et al 2019), first analyzed by Ho et al (2019) and later by Pritchard et al (2020). This object has photometric and spectroscopic features similar to some other recent rapid transients, such as AT 2018cow (Prentice et al 2018;Smartt et al 2018;Margutti et al 2019;Perley et al 2019) and iPTF 16asu (Wang et al 2019;Whitesides et al 2017). SN 2018gep is remarkable for its very early detection by ZTF and its proximity at ∼143 Mpc from Earth, which allowed for detailed follow-up observations.…”

Section: Sn 2018gep As a Rapid Transientmentioning

confidence: 54%

Fast Blue Optical Transients Due to Circumstellar Interaction and the Mysterious Supernova SN 2018gep

Leung

Fuller

Nomoto

2021

ApJ

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The discovery of SN 2018gep (ZTF 18abukavn) challenged our understanding of the late-phase evolution of massive stars and their supernovae (SNe). The fast rise in luminosity of this SN (spectroscopically classified as a broad-lined Type Ic SN) indicates that the ejecta interacts with a dense circumstellar medium (CSM), while an additional energy source such as 56 Ni decay is required to explain the late-time light curve. These features hint at the explosion of a massive star with pre-SN mass loss. In this work, we examine the physical origins of rapidly evolving astrophysical transients like SN 2018gep. We investigate the wave-driven mass-loss mechanism and how it depends on model parameters such as progenitor mass and deposition energy, searching for stellar progenitor models that can reproduce the observational data. A model with an ejecta mass ∼2 M e , explosion energy ∼10 52 erg, a CSM of mass ∼0.3 M e and radius ∼1000 R e , and a 56 Ni mass ∼0.3 M e provides a good fit to the bolometric light curve. We also examine how interaction-powered light curves depend more generally on these parameters and how ejecta velocities can help break degeneracies. We find both wave-driven mass loss and mass ejection via pulsational pair instability can plausibly create the dense CSM in SN 2018gep, but we favor the latter possibility.

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Section: Sn 2018gep As a Rapid Transientmentioning

confidence: 54%

Fast Blue Optical Transients Due to Circumstellar Interaction and the Mysterious Supernova SN 2018gep

Leung

Fuller

Nomoto

2021

ApJ

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“…And then the bolometric luminosities before MJD 58288.44 are estimated using the single band photometry data. We adopt a hybrid model which includes 56 Ni powering and the interaction of the SN ejecta with a dense CSM with density profile as a power-law, i. e. ρ CSM ∝ r −s , where the typical value of s is 2 and 0 (e.g., Chatzopoulos et al 2012Chatzopoulos et al , 2013Wang et al 2019). In our model, the density distribution of the ejecta is uniform in the inner region (δ=0), and follows a power-law (ρ ∝ r −12 ) in the outer region.…”

Section: Modeling the Rapid Evolving Light Curvesmentioning

confidence: 99%

The Peculiar Transient AT2018cow: A Possible Origin of a Type Ibn/IIn Supernova

Xiang¹,

Wang

Lin³

et al. 2021

ApJ

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We present our photometric and spectroscopic observations on the peculiar transient AT2018cow. The multi-band photometry covers from peak to ∼70 days and the spectroscopy ranges from 5 to ∼50 days. The rapid rise (t r 2.9 days), high luminosity (M V,peak ∼ −20.8 mag) and fast decline after peak make AT2018cow stand out of any other optical transients. While we find that its light curves show high resemblance to those of type Ibn supernovae. Moreover, the spectral energy distribution remains high temperature of ∼14,000 K after ∼15 days since discovery. The spectra are featureless in the first 10 days, while some broad emission lines due to H, He, C and O emerge later, with velocity declining from ∼ 14, 000 km s −1 to ∼3000 km s −1 at the end of our observations. Narrow and weak He I emission lines emerge in the spectra at t >20 days since discovery. These emission lines are reminiscent of the features seen in interacting supernovae like type Ibn and IIn subclasses. We fit the bolometric light curves with a model of circumstellar interaction (CSI) and radioactive decay (RD) of 56 Ni and find a good fit with ejecta mass M ej ∼ 3.16 M , circumstellar material mass M CSM ∼ 0.04 M , and ejected 56 Ni mass M56 Ni ∼ 0.23 M . The CSM shell might be formed in an eruptive mass ejection of the progenitor star. Furthermore, host environment of AT2018cow implies connection of AT2018cow with massive stars. Combining observational properties and the light curve fitting results, we conclude that AT2018cow might be a peculiar interacting supernova originated from a massive star.

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“…A handful have been discovered while the transient was still active, enabling prompt follow-up observations. For example, spectroscopic monitoring of the fast luminous transients iPTF16asu (Whitesides et al 2017;Wang et al 2019) and ZTF18abukavn (SN 2018gep;Ho et al 2019a) revealed that, as the optical emission faded, the spectrum developed features typical of broad-lined Ic SNe.…”

Section: Introductionmentioning

confidence: 99%

The Koala: A Fast Blue Optical Transient with Luminous Radio Emission from a Starburst Dwarf Galaxy at z = 0.27

Ho¹,

Perley²,

Kulkarni³

et al. 2020

ApJ

105

111

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We present ZTF18abvkwla (the "Koala"), a fast blue optical transient discovered in the Zwicky Transient Facility (ZTF) One-Day Cadence (1DC) Survey. ZTF18abvkwla has a number of features in common with the groundbreaking transient AT 2018cow: blue colors at peak (-»g r 0.5 mag), a short rise time from half-max of under two days, a decay time to half-max of only three days, a high optical luminosity (»-M 20.6 g,peak mag), a hot (40,000 K) featureless spectrum at peak light, and a luminous radio counterpart. At late times (D > t 80 days), the radio luminosity of ZTF18abvkwla (n n- L 10 erg s 40 1 at 10 GHz, observer-frame) is most similar to that of long-duration gamma-ray bursts (GRBs). The host galaxy is a dwarf starburst galaxy ( »Ḿ M 5 10 8 ,  »-M SFR 7 yr 1) that is moderately metal-enriched ([ ] » log O H 8.5), similar to the hosts of GRBs and superluminous supernovae. As in AT2018cow, the radio and optical emission in ZTF18abvkwla likely arise from two separate components: the radio from fast-moving ejecta (b G > c c 0.38) and the optical from shockinteraction with confined dense material (<0.07 M e in~10 cm 15). Compiling transients in the literature with < t 5 days rise and <-M 20 peak mag, we find that a significant number are engine-powered, and suggest that the high peak optical luminosity is directly related to the presence of this engine. From 18 months of the 1DC survey, we find that transients in this rise-luminosity phase space are at least two to three orders of magnitude less common than CC SNe. Finally, we discuss strategies for identifying such events with future facilities like the Large Synoptic Survey Telescope, as well as prospects for detecting accompanying X-ray and radio emission.

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Broad-lined type Ic supernova iPTF16asu: A challenge to all popular models

Cited by 27 publications

References 96 publications

Fast Blue Optical Transients Due to Circumstellar Interaction and the Mysterious Supernova SN 2018gep

Fast Blue Optical Transients Due to Circumstellar Interaction and the Mysterious Supernova SN 2018gep

The Peculiar Transient AT2018cow: A Possible Origin of a Type Ibn/IIn Supernova

The Koala: A Fast Blue Optical Transient with Luminous Radio Emission from a Starburst Dwarf Galaxy at z = 0.27

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