PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses

Pian, E.; Mazzali, Paolo A.; Moriya, Takashi J.; Rubin, A.; Gal‐Yam, A.; Arcavi, I.; Ben-Ami, Sagi; Blagorodnova, N.; Bufano, F.; Filippenko, A. V.; Kasliwal, Mansi M.; Kulkarni, S. R.; Lunnan, R.; Manulis, I.; Matheson, T.; Nugent, P.; Ofek, E. O.; Perley, D.; Prentice, S.; Yaron, O.

doi:10.1093/mnras/staa2191

“…It has been widely suggested that SLSNe and SNe Ic-BL associated/unassociated with lGRBs, or at least a good fraction of them, are also driven by millisecond magnetars (e.g., Kasen & Bildsten 2010;Lü & Zhang 2014;Mazzali et al 2014;Metzger et al 2015;Kashiyama et al 2016;Liu et al 2017;Nicholl et al 2017;Yu et al 2017;Lü et al 2018). Therefore, it is necessary and interesting to investigate the possible connection and differences between FBOTs and these explosion phenomena, as has been done in previous research (e.g., Milisavljevic et al 2013;Yu et al 2017;Margutti et al 2019;Pian et al 2020) for connecting normal SNe Ib/c, SLSNe, and lGRBs. For comparison, we display the FBOTs along with SLSNe, GRB-SNe, and normal SNe Ic-BL in the M ej versus P i space in Figure 1, and in the P i versus B p space in Figure 2.…”

Section: Connection With Slsne and Sne Ic-blmentioning

confidence: 91%

Magnetar Engines in Fast Blue Optical Transients and Their Connections with SLSNe, SNe Ic-BL, and lGRBs

Liu

¹

,

Zhu

²

,

Liu

³

et al. 2022

ApJL

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We fit the multiband lightcurves of 40 fast blue optical transients (FBOTs) with the magnetar engine model. The mass of the FBOT ejecta, the initial spin period, and the polar magnetic field of the FBOT magnetars are respectively constrained to M ej = 0.11 − 0.09 + 0.22 M ⊙ , P i = 9.1 − 4.4 + 9.3 ms , and B p = 11 − 7 + 18 × 10 14 G . The wide distribution of the value of B p spreads the parameter ranges of the magnetars from superluminous supernovae (SLSNe) to broad-line Type Ic supernovae (SNe Ic-BL; some are observed to be associated with long-duration gamma-ray bursts), which are also suggested to be driven by magnetars. Combining FBOTs with the other transients, we find a strong universal anticorrelation of P i ∝ M ej − 0.41 , indicating they could share a common origin. To be specific, it is suspected that all of these transients originate from the collapse of extremely stripped stars in close binary systems, but with different progenitor masses. As a result, FBOTs distinguish themselves by their small ejecta masses with an upper limit of ∼1 M ⊙, which leads to an observational separation in the rise time of the lightcurves of ∼10 days. In addition, FBOTs together with SLSNe can be separated from SNe Ic-BL by an empirical line in the M peak–t rise plane corresponding to an energy requirement of the mass of 56Ni of ∼0.3M ej, where M peak is the peak absolute magnitude of the transients and t rise is the rise time.

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“…This code has been applied numerous times on strippedenvelope transients (e.g., Mazzali et al 2002;Sauer et al 2006;Mazzali et al 2017;Ashall et al 2019;Pian et al 2020;Teffs et al 2021), including SLSNe (Mazzali et al 2016), and was used for a parameter study in relation to extremely energetic SNe Ic (Ashall & Mazzali 2020). For our models, we needed to create ad-hoc density profiles.…”

Section: Snapshot Spectral Modellingmentioning

confidence: 99%

“…It was noted in Section 4 that none of these objects show emission lines consistent with CSM interaction. We can consider this an external process, as the energy injection occurs on the outside of the ejecta, however interaction has been proposed as a way to power the transitional event PTF11rka without explicit spectroscopic signatures of interaction (Pian et al 2020).…”

Section: Powering Mechanismsmentioning

confidence: 99%

Transitional events in the spectrophotometric regime between stripped envelope and superluminous supernovae

Prentice,

Inserra,

Schulze

et al. 2021

Preprint

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The division between stripped-envelope supernovae (SE-SNe) and superluminous supernovae (SLSNe) is not well defined in either photometric or spectroscopic space. While a sharp luminosity threshold has been suggested, there remains an increasing number of transitional objects that reach this threshold without the spectroscopic signatures common to SLSNe. In this work we present data and analysis on four SNe transitional between SE-SNe and SLSNe; the He-poor SNe 2019dwa and 2019cri, and the He-rich SNe 2019hge and 2019unb. Each object displays long-lived and variable photometric evolution with luminosities around the SLSN threshold of 𝑀 𝑟 < −19.8 mag. Spectroscopically however, these objects are similar to SE-SNe, with line velocities lower than either SE-SNe and SLSNe, and thus represent an interesting case of rare transitional events.

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“…A full investigation of the properties of the inner ejecta of SNe requires modelling with radiative-transfer codes owing to the non-local thermodynamic equilibrium (non-LTE) nature of the line-forming processes during the nebular phase. Such methods have been applied in the literature to SNe II (e.g., Dessart & Hillier 2011;Jerkstrand et al 2012;Jerkstrand et al 2014), SNe Ia (e.g., Botyánszki et al 2018;Mazzali et al 2020;Shingles et al 2020), SNe Ibc (e.g., Mazzali et al 2009Mazzali et al , 2010Jerkstrand et al 2015b;Pian et al 2020), and SLSNe (e.g. Dessart et al 2013;Jerkstrand et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Oxygen and calcium nebular emission line relationships in core-collapse supernovae and Ca-rich transients

Prentice,

Maguire,

Siebenaler

et al. 2022

Preprint

0

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This work examines the relationships between the properties (flux ratios, full width at half-maximum velocities) of the [O ] 𝜆𝜆6300, 6364, [Ca ] 𝜆𝜆7291, 7323, and the Ca near-infrared triplet, emission lines of a large sample of core-collapse supernovae (SNe) and Ca-rich transients (509 spectra of 86 transients, of which 10 transients are Ca-rich events). Line-flux ratios as a function of time were investigated with differences identified between the transient classes, in particular the Type II SNe were found to have distinct line-flux ratios compared to stripped-envelope (SE) SNe. No correlation was found between the [Ca ]/[O ] flux ratios of SE-SNe and their ejecta masses and kinetic energies (as measured from light curve modelling), suggesting that there may be a contribution from an additional power source in more luminous SE-SNe. We found that the mean characteristic width of the [Ca ] emission line is less than the [O ] emission line for all SN types, indicating that the [Ca ] emission typically originates from deeper in the ejecta than [O ]. This is in some tension with standard models for emission in Type II SNe. The emission line properties of Type II SNe were also compared to theoretical models and found to favour lower mass tracks (𝑀 ZAMS < 15 M ), with no evidence found for significant mixing of 56 Ni into the H envelope nor Ca mixed into the O shell. The flux ratios of some superluminous SNe were found to be similar to those of SE-SNe when scaling to account for their longer rise times was applied (although we caution the sample size is small).

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PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses

Cited by 8 publications

References 84 publications

Magnetar Engines in Fast Blue Optical Transients and Their Connections with SLSNe, SNe Ic-BL, and lGRBs

Magnetar Engines in Fast Blue Optical Transients and Their Connections with SLSNe, SNe Ic-BL, and lGRBs

Transitional events in the spectrophotometric regime between stripped envelope and superluminous supernovae

Oxygen and calcium nebular emission line relationships in core-collapse supernovae and Ca-rich transients

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