Constraints on Type IIn supernova progenitor outbursts from the Lick Observatory Supernova Search

Bilinski, Christopher; Smith, Nathan; Li, Weidong; Williams, G. G.; Zheng, Wei; Filippenko, A. V.

doi:10.1093/mnras/stv566

Cited by 31 publications

(32 citation statements)

References 93 publications

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“…This evidence can come in the form of direct detections of pre-SN outbursts (e.g., Foley et al 2007Foley et al , 2011Pastorello et al 2007Pastorello et al , 2013Smith et al 2010;Mauerhan et al 2013) or inferred from the dense CSM needed to explain SN light curves (e.g., Ofek et al 2007;Smith & McCray 2007;Smith et al , 2008Fransson et al 2014). Although how common such eruptions are is still being investigated (see Ofek et al 2014;Bilinski et al 2015), our work may indicate that SNe IIL are just lower mass versions of these. It is interesting to note that the time of the wind t wind given in Table 1 is comparable to the duration of the carbon shell burning for an M M 12 ZAMS =  star (see Fuller et al 2015).…”

Section: Source Of the Csmmentioning

confidence: 69%

Unifying Type II Supernova Light Curves with Dense Circumstellar Material

Morozova

Piro

Valenti

2017

ApJ

178

247

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A longstanding problem in the study of supernovae (SNe) has been the relationship between the TypeIIP and TypeIIL subclasses. Whether they come from distinct progenitors or they are from similar stars with some property that smoothly transitions from one class to another has been the subject of much debate. Here,using onedimensional radiation-hydrodynamic SN models, we showthat the multi-band light curves of SNe IIL are well fit by ordinary red supergiants surrounded by dense circumstellar material (CSM). The inferred extent of this material, coupled with a typical wind velocity of 10 100 km s 1 --, suggests enhanced activity by these stars during the last months to ∼years of their lives, which may be connected with advanced stages of nuclear burning. Furthermore, we find that,even for more plateau-like SNe,dense CSM provides a better fit to the first 20 days of their light curves, indicating that the presence of such material may be more widespread than previously appreciated. Here we choose to model the CSM with a wind-like density profile, but it is unclear whether this just generally represents some other mass distribution, such as a recent mass ejection, thick disk, or even inflated envelope material. Better understanding the exact geometry and density distribution of this material will be an important question for future studies.

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Section: Source Of the Csmmentioning

confidence: 69%

Unifying Type II Supernova Light Curves with Dense Circumstellar Material

Morozova

Piro

Valenti

2017

ApJ

178

247

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“…These correlations are expected if the precursors are mass ejection events, and the early-time light curve of these SNe is powered by interaction of the SN ejecta with optically thick CSM. No precursors were found in a similar search among five SNe IIn that was recently reported by Bilinski et al (2015). They do not provide the absolutemagnitude-dependent search time of their sample, so direct comparison of the two surveys is not straightforward.…”

Section: Introductionmentioning

confidence: 73%

PTF13efv—AN OUTBURST 500 DAYS PRIOR TO THE SNHUNT 275 EXPLOSION AND ITS RADIATIVE EFFICIENCY

Ofek

Cenko

Shaviv

et al. 2016

ApJ

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The progenitors of some supernovae (SNe) exhibit outbursts with super-Eddington luminosities prior to their final explosions. This behavior is common among SNe IIn, but the driving mechanisms of these precursors are not yet well-understood. SNHunt 275 was announced as a possible new SN during 2015 May. Here we report on preexplosion observations of the location of this event by the Palomar Transient Factory (PTF) and report the detection of a precursor about 500 days prior to the 2015 May activity (PTF 13efv). The observed velocities in the 2015 transient and its 2013 precursor absorption spectra are low (1000-2000 km s −1 ), so it is not clear yet if the recent activity indeed marks the final disruption of the progenitor. Regardless of the nature of this event, we use the PTF photometric and spectral observations, as well as Swift-UVOT observations, to constrain the efficiency of the radiated energy relative to the total kinetic energy of the precursor. We find that, using an order-of-magnitude estimate and under the assumption of spherical symmetry, the ratio of the radiated energy to the kinetic energy is in the range of 4 × 10 −2 to 3.4 × 10 3 .

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“…The new astronomical surveys planned, or already in operation, will provide photometry of SNe IIn allowing further tests of the light curve property correlations found or rejected in this study. The new surveys will also allow more precursor outbursts (Ofek et al 2014c;Bilinski et al 2015) to be discovered, opening new windows to the last years of the SNe IIn progenitor stars. The Zwicky Transient Facility (ZTF, e.g.…”

Section: Discussionmentioning

confidence: 99%

Type IIn supernova light-curve properties measured from an untargeted survey sample

Nyholm

Sollerman

Tartaglia

et al. 2020

A&A

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The evolution of a Type IIn supernova (SN IIn) is governed by the interaction between the SN ejecta and a hydrogen-rich circumstellar medium (CSM). SNe IIn thus allow us to probe the late-time mass-loss history of their progenitor stars. We present a sample of SNe IIn from the untargeted, magnitude-limited surveys of the Palomar Transient Factory (PTF) and its successor, the intermediate PTF (iPTF). To date, statistics on SN IIn optical light curve properties have generally been based on small ( 10 SNe) samples from targeted SN surveys. SNe IIn found and followed by the PTF/iPTF were used to select a sample of 42 events with useful constraints on the rise times as well as with available post-peak photometry. The SNe were discovered in 2009-2016 and have at least one low-resolution classification spectrum, as well as photometry from the P48 and P60 telescopes at Palomar Observatory. We study the light-curve properties of these SNe IIn using spline fits (for the peak and the declining portion) and template matching (for the rising portion). We study the peak-magnitude distribution, rise times, decline rates, colour evolution, host galaxies, and K-corrections of the SNe in our sample. We find that the typical rise times are divided into fast and slow risers as 20 ± 8 d and 50 ± 15 d, respectively. The decline rates could possibly be divided into two groups (with slopes 0.013 ± 0.008 mag d −1 and 0.040 ± 0.014 mag d −1 ), but this division has weak statistical significance. We find no significant correlation between the peak luminosity of SNe IIn and their rise times, but the more luminous SNe IIn are generally found to be more durable and the slowly rising SNe IIn are generally found to be slowly declining. The SNe in our sample were hosted by galaxies of absolute magnitude −22 Mg −13 mag. The K-corrections at light-curve peak of the SNe in our sample are found to be within 0.2 mag for the observer's frame r-band, for SNe IIn at redshifts z < 0.25. Applying K-corrections and including also ostensibly "superluminous" SNe IIn, we find that the peak magnitudes are M r peak = −19.18 ± 1.32 mag. We conclude that the occurrence of conspicuous light-curve bumps in SNe IIn, such as in iPTF13z, is limited to 1.4 +14.6 −1.0 % of the SNe IIn. We also investigate a possible subtype of SNe IIn with a fast rise to a 50 d plateau followed by a slow, linear decline. iPTF13agz, iPTF13aki, iPTF13asr, iPTF13cuf, iPTF14bcw, iPTF14bpa, iPTF15aym, iPTF15bky, iPTF15blp, iPTF15eqr, iPTF16fb. ⋆ Based in part on observations made with the Palomar Transient Factory and intermediate Palomar Transient Factory surveys.

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Constraints on Type IIn supernova progenitor outbursts from the Lick Observatory Supernova Search

Cited by 31 publications

References 93 publications

Unifying Type II Supernova Light Curves with Dense Circumstellar Material

Unifying Type II Supernova Light Curves with Dense Circumstellar Material

PTF13efv—AN OUTBURST 500 DAYS PRIOR TO THE SNHUNT 275 EXPLOSION AND ITS RADIATIVE EFFICIENCY

Type IIn supernova light-curve properties measured from an untargeted survey sample

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