The Type II-plateau Supernova 2017eaw in NGC 6946 and Its Red Supergiant Progenitor

Dyk, Schuyler D. Van; Zheng, W.; Maund, Justyn R.; Brink, Thomas G.; Srinivasan, S.; Andrews, Jennifer E.; Smith, Nathan; Leonard, Douglas C.; Morozova, Viktoriya; Filippenko, A. V.; Conner, Brody; Milisavljevic, Dan; Jaeger, Thomas de; Long, Knox S.; Isaacson, Howard; Crossfield, Ian J. M.; Kosiarek, Molly R.; Howard, Andrew W.; Fox, O.; Kelly, Patrick L.; Piro, Anthony L.; Littlefair, S.; Dhillon, V. S.; Wilson, Richard W.; Butterley, Timothy; Yunus, Sameen; Channa, Sanyum; Jeffers, Benjamin T.; Falcon, Edward; Ross, Timothy W.; Hestenes, Julia; Stegman, Samantha; Zhang, Keto D.; Kumar, Sahana

doi:10.3847/1538-4357/ab1136

Cited by 71 publications

(76 citation statements)

References 168 publications

(273 reference statements)

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“…Using the pre-explosion brightness of m F160W = 19.36 ± 0.01 and a distance to the host galaxy of NGC6946 of 7.72±0.32Mpc (see discussion in Van Dyk et al 2019), we find a terminal luminosity of log L/L ⊙ = 4.96 ± 0.11. This is in very good agreement with the Kilpatrick & Foley (2018) and Van Dyk et al (2019) studies.…”

Section: The Input Samplesupporting

confidence: 91%

The ‘red supergiant problem’: the upper luminosity boundary of Type II supernova progenitors

Davies

Beasor

2020

Monthly Notices of the Royal Astronomical Society

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By comparing the properties of Red Supergiant (RSG) supernova progenitors to those of field RSGs, it has been claimed that there is an absence of progenitors with luminosities L above log(L/L ⊙ ) > 5.2. This is in tension with the empirical upper luminosity limit of RSGs at log(L/L ⊙ ) = 5.5, a result known as the 'Red Supergiant Problem'. This has been interpreted as evidence for an upper mass threshold for the formation of black-holes. In this paper, we compare the observed luminosities of RSG SN progenitors with the observed RSG L-distribution in the Magellanic Clouds. Our results indicate that the absence of bright SN II-P/L progenitors in the current sample can be explained at least in part by the steepness of the L-distribution and a small sample size, and that the statistical significance of the Red Supergiant Problem is between 1-2σ . Secondly, we model the luminosity distribution of II-P/L progenitors as a simple power-law with an upper and lower cutoff, and find an upper luminosity limit of log(L hi /L ⊙ ) = 5.20 +0.17 −0.11 (68% confidence), though this increases to ∼5.3 if one fixes the power-law slope to be that expected from theoretical arguments. Again, the results point to the significance of the RSG Problem being within ∼ 2σ. Under the assumption that all progenitors are the result of single-star evolution, this corresponds to an upper mass limit for the parent distribution of M hi = 19.2M ⊙ , ±1.3M ⊙ (systematic), +4.5 −2.3 M ⊙ (random) (68% confidence limits).After the initial study by S09, a larger sample of progenitors was used by Smartt (2015, hereafter S15) to revise the value of M max upwards to 17M ⊙ . Further, Davies & Beasor (2018, hereafter DB18) later revisited the complexities of converting a preexplosion brightness to bolometric luminosity L fin , and the conver-

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Section: The Input Samplesupporting

confidence: 91%

The ‘red supergiant problem’: the upper luminosity boundary of Type II supernova progenitors

Davies

Beasor

2020

Monthly Notices of the Royal Astronomical Society

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“…Van Dyk et al (2019) used Geneva evolutionary tracks(Georgy et al 2013) to estimate the ZAMS mass of the progenitor as ≈ 15 M , but we arrive to the same conclusion based on the pre-explosion luminosities of KE-PLER models.6 Buta & Keel (2019) obtained a higher 56 Ni mass of 0.115 M for the same SN.…”

supporting

confidence: 62%

“…The optical Large Binocular Telescope (LBT) archival images of SN 2017eaw were analyzed by Johnson et al (2018), where no signs of the progenitor pre-explosion activity were found. Further analysis of the Hubble Space Telescope (HST) data by Rui et al (2019) indicated a dimming of the progenitor by 30% one year before the explosion (see also Van Dyk et al 2019). It is possible that the outburst could happen between the relatively scarce HST measurements.…”

Section: Conclusion and Discussionmentioning

confidence: 98%

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The Influence of Late-stage Nuclear Burning on Red Supergiant Supernova Light Curves

Morozova

Piro

Fuller

et al. 2020

ApJL

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Many Type II supernovae (SNe) show hot early (∼30 days) emission, and a diversity in their light curves extending from the Type IIP to the Type IIL, which can be explained by interaction with dense and confined circumstellar material (CSM). We perform hydrodynamical simulations of red supergiants to model the ejection of CSM caused by wave heating during late-stage nuclear burning. Even a small amount of deposited energy (10 46 − 10 47 erg), which is roughly that expected due to waves excited by convection in the core, is sufficient to change the shapes of SN light curves and bring them into better agreement with observations. As a test case, we consider the specific example of SN 2017eaw, which shows that a nuclear burning episode is able to explain the light curve if it occurs ∼150-450 days prior to core-collapse. Due to the long timescale it takes for the low energy shock to traverse the star, this would manifest as a pre-SN outburst ∼50-350 days prior to the full-fledged SN. Applying work like this to other SNe will provide a direct connection between the SN and pre-SN outburst properties, which can be tested by future wide field surveys. In addition, we show that our models can qualitatively explain the short lived 'flash-ionization' lines seen in the early spectra of many Type II SNe.

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“…High-resolution images taken prior to explosion can be used to identify and characterize the properties of an SN progenitor (e.g., Smartt et al 2004;Maund & Smartt 2005, 2009Li et al 2007;Mattila et al 2008;Smartt 2009;Elias-Rosa et al 2010Fraser et al 2010Fraser et al , 2011Fraser et al , 2014Crockett et al 2011;Kochanek et al 2012Kochanek et al , 2017Maund et al 2013Maund et al , 2014Tomasella et al 2013;van Dyk 2017;Kilpatrick & Foley 2018;van Dyk et al 2019). We located pre-explosion HST observations in the Mikulski Archive for Space Telescopes (MAST) and analyzed them for the presence of a progenitor.…”

Section: Progenitor From Hst Pre-imagingmentioning

confidence: 99%

Discovery and Rapid Follow-up Observations of the Unusual Type II SN 2018ivc in NGC 1068

Bostroem

Valenti

Sand

et al. 2020

ApJ

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We present the discovery and high-cadence follow-up observations of SN2018ivc, an unusual SNe II that exploded in NGC1068 (D=10.1 Mpc). The light curve of SN2018ivc declines piecewise-linearly, changing slope frequently, with four clear slope changes in the first 30 days of evolution. This rapidly changing light curve indicates that interaction between the circumstellar material and ejecta plays a significant role in the evolution. Circumstellar interaction is further supported by a strong X-ray detection. The spectra are rapidly evolving and dominated by hydrogen, helium, and calcium emission lines. We identify a rare high-velocity emission-line feature blueshifted at ∼7800 km s 1 (in Hα, Hβ, Pβ, Pγ, He I, and Ca II), which is visible from day 18 until at least day 78 and could be evidence of an asymmetric progenitor or explosion. From the overall similarity between SN2018ivc and SN1996al, the Hα equivalent width of its parent H IIregion, and constraints from pre-explosion archival Hubble Space Telescope images, we find that the progenitor of SN2018ivc could be as massive as 52 M  but is more likely <12 M . SN2018ivc demonstrates the importance of the early discovery and rapid follow-up observations of nearby supernovae to study the physics and progenitors of these cosmic explosions.

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The Type II-plateau Supernova 2017eaw in NGC 6946 and Its Red Supergiant Progenitor

Cited by 71 publications

References 168 publications

The ‘red supergiant problem’: the upper luminosity boundary of Type II supernova progenitors

The ‘red supergiant problem’: the upper luminosity boundary of Type II supernova progenitors

The Influence of Late-stage Nuclear Burning on Red Supergiant Supernova Light Curves

Discovery and Rapid Follow-up Observations of the Unusual Type II SN 2018ivc in NGC 1068

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