SN2017jgh - A high-cadence complete shock cooling lightcurve of a SN IIb with the Kepler telescope

P Armstrong, B E Tucker, A Rest, R Ridden-Harper, Y Zenati, A L Piro, S Hinton, C Lidman, S Margheim, G Narayan, E Shaya, P Garnavich, D Kasen, V Villar, A Zenteno, I Arcavi, M Drout, R J Foley, J Wheeler, J AnaisA Campillay, D Coulter, G Dimitriadis, D Jones, C D Kilpatrick, N Muñoz-Elgueta, C Rojas-Bravo, J Vargas-González, J Bulger, K Chambers, M Huber, T Lowe, E Magnier, B J Shappee, S Smartt, K W Smith, T Barclay, G Barentsen, J Dotson, M Gully-Santiago, C Hedges, S Howell, A Cody, K Auchettl, A Bódi, Zs Bognár, J Brimacombe, P Brown, B Cseh, L Galbany, D Hiramatsu, T W-S Holoien, D A Howell, S W Jha, R Könyves-Tóth, L Kriskovics, C McCully, P Milne, J Muñoz, Y Pan, A Pál, H Sai, K Sárneczky, N Smith, Á Sódor, R Szabó, R Szakáts, S Valenti, J Vinkó, X Wang, K Zhang, G Zsidi

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Abstract

SN 2017jgh is a type IIb supernova discovered by Pan-STARRS during the C16/C17 campaigns of the Kepler/K2 mission. Here we present the Kepler/K2 and ground based observations of SN 2017jgh, which captured the shock cooling of the progenitor shock breakout with an unprecedented cadence. This event presents a unique opportunity to investigate the progenitors of stripped envelope supernovae. By fitting analytical models to the SN 2017jgh lightcurve, we find that the progenitor of SN 2017jgh was likely a yellow supergiant with an envelope radius of ∼50 − 290 R⊙, and an envelope mass of ∼0 − 1.7 M⊙. SN 2017jgh likely had a shock velocity of ∼7500 − 10300 km s−1. Additionally, we use the lightcurve of SN 2017jgh to investigate how early observations of the rise contribute to constraints on progenitor models. Fitting just the ground based observations, we find an envelope radius of ∼50 − 330 R⊙, an envelope mass of ∼0.3 − 1.7 M⊙ and a shock velocity of ∼9, 000 − 15, 000 km s−1. Without the rise, the explosion time can not be well constrained which leads to a systematic offset in the velocity parameter and larger uncertainties in the mass and radius. Therefore, it is likely that progenitor property estimates through these models may have larger systematic uncertainties than previously calculated.
Original languageEnglish
Pages (from-to)3125–3138
Number of pages14
JournalMonthly Notices of the Royal Astronomical Society
Volume507
Issue number3
Early online date03 Aug 2021
DOIs
Publication statusPublished - 06 Sep 2021

Keywords

  • Space and Planetary Science
  • Astronomy and Astrophysics

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