Light Curves of the Type II-P Supernova SN 2017eaw: The First 200 Days

Tsvetkov, D. Yu.; Shugarov, S. Yu.; Volkov, I. M.; Pavlyuk, N. N.; Vozyakova, O. V.; Shatsky, N. I.; Nikiforova, A. A.; Troitsky, I. S.; Troitskaya, Yu. V.; Бакланов, П. В.

doi:10.1134/s1063773718050043

Cited by 30 publications

(27 citation statements)

References 21 publications

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“…Distance reaches (in kpc), defined as the distance with a 50% detection efficiency, for neutrino-driven explosions from Müller (mul1-mul3), Ott (ott1) and Yakunin (yak1-yak4), as well as MHD-driven explosions from Scheidegger (sch1-sch3) and Dimmelmeier (dim1-dim3). [58], respectively. The current GW constraints at low frequencies are comparable with these values.…”

Section: B Constraints On Gw Energy Emissionmentioning

confidence: 97%

“…This is the closest CCSN considered in the search. The analyses in [57][58][59] provide indication that the progenitor was a red supergiant with an estimated initial mass of 13 M and radius of 4000 R . SN 2017gax (DLT17ch), a type-Ib/c supernova, was discovered by the DLT40 on 2017 August 14.71 UTC [41].…”

Section: Targeted Core-collapse Supernovaementioning

confidence: 97%

“…As a consequence, we can extrapolate backward in time from the moment when explosion was caught in the optical bands in order to estimate t 1 and t 2 . Since the interval between t disc − t Null for SN 2017eaw was greater than a week and because SN 2017eaw follow-up observations allow it [57,58], we used the EPM to calculate the OSW. Noise Amplitude…”

Section: Targeted Core-collapse Supernovaementioning

confidence: 99%

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Optically targeted search for gravitational waves emitted by core-collapse supernovae during the first and second observing runs of advanced LIGO and advanced Virgo

Abbott¹,

Abbott²,

Abbott³

et al. 2020

Phys. Rev. D

108

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We present the results from a search for gravitational-wave transients associated with core-collapse supernovae observed within a source distance of approximately 20 Mpc during the first and second observing runs of Advanced LIGO and Advanced Virgo. No significant gravitational-wave candidate was detected. We report the detection efficiencies as a function of the distance for waveforms derived from multidimensional numerical simulations and phenomenological extreme emission models. For neutrino-driven explosions the distance at which we reach 50% detection efficiency is approaching 5 kpc, and for magnetorotationally-driven explosions is up to 54 kpc. However, waveforms for extreme emission models are detectable up to 28 Mpc. For the first time, the gravitational-wave data enabled us to exclude part of the parameter spaces of two extreme emission models with confidence up to 83%, limited by coincident data coverage. Besides, using ad hoc harmonic signals windowed with Gaussian envelopes we constrained the gravitational-wave energy emitted during core-collapse at the levels of 4.27 × 10 −4 M c 2 and 1.28 × 10 −1 M c 2 for emissions at 235 Hz and 1304 Hz respectively. These constraints are two orders of magnitude more stringent than previously derived in the corresponding analysis using initial LIGO, initial Virgo and GEO 600 data.

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Section: B Constraints On Gw Energy Emissionmentioning

confidence: 97%

Section: Targeted Core-collapse Supernovaementioning

confidence: 97%

Section: Targeted Core-collapse Supernovaementioning

confidence: 99%

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Optically targeted search for gravitational waves emitted by core-collapse supernovae during the first and second observing runs of advanced LIGO and advanced Virgo

Abbott¹,

Abbott²,

Abbott³

et al. 2020

Phys. Rev. D

108

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“…In this study, we take photometric data and Fe ii λ5169 Å line velocities from Szalai et al (2019). Additional optical photometry can also be found in Tsvetkov et al (2018), Van Dyk et al (2019, Rui et al (2019), andButa &Keel (2019).…”

Section: Sn 2017eawmentioning

confidence: 99%

Progenitor properties of type II supernovae: fitting to hydrodynamical models using Markov chain Monte Carlo methods

Martínez

Bersten

Anderson

et al. 2020

A&A

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Context. The progenitor and explosion properties of type II supernovae (SNe II) are fundamental to understanding the evolution of massive stars. Particular attention has been paid to the initial masses of their progenitors, but despite the efforts made, the range of initial masses is still uncertain. Direct imaging of progenitors in pre-explosion archival images suggests an upper initial mass cutoff of ∼18 M⊙. However, this is in tension with previous studies in which progenitor masses inferred by light-curve modelling tend to favour high-mass solutions. Moreover, it has been argued that light-curve modelling alone cannot provide a unique solution for the progenitor and explosion properties of SNe II. Aims. We develop a robust method which helps us to constrain the physical parameters of SNe II by simultaneously fitting their bolometric light curve and the evolution of the photospheric velocity to hydrodynamical models using statistical inference techniques. Methods. We created pre-supernova red supergiant models using the stellar evolution code MESA, varying the initial progenitor mass. We then processed the explosion of these progenitors through hydrodynamical simulations, where we changed the explosion energy and the synthesised nickel mass together with its spatial distribution within the ejecta. We compared the results to observations using Markov chain Monte Carlo methods. Results. We apply this method to a well-studied set of SNe with an observed progenitor in pre-explosion images and compare with results in the literature. Progenitor mass constraints are found to be consistent between our results and those derived by pre-SN imaging and the analysis of late-time spectral modelling. Conclusions. We have developed a robust method to infer progenitor and explosion properties of SN II progenitors which is consistent with other methods in the literature. Our results show that hydrodynamical modelling can be used to accurately constrain the physical properties of SNe II. This study is the starting point for a further analysis of a large sample of hydrogen-rich SNe.

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“…SN 2017eaw was discovered on 2017 May 14.238 (UT) (Wiggins 2017;Dong & Stanek 2017) and reached a peak V magnitude of 12.8. Its light curve and spectroscopic evolution followed that of a normal SN II-P (Cheng et al 2017;Xiang et al 2017;Tomasella et al 2017;Tsvetkov et al 2018;Szalai et al 2019;Van Dyk et al 2019;Buta & Keel 2019).…”

mentioning

confidence: 83%

Detection of Late-Time Circumstellar Interaction of SN 2017eaw in NGC 6946

Weil,

Fesen,

Patnaude

et al. 2020

Preprint

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SN 2017eaw, the tenth supernova observed in NGC 6946, was a normal Type II-P supernova with an estimated 11 -13 M red supergiant progenitor. Here we present nebular phase spectra of SN 2017eaw at +545 and +900 days post-max, extending approximately 50 -400 days past the epochs of previously published spectra. While the +545 day spectra is similar to spectra taken between days +400 and +493, the +900 day spectrum shows dramatic changes both in spectral features and emission line profiles. The Hα emission is flat-topped and box-like with sharp blue and red profile velocities of −8000 and +7500 km s −1 . These late-time spectral changes indicate strong circumstellar interaction with a mass-loss shell, expelled ∼ 1700 years before explosion. SN 2017eaw's +900 day spectrum is similar to those seen for SN 2004et and SN 2013ej observed 2 -3 years after explosion. We discuss the importance of late-time monitoring of bright SNe II-P and the nature of pre-supernova mass-loss events for SN II-P evolution.

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Light Curves of the Type II-P Supernova SN 2017eaw: The First 200 Days

Cited by 30 publications

References 21 publications

Optically targeted search for gravitational waves emitted by core-collapse supernovae during the first and second observing runs of advanced LIGO and advanced Virgo

Optically targeted search for gravitational waves emitted by core-collapse supernovae during the first and second observing runs of advanced LIGO and advanced Virgo

Progenitor properties of type II supernovae: fitting to hydrodynamical models using Markov chain Monte Carlo methods

Detection of Late-Time Circumstellar Interaction of SN 2017eaw in NGC 6946

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