A potential progenitor for the Type Ic supernova 2017ein

Kilpatrick, C. D.; Takaro, T.; Foley, R. J.; Leibler, C.; Pan, Y.-C.; Campbell, R.; Jacobson-Galán, Wynn V.; Lewis, Hilton; Lyke, James E.; Max, C. E.; Medallon, Sophia A.; Rest, A.

doi:10.1093/mnras/sty2022

Cited by 50 publications

(68 citation statements)

References 86 publications

(135 reference statements)

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“…Thus despite their high luminosities they may be challenging to observe, requiring ultraviolet, or very blue-sensitive optical, detectors. Supernova 2017ein, the only SN Ic to have a progenitor system identified so far, occurred at a redshift ∼0.0027, with the candidate identified in archival Hubble Space Telescope (HST) imaging (Van Dyk et al 2018;Kilpatrick et al 2018). The star, if single, had an absolute F555W magnitude of −7.5.…”

Section: Future Possibilitiesmentioning

confidence: 99%

“…Observed progenitors (in black) include the vanishing star N6946-BH1 (marked by a cross, Adams et al 2017), for which we have adjusted the luminosity to reflect an updated distance estimate (Eldridge & Xiao 2019), SN 1987A (marked by a star in the IIP section, Walborn et al 1987), several IIP SNe from Smartt (2015), type IIb and IIL SNe (both classified as II-other, and marked by dots and crosses respectively, Smartt 2015), SN 1993J (also a IIb event, Aldering et al 1994), the Ib progenitor of SN iPTF13bvn (Eldridge & Maund 2016) and finally the candidate Ic progenitor of SN 2017ein (Van Dyk et al 2018). The marked luminosity for 2017ein is an upper estimate, assuming that it was a single star (Kilpatrick et al 2018). This progenitor system is also indicated on the 'vanishing' panel (in purple) for reference.…”

Section: Classification Of Core-collapse Progenitor Modelsmentioning

confidence: 99%

See 1 more Smart Citation

Binary population synthesis models for core-collapse gamma-ray burst progenitors

Chrimes

Stanway

Eldridge

2019

Monthly Notices of the Royal Astronomical Society

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Long-duration gamma-ray bursts (GRBs) are understood to be the final fate for a subset of massive, stripped envelope, rapidly rotating stars. Beyond this, our knowledge of the progenitor systems is limited. Using the BPASS (Binary Population and Spectral Synthesis) stellar evolution models, we investigate the possibility that some massive stars in binaries can maintain the angular momentum required for jet production, while still loosing their outer envelope through winds or binary interactions. We find that a total hydrogen mass of M H < 5 × 10 −4 M and a helium ejecta mass fraction of F He < 0.20 provide the best thresholds for the supernova II/Ibc and Ib/Ic divisions respectively. Tidal interactions in binaries are accounted for by applying a tidal algorithm to post-process the stellar evolution models output by BPASS. We show that the observed volumetric gamma-ray burst rate evolution can be recreated using two distinct pathways and plausible distributions for burst parameters. In the first pathway, stars are spun up by mass accretion into a quasi-homogeneous state. In the second, tides maintain rotation where otherwise the star would spin down. Both lead to type Ic supernova progenitors, and a metallicity distribution consistent with the GRB host galaxy population. The inferred core angular momentum threshold for jet production is consistent with theoretical requirements for collapsars, given the assumptions made in our model. We can therefore reproduce several aspects of core collapse supernova/GRB observation and theory simultaneously. We discuss the predicted observable properties of GRB progenitors and their surviving companions.

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Section: Future Possibilitiesmentioning

confidence: 99%

Section: Classification Of Core-collapse Progenitor Modelsmentioning

confidence: 99%

Binary population synthesis models for core-collapse gamma-ray burst progenitors

Chrimes

Stanway

Eldridge

2019

Monthly Notices of the Royal Astronomical Society

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“…This suggestion was supported by the discovery of the disappearing ∼ 25M red supergiant in NGC 6946 that likely underwent a failed SN (Gerke et al 2015;Adams et al 2017). However, recent studies by Maund (2017Maund ( , 2018 of the resolved stellar populations around Type IIP and strippedenvelope SNe, as well as the discovery of a possible progenitor system for Type Ic SN 2017ein (Kilpatrick et al 2018), suggest that even progenitors 18M can produce observable explosions. However, due to a number of factors discussed in Smartt (2015), the discovery rate of progenitor stars associated with SNe is small.…”

Section: The Initial Mass Functionmentioning

confidence: 99%

Measurement of the Core-collapse Progenitor Mass Distribution of the Small Magellanic Cloud

Auchettl

Lopez

Badenes

et al. 2019

ApJ

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The physics of core-collapse (CC) supernovae (SNe) and how the explosions depend on progenitor properties are central questions in astronomy. For only a handful of SNe, the progenitor star has been identified in preexplosion images. Supernova remnants (SNRs), which are observed long after the original SN event, provide a unique opportunity to increase the number of progenitor measurements. Here, we systematically examine the stellar populations in the vicinities of 23 known SNRs in the Small Magellanic Cloud (SMC) using the star formation history (SFH) maps of Harris & Zaritsky (2004). We combine the results with constraints on the SNR metal abundances and environment from X-ray and optical observations. We find that 22 SNRs in the SMC have local SFHs and properties consistent with a CC explosion, several of which are likely to have been high-mass progenitors. This result supports recent theoretical findings that high-mass progenitors can produce successful explosions. We estimate the mass distribution of the CC progenitors and find that this distribution is similar to a Salpeter IMF (within the uncertainties), while this result is shallower than the mass distribution found in M31 and M33 by Jennings et al. (2014) and Díaz-Rodríguez et al. (2018) using a similar approach. Additionally, we find that a number of the SMC SNRs exhibit a burst of star formation between 50-200 Myr ago. As these sources are likely CC, this signature may be indicative of massive stars undergoing delayed CC as a consequence of binary interaction, rapid rotation, or low metallicity. In addition, the lack of Type Ia SNRs in the SMC is possibly a result of the short visibility times of these sources as they may fall below the sensitivity limits of current radio observations.

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“…This result was later disputed by Bersten et al (2014a). More recently, Van Dyk et al (2018), Kilpatrick et al (2018) and Xiang et al (2019) identified a source in archival Hubble Space Telescope (HST) images covering the location of the type Ic SN 2017ein, with properties compatible with a WR star of M ZAMS ∼55 M (although the presence of a companion star could not be ruled out).…”

Section: Introductionmentioning

confidence: 99%

SN 2016coi (ASASSN-16fp): An Energetic H-stripped Core-collapse Supernova from a Massive Stellar Progenitor with Large Mass Loss

Terreran¹,

Margutti²,

Bersier³

et al. 2019

ApJ

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We present comprehensive observations and analysis of the energetic H-stripped SN 2016coi (a.k.a. ASASSN-16fp), spanning the γ-ray through optical and radio wavelengths, acquired within the first hours to ∼420 days post explosion. Our observational campaign confirms the identification of He in the SN ejecta, which we interpret to be caused by a larger mixing of Ni into the outer ejecta layers. From the modeling of the broad bolometric light curve we derive a large ejecta mass to kinetic energy ratio (M ej ∼ 4 − 7 M , E k ∼ 7 − 8 × 10 51 erg). The small [Ca II] λλ7291,7324 to [O I] λλ6300,6364 ratio (∼0.2) observed in our latetime optical spectra is suggestive of a large progenitor core mass at the time of collapse. We find that SN 2016coi is a luminous source of X-rays (L X > 10 39 erg s −1 in the first ∼ 100 days post explosion) and radio emission (L 8.5 GHz ∼ 7 × 10 27 erg s −1 Hz −1 at peak). These values are in line with those of relativistic SNe (2 pre-explosion progenitor mass-loss with rateṀ ∼ (1 − 2) × 10 −4 M yr −1 and a sub-relativistic shock velocity v sh ∼ 0.15c, in stark contrast with relativistic SNe and similar to normal SNe. Finally, we find no evidence for a SN-associated shock breakout γ-ray pulse with energy E γ > 2 × 10 46 erg. While we cannot exclude the presence of a companion in a binary system, taken together, our findings are consistent with a massive single star progenitor that experienced large mass loss in the years leading up to core-collapse, but was unable to achieve complete stripping of its outer layers before explosion.

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A potential progenitor for the Type Ic supernova 2017ein

Cited by 50 publications

References 86 publications

Binary population synthesis models for core-collapse gamma-ray burst progenitors

Binary population synthesis models for core-collapse gamma-ray burst progenitors

Measurement of the Core-collapse Progenitor Mass Distribution of the Small Magellanic Cloud

SN 2016coi (ASASSN-16fp): An Energetic H-stripped Core-collapse Supernova from a Massive Stellar Progenitor with Large Mass Loss

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