THE TYPE IIb SUPERNOVA 2013df AND ITS COOL SUPERGIANT PROGENITOR

Dyk, Schuyler D. Van; Zheng, W.; Fox, O.; Cenko, S. B.; Clubb, K. I.; Filippenko, A. V.; Foley, R. J.; Miller, A. A.; Smith, Nathan; Kelly, Patrick L.; Lee, William H.; Ben-Ami, Sagi; Gal‐Yam, A.

doi:10.1088/0004-6256/147/2/37

Cited by 124 publications

(111 citation statements)

References 77 publications

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“…We first present earlytime data on the SN itself and compare its properties to those of other well-studied SNe Ic, in particular SN 2007gr. We then show our detection of a candidate for the progenitor in archival Hubble Space Telescope (HST) images, which we isolated with high spatial resolution HST images of the SN; we initially reported this identification in Van Dyk et al (2017). Finally, we attempt to constrain the nature of the detected progenitor and compare these properties to predictions from the recent models of SESN progenitors.…”

Section: Introductionmentioning

confidence: 90%

“…The situation is less clear for SNe whose progenitor has had its H-rich envelope partially or entirely stripped away before explosion, the so-called strippedenvelope SNe (SESNe; e.g., Filippenko 1997). We now have accumulating evidence that the progenitors of Type IIb SNe (SNe IIb), stripped but still retaining 0.1 M e of hydrogen, appear to be yellow to somewhat blue supergiants (e.g., Maund et al 2011;van Dyk et al 2011van Dyk et al , 2014Folatelli et al 2015;Bersten et al 2018), likely in interacting binary systems of moderate mass (∼12-15 M e ; e.g., Podsiadlowski et al 1993;Stancliffe & Eldridge 2009;Benvenuto et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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SN 2017ein and the Possible First Identification of a Type Ic Supernova Progenitor

Dyk

Zheng

Brink

et al. 2018

ApJ

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We have identified a progenitor candidate in archival Hubble Space Telescope (HST) images for the Type Ic supernova (SN Ic) SN 2017ein in NGC 3938, pinpointing the candidate's location via HST Target of Opportunity imaging of the SN itself. This would be the first identification of a stellar-like object as a progenitor candidate for any SN Ic to date. We also present observations of SN 2017ein during the first ∼49 days since explosion. We find that SN 2017ein most resembles the well-studied SN Ic SN 2007gr. We infer that SN 2017ein experienced a total visual extinction of A V ≈1.0-1.9 mag, predominantly because of dust within the host galaxy. Although the distance is not well known, if this object is the progenitor, it was likely of high initial mass, ∼47-48 M e if a single star, or ∼60-80 M e if in a binary system. However, we also find that the progenitor candidate could be a very blue and young compact cluster, further implying a very massive (>65 M e ) progenitor. Furthermore, the actual progenitor might not be associated with the candidate at all and could be far less massive. From the immediate stellar environment, we find possible evidence for three different populations; if the SN progenitor was a member of the youngest population, this would be consistent with an initial mass of ∼57 M e . After it has faded, the SN should be reobserved at high spatial resolution and sensitivity, to determine whether the candidate is indeed the progenitor.

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Section: Introductionmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

SN 2017ein and the Possible First Identification of a Type Ic Supernova Progenitor

Dyk

Zheng

Brink

et al. 2018

ApJ

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“…The first spectrum, obtained by Cenko et al (2013), showed clear resemblance to the early spectra of SN 1993J, which suggested that SN 2013df was a SN IIb. This suspicion was verified by Van Dyk et al (2014) (hereafter VD14), who presented early photometric and spectroscopic data and reached conclusions concerning the properties of the progenitor, identifying it as a yellow supergiant star with an estimated initial mass of Min ∼13-17 M⊙, an effective temperature of T eff ∼4250 K, and an initial radius of R eff ∼545 R⊙. Morales-Garoffolo et al (2014) (hereafter MG14) presented a detailed analysis of early UV-optical light curves and some spectra, including nebular ones.…”

Section: Introductionmentioning

confidence: 84%

“…The quasibolometric light curve was derived by integrating the dered- . d Calculated in this work, adopted parameters: t 0 = 2,456,447.8 ± 0.5, E(B − V ) = 0.09 ± 0.01 mag, µ 0 = 31.10 ± 0.05 mag (Freedman et al 2001;Van Dyk et al 2014).…”

Section: Analysis Of the Early Bolometric Light Curvementioning

confidence: 99%

The continuing story of SN IIb 2013df: new optical and IR observations and analysis

Szalai

Vinkó

Nagy

et al. 2016

Mon. Not. R. Astron. Soc.

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SN 2013df is a nearby Type IIb supernova that seems to be the spectroscopic twin of the well-known SN 1993J. Previous studies revealed many, but not all interesting properties of this event. Our goal was to add new understanding of both the early and late-time phases of SN 2013df. Our spectral analysis is based on 6 optical spectra obtained with the 9.2m Hobby-Eberly Telescope during the first month after explosion, complemented by a near-infrared spectrum. We applied the SYNAPPS spectral synthesis code to constrain the chemical composition and physical properties of the ejecta. A principal result is the identification of "high-velocity" He I lines in the early spectra of SN 2013df, manifest as the blue component of the double-troughed profile at ∼5650Å. This finding, together with the lack of clear separation of H and He lines in velocity space, indicates that both H and He features form at the outer envelope during the early phases. We also obtained ground-based BVRI and g ′ r ′ i ′ z ′ photometric data up to +45 days and unfiltered measurements with the ROTSE-IIIb telescope up to +168 days. From the modelling of the early-time quasi-bolometric light curve, we find M ej ∼ 3.2−4.6 M ⊙ and E kin ∼ 2.6−2.8 × 10 51 erg for the initial ejecta mass and the initial kinetic energy, respectively, which agree well with the values derived from the separate modelling of the light-curve tail. Late-time mid-infrared excess indicates circumstellar interaction starting ∼1 year after explosion, in accordance with previously published optical, X-ray, and radio data.

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“…Prior to 2009, fourteen CCSN progenitor stars or progenitor outbursts (eight SNe II-P, three IIb, one IIn, one Ibn, and one II-pec) had been detected in pre-explosion images (Smartt 2009, and references therein). Over the last few years, at least six more (IIn: 1961V, 2009ip, 2010jl;IIb: 2011dh, 2013df; IIn-P: 2011ht) have been found (Smith et al 2010a(Smith et al , 2011aKochanek et al 2011;Foley et al 2011;Maund et al 2011;Van Dyk et al 2014;Fraser et al 2013a). Detection of these progenitors is crucial for gaining a better understanding of the observed SN diversity.…”

Section: Introductionmentioning

confidence: 99%

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

Bilinski¹,

Smith²,

Li³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We searched through roughly 12 years of archival survey data acquired by the Katzman Automatic Imaging Telescope (KAIT) as part of the Lick Observatory Supernova Search (LOSS) in order to detect or place limits on possible progenitor outbursts of Type IIn supernovae (SNe IIn). The KAIT database contains multiple pre-SN images for 5 SNe IIn (plus one ambiguous case of a SN IIn/imposter) within 50 Mpc. No progenitor outbursts are found using the false discovery rate (FDR) statistical method in any of our targets. Instead, we derive limiting magnitudes (LMs) at the locations of the SNe. These limiting magnitudes (typically reaching m R ≈ 19.5 mag) are compared to outbursts of SN 2009ip and η Car, plus additional simulated outbursts. We find that the data for SN 1999el and SN 2003dv are of sufficient quality to rule out events ∼ 40 days before the main peak caused by initially faint SNe from blue supergiant (BSG) precursor stars, as in the cases of SN 2009ip and SN 2010mc. These SNe IIn may thus have arisen from red supergiant progenitors, or they may have had a more rapid onset of circumstellar matter interaction. We also estimate the probability of detecting at least one outburst in our dataset to be 60% for each type of the example outbursts, so the lack of any detections suggests that such outbursts are either typically less luminous (intrinsically or owing to dust) than ∼ −13 mag, or not very common among SNe IIn within a few years prior to explosion.

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THE TYPE IIb SUPERNOVA 2013df AND ITS COOL SUPERGIANT PROGENITOR

Cited by 124 publications

References 77 publications

SN 2017ein and the Possible First Identification of a Type Ic Supernova Progenitor

SN 2017ein and the Possible First Identification of a Type Ic Supernova Progenitor

The continuing story of SN IIb 2013df: new optical and IR observations and analysis

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

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