THE PROGENITOR OF THE TYPE IIb SN 2008ax REVISITED

Folatelli, G.; Bersten, Melina C.; Kuncarayakti, H.; Benvenuto, O. G.; Maeda, Keiichi; Nomoto, Ken’ichi

doi:10.1088/0004-637x/811/2/147

Cited by 74 publications

(82 citation statements)

References 49 publications

(88 reference statements)

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“…Their progenitors (or strong candidates) have also been identified (Maund et al 2004(Maund et al , 2011Van Dyk et al 2014;Folatelli et al 2015). In Table 1, characteristic properties of these progenitors are listed.…”

Section: Introductionmentioning

confidence: 94%

Radii and Mass-loss Rates of Type IIb Supernova Progenitors

Ouchi

Maeda

2017

ApJ

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Several Type IIb supernovae (SNe IIb) have been extensively studied, both in terms of the progenitor radius and the mass-loss rate in the final centuries before the explosion. While the sample is still limited, evidence has been accumulating that the final mass-loss rate tends to be larger for a more extended progenitor, with the difference exceeding an order of magnitude between the more and less extended progenitors. The high mass-loss rates inferred for the more extended progenitors are not readily explained by a prescription commonly used for a single stellar wind. In this paper, we calculate a grid of binary evolution models. We show that the observational relation in the progenitor radii and mass-loss rates may be a consequence of non-conservative mass transfer in the final phase of progenitor evolution without fine tuning. Further, we find a possible link between SNe IIb and SNe IIn. The binary scenario for SNe IIb inevitably leads to a population of SN progenitors surrounded by dense circumstellar matter (CSM) due to extensive mass loss (Ṁ 10 −4 M ⊙ yr −1 ) in the binary origin. About 4 % of all observed SNe IIn are predicted to have dense CSM, produced by binary non-conservative mass transfer, whose observed characteristics are distinguishable from SNe IIn from other scenarios. Indeed, such SNe may be observationally dominated by systems experiencing huge mass loss in the final 10 3 yr, leading to luminous SNe IIn or initially bright SNe IIP or IIL with a characteristics of SNe IIn in their early spectra.

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Section: Introductionmentioning

confidence: 94%

Radii and Mass-loss Rates of Type IIb Supernova Progenitors

Ouchi

Maeda

2017

ApJ

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“…39 [103,104]. Most recent observations and phenomenological modeling by [105] suggest that the progenitor was in a binary system and may have had a blue-supergiant appearance and an extended (30 − 40 R ) low-density (thus, low-mass) hydrogen-rich envelope at the time of explosion. To be conservative, we add an additional day to account for the uncertainty in shock propagation time and define the GW on-source window as II.…”

Section: Identifiermentioning

confidence: 99%

First targeted search for gravitational-wave bursts from core-collapse supernovae in data of first-generation laser interferometer detectors

Abbott¹,

Abbott²,

Abbott³

et al. 2016

Phys. Rev. D

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We present results from a search for gravitational-wave bursts coincident with two core-collapse supernovae observed optically in 2007 and 2011. We employ data from the Laser Interferometer Gravitational-wave Observatory (LIGO), the Virgo gravitational-wave observatory, and the GEO 600 gravitational-wave observatory. The targeted core-collapse supernovae were selected on the basis of (1) proximity (within approximately 15 Mpc), (2) tightness of observational constraints on the time of core collapse that defines the gravitational-wave search window, and (3) coincident operation of 6 at least two interferometers at the time of core collapse. We find no plausible gravitational-wave candidates. We present the probability of detecting signals from both astrophysically well-motivated and more speculative gravitational-wave emission mechanisms as a function of distance from Earth, and discuss the implications for the detection of gravitational waves from core-collapse supernovae by the upgraded Advanced LIGO and Virgo detectors.

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“…Aldering et al 1994;Maund et al 2004;van Dyk et al 2011;Folatelli et al 2014;Fox et al 2014;Maeda et al 2014;Folatelli et al 2015), and a WR progenitor was ruled out for SN 2008ax (Folatelli et al 2015) although the proposed binary companion of the SN 2011dh progenitor was disputed by Maund et al (2015a). Maeda et al (2015) found that the more extended progenitors may still be undergoing binary interaction, while for the less extended ones this phase would be over.…”

Section: Introductionmentioning

confidence: 99%

“…Maeda et al (2015) found that the more extended progenitors may still be undergoing binary interaction, while for the less extended ones this phase would be over. The detected type IIb progenitors have been identified as yellow or blue supergiants (YSGs or BSGs, respectively) with initial masses between 13 and 19 M (van Maund et al 2011;van Dyk et al 2014;Folatelli et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Core-collapse supernova progenitor constraints using the spatial distributions of massive stars in local galaxies

Kangas

Portinari

Mattila

et al. 2017

A&A

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We study the spatial correlations between the H α emission and different types of massive stars in two local galaxies, the Large Magellanic Cloud (LMC) and Messier 33. We compare these to correlations derived for core-collapse supernovae (CCSNe) in the literature to connect CCSNe of different types with the initial masses of their progenitors and to test the validity of progenitor mass estimates which use the pixel statistics method. We obtain samples of evolved massive stars in both galaxies from catalogues with good spatial coverage and/or completeness, and combine them with coordinates of main-sequence stars in the LMC from the SIMBAD database. We calculate the spatial correlation of stars of different classes and spectral types with H α emission. We also investigate the effects of distance, noise and positional errors on the pixel statistics method. A higher correlation with H α emission is found to correspond to a shorter stellar lifespan, and we conclude that the method can be used as an indicator of the ages, and therefore initial masses, of SN progenitors. We find that the spatial distributions of type II-P SNe and red supergiants of appropriate initial mass ( 9 M ) are consistent with each other. We also find the distributions of type Ic SNe and WN stars with initial masses 20 M consistent, while supergiants with initial masses around 15 M are a better match for type IIb and II-L SNe. The type Ib distribution corresponds to the same stellar types as type II-P, which suggests an origin in interacting binaries. On the other hand, we find that luminous blue variable stars show a much stronger correlation with H α emission than do type IIn SNe.

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THE PROGENITOR OF THE TYPE IIb SN 2008ax REVISITED

Cited by 74 publications

References 49 publications

Radii and Mass-loss Rates of Type IIb Supernova Progenitors

Radii and Mass-loss Rates of Type IIb Supernova Progenitors

First targeted search for gravitational-wave bursts from core-collapse supernovae in data of first-generation laser interferometer detectors

Core-collapse supernova progenitor constraints using the spatial distributions of massive stars in local galaxies

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