Cas A and the Crab were not stellar binaries at death

Kochanek, C. S.

doi:10.1093/mnras/stx2423

Cited by 36 publications

(39 citation statements)

References 110 publications

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“…The Cas A supernova appears to have been a Type IIb based on light echo spectra which showed strong spectral similarities to the prototypical Type IIb event SN 1993J (Krause et al 2008;Rest et al 2008Rest et al , 2011. No surviving companion has been identified for Cas A, suggesting that if the system was a binary then either the two stars merged before the explosion, or the companion is a relatively faint, low mass dwarf star (Kochanek 2018;Kerzendorf et al 2019).…”

Section: Introductionmentioning

confidence: 93%

“…From pre-explosion images some SN IIb progenitors have been identified as yellow supergiants (e.g., SN 1993J, Aldering et al 1994SN 2011dh, Maund et al 2011Van Dyk et al 2011;SN 2013df, Van Dyk et al 2014andSN 2016gkg, Tartaglia et al 2017). In addition, for a handful of systems surviving companion candidates have been identified (e.g., SN 1993J, Maund et al 2004;Fox et al 2014;SN 2001ig, Ryder et al 2006, 2018andSN 2011dh, Folatelli et al 2014;Maund et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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Detection of the Red Supergiant Wind from the Progenitor of Cassiopeia A

Weil

Fesen

Patnaude

et al. 2020

ApJ

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Cassiopeia A (Cas A) is one of the best studied young Galactic supernova remnants. While providing a rare opportunity to study in detail the remnant of a Type IIb supernova, questions remain regarding the nature of its progenitor, its mass-loss history, and its pre-SN evolution. Here we present an optical investigation of the circumstellar environment around Cas A and find clumpy and filamentary Hα emission nebulosities concentrated 10-15 pc (10-15 arcminutes) to the north and east. First reported by Minkowski as a faint H II region, these nebulosities exhibit distinct morphological and spectroscopic properties relative to the surrounding diffuse emissions. Compared to neighboring H II regions, these nebulae show stronger [N II] 6548, 6583Å and [S II] 6716, 6731Å emissions relative to Hα. We show that Cas A's highest-velocity ejecta knots are interacting with some of the closest projected emission nebulae, thus providing strong evidence that these nebulae lie at the same distance as the remnant. We interpret these surrounding nebulosities to be the remains of the progenitor's red supergiant wind which accumulated against the southern edge of a large extended H II region located north of Cas A. Our findings are consistent with the view that Cas A's progenitor underwent considerable mass-loss, first from a fast main-sequence wind, then from a slower, clumpy red supergiant wind, and finally from a brief high-velocity wind, like that from a yellow supergiant.

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Section: Introductionmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Detection of the Red Supergiant Wind from the Progenitor of Cassiopeia A

Weil

Fesen

Patnaude

et al. 2020

ApJ

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“…Given the assumption that SN IIn light-curve bumps are caused by SN ejecta encountering denser regions of CSM, the rarity of such bumps is noteworthy. Modelling (e.g., Kochanek 2009) and observations (Sana et al 2012;Dunstall et al 2015;Kochanek 2018) suggest that at least 50% of massive stars reside in binary or multiple systems. In such binaries, the mass lost by the constituent stars can be shaped into spiral patterns (Tuthill et al 2008) which could cause light-curve bumps if one of the stars explodes as a CSI-dominated SN (as invoked by Schwarz & Pringle 1996.…”

Section: The Frequency Of Sn Iin Light-curve Bumpsmentioning

confidence: 99%

Type IIn supernova light-curve properties measured from an untargeted survey sample

Nyholm

Sollerman

Tartaglia

et al. 2020

A&A

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The evolution of a Type IIn supernova (SN IIn) is governed by the interaction between the SN ejecta and a hydrogen-rich circumstellar medium (CSM). SNe IIn thus allow us to probe the late-time mass-loss history of their progenitor stars. We present a sample of SNe IIn from the untargeted, magnitude-limited surveys of the Palomar Transient Factory (PTF) and its successor, the intermediate PTF (iPTF). To date, statistics on SN IIn optical light curve properties have generally been based on small ( 10 SNe) samples from targeted SN surveys. SNe IIn found and followed by the PTF/iPTF were used to select a sample of 42 events with useful constraints on the rise times as well as with available post-peak photometry. The SNe were discovered in 2009-2016 and have at least one low-resolution classification spectrum, as well as photometry from the P48 and P60 telescopes at Palomar Observatory. We study the light-curve properties of these SNe IIn using spline fits (for the peak and the declining portion) and template matching (for the rising portion). We study the peak-magnitude distribution, rise times, decline rates, colour evolution, host galaxies, and K-corrections of the SNe in our sample. We find that the typical rise times are divided into fast and slow risers as 20 ± 8 d and 50 ± 15 d, respectively. The decline rates could possibly be divided into two groups (with slopes 0.013 ± 0.008 mag d −1 and 0.040 ± 0.014 mag d −1 ), but this division has weak statistical significance. We find no significant correlation between the peak luminosity of SNe IIn and their rise times, but the more luminous SNe IIn are generally found to be more durable and the slowly rising SNe IIn are generally found to be slowly declining. The SNe in our sample were hosted by galaxies of absolute magnitude −22 Mg −13 mag. The K-corrections at light-curve peak of the SNe in our sample are found to be within 0.2 mag for the observer's frame r-band, for SNe IIn at redshifts z < 0.25. Applying K-corrections and including also ostensibly "superluminous" SNe IIn, we find that the peak magnitudes are M r peak = −19.18 ± 1.32 mag. We conclude that the occurrence of conspicuous light-curve bumps in SNe IIn, such as in iPTF13z, is limited to 1.4 +14.6 −1.0 % of the SNe IIn. We also investigate a possible subtype of SNe IIn with a fast rise to a 50 d plateau followed by a slow, linear decline. iPTF13agz, iPTF13aki, iPTF13asr, iPTF13cuf, iPTF14bcw, iPTF14bpa, iPTF15aym, iPTF15bky, iPTF15blp, iPTF15eqr, iPTF16fb. ⋆ Based in part on observations made with the Palomar Transient Factory and intermediate Palomar Transient Factory surveys.

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“…So far, none of these searches for companions of Type II SNe resulted in a detection, establishing upper limits on possible companions for the Type II-P SN 2005cs Li et al 2006), the Type II-P SN 2008bk (Mattila et al 2008) and for the Type II-peculiar SN1987A (Kochanek 2017). In addition, the Crab, which was probably a Type II SN, seems to lack a surviving companion (Kochanek 2018). Thus, our predictions are consistent with the so-far lack Article number, page 17 of 19 A&A proofs: manuscript no.…”

Section: No Stellar Companions Expected For Type II Snementioning

confidence: 99%

The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: the role of binary interaction

Zapartas

Mink

Justham

et al. 2019

A&A

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Hydrogen-rich supernovae, known as Type II (SNe II), are the most common class of explosions observed following the collapse of the core of massive stars. We use analytical estimates and population synthesis simulations to assess the fraction of SNe II progenitors that are expected to have exchanged mass with a companion prior to explosion. We estimate that 1/3 to 1/2 of SN II progenitors have a history of mass exchange with a binary companion before exploding. The dominant binary channels leading to SN II progenitors involve the merger of binary stars. Mergers are expected to produce a diversity of SN II progenitor characteristics, depending on the evolutionary timing and properties of the merger. Alternatively, SN II progenitors from interacting binaries may have accreted mass from their companion, and subsequently been ejected from the binary system after their companion exploded. We show that the overall fraction of SN II progenitors that are predicted to have experienced binary interaction is robust against the main physical uncertainties in our models. However, the relative importance of different binary evolutionary channels is affected by changing physical assumptions. We further discuss ways in which binarity might contribute to the observed diversity of SNe II by considering potential observational signatures arising from each binary channel. For supernovae which have a substantial H-rich envelope at explosion (i.e., excluding Type IIb SNe), a surviving non-compact companion would typically indicate that the supernova progenitor star was in a wide, non-interacting binary. We argue that a significant fraction of even Type II-P SNe are expected to have gained mass from a companion prior to explosion.

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Cas A and the Crab were not stellar binaries at death

Cited by 36 publications

References 110 publications

Detection of the Red Supergiant Wind from the Progenitor of Cassiopeia A

Detection of the Red Supergiant Wind from the Progenitor of Cassiopeia A

Type IIn supernova light-curve properties measured from an untargeted survey sample

The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: the role of binary interaction

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