JWST Reveals a Luminous Infrared Source at the Position of the Failed Supernova Candidate N6946-BH1

Beasor, Emma R.; Hosseinzadeh, Griffin; Smith, Nathan; Davies, Ben; Jencson, Jacob E.; Pearson, Jeniveve; Sand, David J.

doi:10.3847/1538-4357/ad21fa

Cited by 3 publications

(1 citation statement)

References 69 publications

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“…There is at least one recent example of a "failed supernova" candidate in which a source remained afterward but was highly reddened and fainter (Adams et al 2017;Beasor et al 2024;Kochanek et al 2024). As far as we are aware, though, there are no millimeter-wavelength observations of N6946-BH1, so we cannot (yet) make a direct comparison between it and the MUBLO.…”

Section: Supernovamentioning

confidence: 93%

A Broad Line-width, Compact, Millimeter-bright Molecular Emission Line Source near the Galactic Center

Ginsburg,

Bally,

Barnes

et al. 2024

ApJL

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A compact source, G0.02467–0.0727, was detected in Atacama Large Millimeter/submillimeter Array 3 mm observations in continuum and very broad line emission. The continuum emission has a spectral index α ≈ 3.3, suggesting that the emission is from dust. The line emission is detected in several transitions of CS, SO, and SO2 and exhibits a line width FWHM ≈ 160 km s−1. The line profile appears Gaussian. The emission is weakly spatially resolved, coming from an area on the sky ≲1″ in diameter (≲104 au at the distance of the Galactic center, GC). The centroid velocity is v LSR ≈ 40–50 km s−1, which is consistent with a location in the GC. With multiple SO lines detected, and assuming local thermodynamic equilibrium (LTE) conditions, the gas temperature is T LTE = 13 K, which is colder than seen in typical GC clouds, though we cannot rule out low-density, subthermally excited, warmer gas. Despite the high velocity dispersion, no emission is observed from SiO, suggesting that there are no strong (≳10 km s−1) shocks in the molecular gas. There are no detections at other wavelengths, including X-ray, infrared, and radio. We consider several explanations for the millimeter ultra-broad-line object (MUBLO), including protostellar outflow, explosive outflow, a collapsing cloud, an evolved star, a stellar merger, a high-velocity compact cloud, an intermediate-mass black hole, and a background galaxy. Most of these conceptual models are either inconsistent with the data or do not fully explain them. The MUBLO is, at present, an observationally unique object.

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Section: Supernovamentioning

confidence: 93%

A Broad Line-width, Compact, Millimeter-bright Molecular Emission Line Source near the Galactic Center

Ginsburg,

Bally,

Barnes

et al. 2024

ApJL

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Pre-supernova evolution and final fate of stellar mergers and accretors of binary mass transfer

Schneider,

Podsiadlowski,

Laplace

2024

A&A

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The majority of massive stars are expected to exchange mass or merge with a companion during their lives. This immediately implies that most supernovae (SNe) are from such post-mass-exchange objects. Here, we explore how mass accretion and merging affect the pre-SN structures of stars and their final fates. To this end, we modelled these complex processes by rapid mass accretion onto stars of different evolutionary stages and followed their evolution up to iron core collapse. We used the stellar evolution code and inferred the outcome of core-collapse using a neutrino-driven SN model. Our models cover initial masses from $11$ to $70\ and the accreted mass ranges from 10--200<!PCT!> of the initial mass. All models are non-rotating and for solar metallicity. The rapid accretion model offers a systematic way to approach the landscape of mass accretion and stellar mergers. It is naturally limited in scope and serves as a clean zeroth order baseline for these processes. We find that mass accretion, in particular onto post-main-sequence (post-MS) stars, can lead to a long-lived blue supergiant (BSG) phase during which stars burn helium in their cores. In comparison to genuine single stars, post-MS accretors have small core-to-total mass ratios, regardless of whether they end their lives as BSGs or cool supergiants (CSGs), and they can have genuinely different pre-SN core structures. As in single and binary-stripped stars, we find black-hole (BH) formation for the same characteristic CO core masses $M_ CO $ of $ and $ In models with the largest mass accretion, the BH formation landscape as a function of $M_ CO $ is shifted by about $0.5\ to lower masses such accretors are more difficult to explode. We find a tight relation between our neutron-star (NS) masses and the central entropy of the pre-SN models in all accretors and single stars, suggesting a universal relation that is independent of the evolutionary history of stars. Post-MS accretors explode both as BSGs and CSGs, and we show how to understand their pre-SN locations in the Hertzsprung--Russell (HR) diagram. Accretors exploding as CSGs can have much higher envelope masses than single stars. Some BSGs that avoid the luminous-blue-variable (LBV) regime in the HR diagram are predicted to collapse into BHs of up to $50\ while others explode in SNe and eject up to $40\ greatly exceeding ejecta masses from single stars. Both the BH and SN ejecta masses increase to about $80\ in our models when allowing for multiple mergers in initial triple-star systems, and they can be even higher at lower metallicities. Such high BH masses may fall into the pair-instability-SN mass gap and could help explain binary BH mergers involving very massive BHs as observed in GW190521. We further find that some of the BSG models explode as LBVs, which may lead to interacting SNe and possibly even superluminous SNe.

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The Two Alternative Explosion Mechanisms of Core-Collapse Supernovae: 2024 Status Report

Soker

2024

Universe

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In comparing the two alternative explosion mechanisms of core-collapse supernovae (CCSNe), I examine recent three-dimensional (3D) hydrodynamical simulations of CCSNe in the frame of the delayed neutrino explosion mechanism (neutrino mechanism) and argue that these valuable simulations show that neutrino heating can supply a non-negligible fraction of the explosion energy but not the observed energies, and hence cannot be the primary explosion mechanism. In addition to the energy crisis, the neutrino mechanism predicts many failed supernovae that are not observed. The most challenging issue of the neutrino mechanism is that it cannot account for point-symmetric morphologies of CCSN remnants, many of which were identified in 2024. These contradictions with observations imply that the neutrino mechanism cannot be the primary explosion mechanism of CCSNe. The alternative jittering jets explosion mechanism (JJEM) seems to be the primary explosion mechanism of CCSNe; neutrino heating boosts the energy of the jittering jets. Even if some simulations show explosions of stellar models (but usually with energies below that observed), it does not mean that the neutrino mechanism is the explosion mechanism. Jittering jets, which simulations do not include, can explode the core before the neutrino heating process does. Morphological signatures of jets in many CCSN remnants suggest that jittering jets are the primary driving mechanism, as expected by the JJEM.

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JWST Reveals a Luminous Infrared Source at the Position of the Failed Supernova Candidate N6946-BH1

Cited by 3 publications

References 69 publications

A Broad Line-width, Compact, Millimeter-bright Molecular Emission Line Source near the Galactic Center

A Broad Line-width, Compact, Millimeter-bright Molecular Emission Line Source near the Galactic Center

Pre-supernova evolution and final fate of stellar mergers and accretors of binary mass transfer

The Two Alternative Explosion Mechanisms of Core-Collapse Supernovae: 2024 Status Report

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