An extremely energetic supernova from a very massive star in a dense medium

Nicholl, M.; Blanchard, P. K.; Berger, E.; Chornock, R.; Margutti, R.; Gómez, Sebastián; Lunnan, R.; Miller, A. A.; Fong, W.; Terreran, G.; Vigna-Gómez, Alejandro; Bhirombhakdi, Kornpob; Bieryla, Allyson; Challis, P.; Laher, Russ R.; Masci, Frank J.; Paterson, K.

doi:10.1038/s41550-020-1066-7

Cited by 57 publications

(58 citation statements)

References 96 publications

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“…12 16 ( ) reaction rate. If the existence of PPISNe can be confirmed though photometric observations (for instance, candidate PPISN SN 2006gy (Woosley et al 2007), SN 2006jc (Pastorello et al 2007, SN iPTF14hls (Arcavi et al 2017;Woosley 2018;Vigna-Gómez et al 2019), SN iPTF16eh (Lunnan et al 2018), SN 2016iet (Gomez et al 2019), or SN 2016aps (Nicholl et al 2020)) then we can place a lower limit on the a g C , O…”

Section: C12mentioning

confidence: 96%

Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the ¹²C(α, γ)¹⁶O Rate

Farmer

Renzo

Mink

et al. 2020

ApJL

197

171

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Gravitational-wave detections are starting to allow us to probe the physical processes in the evolution of very massive stars through the imprints they leave on their final remnants. Stellar evolution theory predicts the existence of a gap in the black hole mass distribution at high mass due to the effects of pair instability. Previously, we showed that the location of the gap is robust against model uncertainties, but it does depend sensitively on the uncertain a g C , O 12 16 300. Degeneracies with other model uncertainties need to be investigated further, but probing nuclear stellar astrophysics poses a promising science case for the future gravitational-wave detectors.

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Section: C12mentioning

confidence: 96%

Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the ¹²C(α, γ)¹⁶O Rate

Farmer

Renzo

Mink

et al. 2020

ApJL

197

171

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“…A better fit with a Lorentzian function indicates that broadening is due to electron scattering rather than expansion (e.g. Chatzopoulos et al 2011;Taddia et al 2013;Nicholl et al 2020). However, as a Lorentzian is not a significantly better fit, this scenario is not supported.…”

Section: Photospheric H α Profilementioning

confidence: 97%

SN 2019hcc: a Type II supernova displaying early O ii lines

Parrag

Inserra

Schulze

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present optical spectroscopy together with ultraviolet, optical and near-infrared photometry of SN 2019hcc, which resides in a host galaxy at redshift 0.044, displaying a sub-solar metallicity. The supernova spectrum near peak epoch shows a ‘w’ shape at around 4000 Åwhich is usually associated with O ii lines and is typical of Type I superluminous supernovae. SN 2019hcc post-peak spectra show a well-developed Hα P-Cygni profile from 19 days past maximum and its light curve, in terms of its absolute peak luminosity and evolution, resembles that of a fast-declining Hydrogen-rich supernova (SN IIL). The object does not show any unambiguous sign of interaction as there is no evidence of narrow lines in the spectra or undulations in the light curve. Our tardis spectral modelling of the first spectrum shows that Carbon, Nitrogen and Oxygen (CNO) at 19000 K reproduce the ‘w’ shape and suggests that a combination of non-thermally excited CNO and metal lines at 8000 K could reproduce the feature seen at 4000 Å. The Bolometric light curve modelling reveals that SN 2019hcc could be fit with a magnetar model, showing a relatively strong magnetic field (B>3 × 1014G), which matches the peak luminosity and rise time without powering up the light curve to superluminous luminosities. The high-energy photons produced by the magnetar would then be responsible for the detected O ii lines. As a consequence, SN 2019hcc shows that a ‘w’ shape profile at around 4000 Å, usually attributed to O ii, is not only shown in superluminous supernovae and hence it should not be treated as the sole evidence of the belonging to such a supernova type.

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“…) and broad light curves (rise times as long as ∼150 days) as a consequence of the large ejecta masses, and therefore, long diffusion times (e.g., Dessart et al 2013;Kozyreva et al 2014). A number of observed events have been associated with PISNe, including SN 2006gy (Smith et al 2007), SN2007bi (Gal-Yam et al 2009), SN 2213-1745(Cooke et al 2012, OGLE14-073 (Terreran et al 2017), SN 2016iet (Gomez et al 2019), and SN2016aps (Nicholl et al 2020). Several of these candidates have been observed at low redshift, implying that potential formation pathways for PISNe do indeed exist for highermetallicity Population I/II stars.…”

Section: Observational Prospectsmentioning

confidence: 99%

Populating the Upper Black Hole Mass Gap through Stellar Collisions in Young Star Clusters

Kremer

Spera

Becker

et al. 2020

ApJ

146

117

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Theoretical modeling of massive stars predicts a gap in the black hole (BH) mass function above ∼40-50 M e for BHs formed through single star evolution, arising from (pulsational) pair-instability supernovae (PISNe). However, in dense star clusters, dynamical channels may exist that allow construction of BHs with masses in excess of those allowed from single star evolution. The detection of BHs in this so-called "upper-mass gap" would provide strong evidence for the dynamical processing of BHs prior to their eventual merger. Here, we explore in detail the formation of BHs with masses within or above the pair-instability gap through collisions of young massive stars in dense star clusters. We run a suite of 68 independent cluster simulations, exploring a variety of physical assumptions pertaining to growth through stellar collisions, including primordial cluster mass segregation and the efficiency of envelope stripping during collisions. We find that as many as ∼20% of all BH progenitors undergo one or more collisions prior to stellar collapse and up to ∼1% of all BHs reside within or above the pair-instability gap through the effects of these collisions. We show that these BHs readily go on to merge with other BHs in the cluster, creating a population of massive BH mergers at a rate that may compete with the "multiple-generation" merger channel described in other analyses. This has clear relevance for the formation of very massive BH binaries as recently detected by the Laser Interferometer Gravitational-Wave Observatory/Virgo in GW190521. Finally, we describe how stellar collisions in clusters may provide a unique pathway to PISNe and briefly discuss the expected rate of these events and other electromagnetic transients.

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An extremely energetic supernova from a very massive star in a dense medium

Cited by 57 publications

References 96 publications

Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the ¹²C(α, γ)¹⁶O Rate

Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the ¹²C(α, γ)¹⁶O Rate

SN 2019hcc: a Type II supernova displaying early O ii lines

Populating the Upper Black Hole Mass Gap through Stellar Collisions in Young Star Clusters

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An extremely energetic supernova from a very massive star in a dense medium

Cited by 57 publications

References 96 publications

Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the 12C(α, γ)16O Rate

Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the 12C(α, γ)16O Rate

SN 2019hcc: a Type II supernova displaying early O ii lines

Populating the Upper Black Hole Mass Gap through Stellar Collisions in Young Star Clusters

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Product

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Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the ¹²C(α, γ)¹⁶O Rate

Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the ¹²C(α, γ)¹⁶O Rate