SN1991bg-like supernovae are associated with old stellar populations

Panther, F. H.; Seitenzahl, Ivo R.; Ruiter, Ashley J.; Crocker, Roland M.; Lidman, C.; Wang, Ella; Tucker, B.; Groves, Brent

doi:10.1017/pasa.2019.24

Cited by 23 publications

(15 citation statements)

References 55 publications

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“…In fact, both SNe 2018cqj and 2016jae appeared in the outskirts of their putative host galaxies, suggesting either that they are halo objects, whereas the host of SN 2018fhw was a dwarf elliptical. This is consistent with the progenitor environment of the majority of the 91bg-like and transitional SNe (see, e.g., Panther et al 2019), rather than with that of Type Ia-CSM SNe, which are found in star-forming galaxies (see, e.g., Hamuy et al 2003;Prieto et al 2007;Dilday et al 2012;Silverman et al 2013).…”

Section: Discussion and Summary On The Nature Of Sn 2016jae And Its P...supporting

confidence: 81%

Nebular Hα emission in Type Ia supernova 2016jae

Elias‐Rosa

Chen

Benetti

et al. 2021

A&A

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There is a wide consensus that Type Ia supernovae (SNe Ia) originate from the thermonuclear explosion of CO white dwarfs (WDs), with the lack of hydrogen in the observed spectra as a distinctive feature. Here, we present supernova (SN) 2016jae, which was classified as an SN Ia from a spectrum obtained soon after its discovery. The SN reached a B-band peak of −17.93 ± 0.34 mag, followed by a fast luminosity decline with sBV0.56 ± 0.06 and inferred Δm15(B) of 1.88 ± 0.10 mag. Overall, the SN appears to be a ‘transitional’ event between a ‘normal’ SN Ia and a very dim SN Ia, such as 91bg-like SNe. Its peculiarity is that two late-time spectra, taken at +84 and +142 days after the peak, show a narrow line of Hα (with full width at half maximum of ∼650 and 1000 km s−1, respectively). This is the third low-luminosity and fast-declining SN Ia, after SN2018cqj/ATLAS18qtd and SN2018fhw/ASASSN-18tb, found in the 100IAS survey to show a resolved narrow Hα line in emission in its nebular-phase spectra. We argue that the nebular Hα emission originates in an expanding hydrogen-rich shell (with velocity ≤1000 km s−1). The hydrogen shell velocity is too high to be produced during a common envelope phase, though it may be consistent with some material stripped from an H-rich companion star in a single-degenerate progenitor system. However, the derived mass of this stripped hydrogen is ∼0.002–0.003 M⊙, which is much less than that expected (> 0.1 M⊙) from standard models for these scenarios. Another plausible sequence of events is a weak SN ejecta interaction with an H shell ejected by optically thick winds or a nova-like eruption on the CO WD progenitor some years before the SN explosion.

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Section: Discussion and Summary On The Nature Of Sn 2016jae And Its P...supporting

confidence: 81%

Nebular Hα emission in Type Ia supernova 2016jae

Elias‐Rosa

Chen

Benetti

et al. 2021

A&A

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“…Some simulations involving higher mass CO WD cores have been carried out (e.g. Pakmor et al 2021), which yield interesting synthetic observables that may be of interest in the era of large-scale surveys by the likes of the Vera C. Rubin Observatory.…”

Section: Discussionmentioning

confidence: 99%

“…converting the helium to carbon, thereby removing helium), there are certain regions of parameter space during stable Roche lobe overflow where helium will be accumulated on the CO WD and will not burn (Piersanti, Tornambé & Yungelson 2014). Is is also plausible that a somewhat low-mass CO white dwarf with a rather thick helium surface layer could be realized through a merging event (Crocker et al 2017), though detailed studies of such a situation remain largely unexplored, particularly in 3D (but see Pakmor et al 2021).…”

Section: P Ro S P E C T S F O R D E T E C Ta B I L I T Ymentioning

confidence: 99%

Prospects of direct detection of 48V gamma-rays from thermonuclear supernovae

Panther

Seitenzahl

Ruiter

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Detection of gamma-rays emitted by radioactive isotopes synthesized in stellar explosions can give important insights into the processes that power transients such as supernovae, as well as providing a detailed census of the abundance of different isotope species relevant to the chemical evolution of the Universe. Observations of nearby supernovae have yielded observational proof that 57Co powered the late-time evolution of SN1987A’s lightcurve, and conclusive evidence that 56Ni and its daughter nuclei power the light curves of Type Ia supernovae. In this paper we describe the prospects for detecting nuclear decay lines associated with the decay of 48V, the daughter nucleus of 48Cr, which is expected to be synthesised in large quantities - MCr ∼ 1.9 × 10−2 M⊙ - in transients initiated by explosive helium burning (α-capture) of a thick helium shell. We calculate emergent gamma-ray line fluxes for a simulated explosion model of a thermonuclear explosion of carbon-oxygen white dwarf core of mass 0.45 M⊙ surrounded by a thick helium layer of mass 0.21 M⊙. We present observational limits on the presence of 48V in nearby SNe Ia 2014J using the INTEGRAL space telescope, excluding a 48Cr production on the surface of more than 0.1 M⊙. We find that the future gamma-ray mission AMEGO will have an approximately 5 per cent chance of observing 48V gamma-rays from such events during the currently-planned operational lifetime, based on our birthrate predictions of faint thermonuclear transients. We describe the conditions for a 3σ detection by the gamma-ray telescopes INTEGRAL/SPI, COSI and AMEGO.

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“…This results in an underestimate of supernova rates from systems with long-delay times (e.g. Panther et al 2019), as it does not take into account the total mass that formed into stars -most massive stars that formed in the past will have since exploded as supernovae. As the binary population synthesis calculation depends on knowing the total mass that formed into stars, our calculation underestimates the rate.…”

Section: Discussionmentioning

confidence: 99%

Prospects of direct detection of $^{48}$V gamma-rays from thermonuclear supernovae

Panther,

Seitenzahl,

Ruiter

et al. 2021

Preprint

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Detection of gamma-rays emitted by radioactive isotopes synthesized in stellar outbursts or explosions can give important insights into the processes that power transients such as supernovae, as well as providing a detailed census of the abundance of different isotope species relevant to the chemical evolution of the Universe. Observations of nearby supernovae have yielded observational proof that 57 Co drove the late-time evolution of SN1987A's lightcurve, and conclusive evidence that 56 Ni and its daughter nuclei power the light curves of Type Ia supernovae. In this paper we describe the prospects for detecting nuclear decay lines associated with the decay of 48 V, the daughter nucleus of 48 Cr, which is expected to be synthesised in large quantities in transients initiated by explosive helium burning ( -capture) of a thick helium shell. We investigate these prospects using results for the emergent gamma-ray line fluxes from a radiative transfer simulation performed for a simulated explosion model of a thermonuclear explosion of carbon-oxygen white dwarf core of mass 0.45 ⊙ surrounded by a thick helium layer of mass 0.21 ⊙ . We find that the future gamma-ray mission AMEGO will have an approximately 5 per cent chance of observing 48 V gamma-rays from such events during the currently-planned operational lifetime, based on our birthrate predictions of faint thermonuclear transients. We describe the conditions for a 3 detection by the gamma-ray instruments INTEGRAL/SPI, COSI and AMEGO.

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SN1991bg-like supernovae are associated with old stellar populations

Cited by 23 publications

References 55 publications

Nebular Hα emission in Type Ia supernova 2016jae

Nebular Hα emission in Type Ia supernova 2016jae

Prospects of direct detection of 48V gamma-rays from thermonuclear supernovae

Prospects of direct detection of $^{48}$V gamma-rays from thermonuclear supernovae

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