Nebular Hα Limits for Fast Declining SNe Ia

Sand, David J.; Amaro, R.; Moe, Maxwell; Graham, M. L.; Andrews, Jennifer E.; Burke, J.; Cartier, R.; Eweis, Y.; Galbany, L.; Hiramatsu, D.; Howell, D. A.; Jha, Saurabh W.; Lundquist, M.; Matheson, T.; McCully, C.; Milne, Peter; Smith, Nathan; Valenti, S.; Wyatt, S.

doi:10.3847/2041-8213/ab1eaf

Cited by 28 publications

(23 citation statements)

References 83 publications

(112 reference statements)

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“…We find no such emission in any spectrum in our sample, and place new or updated stripped/ablated mass constraints for each SN Ia. The entirety of similar work in the literature totals 33 SNe Ia (Mattila et al 2005;Leonard 2007;Shappee et al 2013a;Lundqvist et al 2013Lundqvist et al , 2015Maguire et al 2016;Graham et al 2017;Shappee et al 2018;Sand et al 2018a;Holmbo et al 2018;Dimitriadis et al 2019a;Tucker et al 2018;Sand et al 2019), a fraction of the sample analyzed in this work. All SNe Ia included in this study are listed in Table B2 and photometric parameters (t max , ∆m 15 , µ, E(B − V) host ) are provided in Table B3.…”

Section: ; Livio and Mazzali 2018;supporting

confidence: 60%

Nebular spectra of 111 Type Ia supernovae disfavour single-degenerate progenitors

Tucker

Shappee

Vallely

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We place statistical constraints on Type Ia supernova (SN Ia) progenitors using 227 nebular phase spectra of 111 SNe Ia. We find no evidence of stripped companion emission in any of the nebular phase spectra. Upper limits are placed on the amount of mass that could go undetected in each spectrum using recent hydrodynamic simulations. With these null detections, we place an observational 3σ upper limit on the fraction of SNe Ia that are produced through the classical H-rich non-degenerate companion scenario of < 5.5%. Additionally, we set a tentative 3σ upper limit on He star progenitor scenarios of < 6.4%, although further theoretical modelling is required. These limits refer to our most representative sample including normal, 91bg-like, 91Tlike, and "Super Chandrasekhar" SNe Ia but excluding SNe Iax and SNe Ia-CSM. As part of our analysis, we also derive a Nebular Phase Phillips Relation, which approximates the brightness of a SN Ia from 150 − 500 days after maximum using the peak magnitude and decline rate parameter ∆m 15 (B).

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Section: ; Livio and Mazzali 2018;supporting

confidence: 60%

Nebular spectra of 111 Type Ia supernovae disfavour single-degenerate progenitors

Tucker

Shappee

Vallely

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Material from a hydrogen-or helium-rich companion star has been predicted to be stripped (or ablated) during the explosion and result in the presence of low-velocity hydrogen-or helium-rich material in the SN ejecta where it can be energized by the radioactive decay and become visible. Searches for this material have been made in many nearby SN Ia using late-time spectra, without detection 29,[75][76][77][78][79][80][81][82][83][84] . This suggests that either the material is present and is not visible because it is not located cospatially with the radioactive material or that these objects do not have hydrogen-or helium-rich companions.…”

Section: Type Ia Supernovaementioning

confidence: 99%

Observational properties of thermonuclear supernovae

2019

Self Cite

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The explosive death of a star as a supernova is one of the most dramatic events in the Universe. Supernovae have an outsized impact on many areas of astrophysics: they are major contributors to the chemical enrichment of the cosmos and significantly influence the formation of subsequent generations of stars and the evolution of galaxies. Here we review the observational properties of thermonuclear supernovae, exploding white dwarf stars resulting from the stellar evolution of low-mass stars in close binary systems. The best known objects in this class are type Ia supernovae (SN Ia), astrophysically important in their application as standardisable candles to measure cosmological distances and the primary source of iron group elements in the Universe. Surprisingly, given their prominent role, SN Ia progenitor systems and explosion mechanisms are not fully understood; the observations we describe here provide constraints on models, not always in consistent ways. Recent advances in supernova discovery and follow-up have shown that the class of thermonuclear supernovae includes more than just SN Ia, and we characterise that diversity in this review.The modern classification scheme for supernovae traces back to Minkowski 1 who in 1941 split "Type I" from "Type II" supernovae based on optical spectra. Further subdivision of these basic classes has continued on an empirical basis 2, 3 , and in our review we describe the observational properties of what are now called SN Ia, along with other similar objects. The observational classification effort arises from a desire for physical understanding of these objects, explaining our use of the term thermonuclear supernovae in the title. That categorisation is based on the explosion mechanism: objects where the energy released in the explosion is primarily the result of thermonuclear fusion. Given our current state of knowledge, we could equally well call this a review of the observational properties of white dwarf supernovae, a categorisation based on the kind of object that explodes. This is contrasted with core-collapse or massive star supernovae, respectively, in the explosion mechanism or exploding object categorisations. Unlike those objects, where clear observational evidence exists for massive star progenitors and corecollapse (from both neutrino emission and remnant pulsars), the direct evidence for thermonuclear supernova explosions of white dwarfs is limited 4, 5 and not necessarily simply interpretable 6, 7 . Nevertheless, the indirect evidence is strong, though many open questions about the progenitor systems and explosion mechanisms remain.SN Ia are important both to the evolution of the Universe and to our understanding of it. As standardisable candles whose distance can be observationally inferred 8 , SN Ia have a starring role in the discovery of the accelerating expansion of the Universe 9, 10 and in measurement of its current expansion rate 11 . SN Ia are also major contributors to the chemical enrichment of the Universe, producing most of its iron 12 and elem...

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“…This is much less than predicted by all hydrodynamical simulations of this scenario, which suggest that at least 0.1 M of material should be stripped (see original work by Marietta et al 2000 and the most recent complete study by Liu et al 2012). Another tension for the single-degenerate scenario is that such Hα emission is very rarely seen (stringent upper limits on M st are placed instead), even for the most nearby SN Ia events or those with very high quality observations (Leonard 2007;Lundqvist et al 2013Lundqvist et al , 2015Shappee et al 2013Shappee et al , 2018Maguire et al 2016;Graham et al 2017;Sand et al 2018Sand et al , 2019Holmbo et al 2019;Dimitriadis et al 2019;Tucker et al 2019Tucker et al , 2020, while theory predicts that it should instead be systematically detected. In the current framework, this is a major problem for the single-degenerate scenario for SNe Ia.…”

Section: Introductionmentioning

confidence: 97%

Spectral signatures of H-rich material stripped from a non-degenerate companion by a Type Ia supernova

Dessart

Leonard

Prieto

2020

A&A

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The single-degenerate scenario for Type Ia supernovae should yield metal-rich ejecta that enclose some stripped material from the non-degenerate H-rich companion star. We present a large grid of non-local thermodynamic equilibrium steady-state radiative transfer calculations for such hybrid ejecta and provide analytical fits for the Hα luminosity and equivalent width. Our set of models covers a range of masses for 56Ni and the ejecta, for the stripped material (Mst), and post-explosion epochs from 100 to 300 d. The brightness contrast between stripped material and metal-rich ejecta challenges the detection of H I and He I lines prior to ~100 d. Intrinsic and extrinsic optical depth effects also influence the radiation emanating from the stripped material. This inner denser region is marginally thick in the continuum and optically thick in all Balmer lines. The overlying metal-rich ejecta blanket the inner regions, completely below about 5000 Å, and more sparsely at longer wavelengths. As a consequence, Hβ should not be observed for all values of Mst up to at least 300 days, while Hα should be observed after ~100 d for all Mst ≥ 0.01 M⊙. Observational non-detections capable of limiting the Hα equivalent width to <1 Å set a formal upper limit of Mst < 0.001M⊙. This contrasts with the case of circumstellar-material (CSM) interaction, not subject to external blanketing, which should produce Hα and Hβ lines with a strength dependent primarily on CSM density. We confirm previous analyses that suggest low values of order 0.001 M⊙ for Mst to explain the observations of the two Type Ia supernovae with nebular-phase Hα detection, in conflict with the much greater stripped mass predicted by hydrodynamical simulations for the single-degenerate scenario. A more likely solution is the double-degenerate scenario, together with CSM interaction, or enclosed material from a tertiary star in a triple system or from a giant planet.

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Nebular Hα Limits for Fast Declining SNe Ia

Cited by 28 publications

References 83 publications

Nebular spectra of 111 Type Ia supernovae disfavour single-degenerate progenitors

Nebular spectra of 111 Type Ia supernovae disfavour single-degenerate progenitors

Observational properties of thermonuclear supernovae

Spectral signatures of H-rich material stripped from a non-degenerate companion by a Type Ia supernova

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