The Extremes of Thermonuclear Supernovae

Taubenberger, S.

doi:10.1007/978-3-319-20794-0_37-1

Cited by 30 publications

(45 citation statements)

References 180 publications

(509 reference statements)

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“…Since we do not have a ∆m15(B) measurement for SN 2016brx, but it is a confirmed SN91bg-like SN Ia, we have placed a range of 1.7<∆m15(B)<2 on this object, corresponding to the observed range for this subtype (see e.g. Figure 1 of Taubenberger 2017). Also shown is the Hα detection in ASASSN-18tb (Kollmeier et al 2019, blue star), which is significantly stronger than the Hα luminosity limits presented here.…”

Section: Discussionmentioning

confidence: 99%

Nebular Hα Limits for Fast Declining SNe Ia

Sand

Amaro

Moe

et al. 2019

ApJL

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One clear observational prediction of the single degenerate progenitor scenario as the origin of type Ia supernovae (SNe) is the presence of relatively narrow (≈1000 km s −1 ) Hα emission at nebular phases, although this feature is rarely seen. We present a compilation of nebular phase Hα limits for SN Ia in the literature and demonstrate that this heterogenous sample has been biased towards SN Ia with relatively high luminosities and slow decline rates, as parameterized by ∆m 15 (B), the difference in B-band magnitude between maximum light and fifteen days afterward. Motivated by the need to explore the full parameter space of SN Ia and their subtypes, we present two new and six previously published nebular spectra of SN Ia with ∆m 15 (B) > 1.3 mag (including members of the transitional and SN1991bg-like subclasses) and measure nondetection limits of L Hα < 0.85-9.9×10 36 ergs s −1 , which we confirmed by implanting simulated Hα emission into our data. Based on the lastest models of swept-up material stripped from a nondegenerate companion star, these L Hα values correspond to hydrogen mass limits of M H 1-3×10 −4 M ⊙ , roughly three orders of magnitude below that expected for the systems modeled, although we note that no simulations of Hα nebular emission in such weak explosions have yet been performed. Despite the recent detection of strong Hα in ASASSN-18tb (SN 2018fhw; ∆m 15 (B) = 2.0 mag), we see no evidence that fast declining systems are more likely to have late time Hα emission, although a larger sample is needed to confirm this result.

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Section: Discussionmentioning

confidence: 99%

Nebular Hα Limits for Fast Declining SNe Ia

Sand

Amaro

Moe

et al. 2019

ApJL

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“…For example, the overluminous 91T-like events (Filippenko et al 1992a) and 99aa-like events ) have distinct Fe III lines dominating their early spectra; while the subluminous 91bg-like events (Filippenko et al 1992b) and 86G-like events (Phillips et al 1987) display pronounced Si II and Ti II lines. Recent reviews of the observational characteristics and physical interpretation of different subtypes can be found in the literature (e.g., Parrent et al 2014;Maeda & Terada 2016;Taubenberger 2017). Within our sample, 95 objects have 1 spectrum; 22 have two spectra, 5 have 3 spectra, 1 has 4 spectra, 2 have 5 spectra, and 1 has 10 spectra.…”

Section: Subtype Classificationmentioning

confidence: 99%

ZTF Early Observations of Type Ia Supernovae. I. Properties of the 2018 Sample

Yao

Miller

Kulkarni

et al. 2019

ApJ

103

158

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Early-time observations of Type Ia supernovae (SNe Ia) are essential to constrain their progenitor properties. In this paper, we present high-quality light curves of 127 SNe Ia discovered by the Zwicky Transient Facility (ZTF) in 2018. We describe our method to perform forced point spread function (PSF) photometry, which can be applied to other types of extragalactic transients. With a planned cadence of six observations per night (3g + 3r), all of the 127 SNe Ia are detected in both g and r band more than 10 d (in the rest frame) prior to the epoch of g-band maximum light. The redshifts of these objects range from z = 0.0181 to 0.165; the median redshift is 0.074. Among the 127 SNe, 50 are detected at least 14 d prior to maximum light (in the rest frame), with a subset of 9 objects being detected more than 17 d before g-band peak. This is the largest sample of young SNe Ia collected to date; it can be used to study the shape and color evolution of the rising light curves in unprecedented detail. We discuss six peculiar events in this sample, including one 02cx-like event ZTF18abclfee (SN 2018crl), one Ia-CSM SN ZTF18aaykjei (SN 2018cxk), and four objects with possible super-Chandrasekhar mass

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“…Off the Phillips relation is the realm of "peculiar" thermonuclear supernovae. The same luminosity/decline-rate parameter space has been used to distinguish these objects 135 (Figure 7). Several groups of white dwarf supernovae show low ejecta velocities, below the typical 10,000 km s −1 Si II velocity seen in normal SN Ia around maximum light.…”

Section: The Thermonuclear Supernova Zoomentioning

confidence: 99%

Observational properties of thermonuclear supernovae

2019

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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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The Extremes of Thermonuclear Supernovae

Cited by 30 publications

References 180 publications

Nebular Hα Limits for Fast Declining SNe Ia

Nebular Hα Limits for Fast Declining SNe Ia

ZTF Early Observations of Type Ia Supernovae. I. Properties of the 2018 Sample

Observational properties of thermonuclear supernovae

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