SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

Galbany, L.; Moreno-Raya, M. E.; Ruiz‐Lapuente, P.; Hernández, J. I. González; Méndez, J.; Vallely, P.; Baron, E.; Domı́nguez, I.; Hamuy, M.; López-Sánchez, Á. R.; Mollá, M.; Catalán, S.; Cooke, Elizabeth A.; Fariña, C.; Génova-Santos, R. T.; Karjalainen, R.; Lietzen, H.; McCormac, J.; Riddick, F.; Rubiño-Martín, J. A.; Skillen, I.; Tudor, Vlad; Văduvescu, O.

doi:10.1093/mnras/stw026

Cited by 16 publications

(15 citation statements)

References 70 publications

(91 reference statements)

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“…Although SN 2014J was discovered relatively late considering the proximity of its host galaxy, M82, pre-discovery images from surveys do exist and data of the early-time rise of the SN have been analyzed by Zheng et al (2014) and Goobar et al (2014Goobar et al ( , 2015. Because of its closeness at under 4 Mpc (Dalcanton et al 2009), the post-discovery light curve and spectral evolution of this SN have been well-observed in many different wavelength regions (see Ashall et al 2014;Foley et al 2014;Margutti et al 2014;Pérez-Torres et al 2014;Jack et al 2015;Marion et al 2015;Siverd et al 2015;Telesco et al 2015;Galbany et al 2016;Sand et al 2016;Srivastav et al 2016, and many others).…”

Section: Sn 2014j and Observational Evidence For The Progenitor Systemmentioning

confidence: 99%

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Near-infrared Spectral Evolution of the Type Ia Supernova 2014J in the Nebular Phase: Implications for the Progenitor System

Diamond

Hoêflich

Hsiao

et al. 2018

ApJ

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As the closest Type Ia supernova in decades, SN 2014J provides a unique opportunity for detailed investigation into observational signatures of the progenitor system, explosion mechanism, and burning product distribution. We present a late-time near-infrared spectral series from Gemini-N at 307 − 466 days after the explosion. Following the H-band evolution probes the distribution of radioactive iron group elements, the extent of mixing, and presence of magnetic fields in the expanding ejecta. Comparing the isolated 1.6440 µm [Fe II] emission line with synthetic models shows consistency with a Chandrasekhar-mass white dwarf of ρ c = 0.7 × 10 9 g cm −3 undergoing a delayed detonation. The ratio of the flux in the neighboring 1.54 µm emission feature to the flux in the 1.6440 µm feature shows evidence of some limited mixing of stable and radioactive iron group elements in the central regions. Additionally, the evolution of the 1.6440 µm line shows an intriguing asymmetry. When measuring line-width of this feature, the data show an increase in line width not seen in the evolution of the synthetic spectra, corresponding to ≈ 1,000 km s −1 , which could be caused by a localized transition to detonation producing asymmetric ionization in the ejecta. Using the difference in width between the different epochs, an asymmetric component in the central regions, corresponding to approximately the inner 2 × 10 −4 of white dwarf mass suggests an off-center ignition of the initial explosion and hence of the kinematic center from the chemical center. Several additional models investigated, including a He detonation and a merger, have difficulty reproducing the features seen these spectra.

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Section: Sn 2014j and Observational Evidence For The Progenitor Systemmentioning

confidence: 99%

“…Overall, SN 2014J has been shown to be a fairly standard SN Ia (Galbany et al 2016), which makes it ideal for probing deeper into the underlying physics of the progenitor scenarios and explosions. There are a variety of light curve parameters for SN 2014J depending on the source article.…”

Section: Sn 2014j and Observational Evidence For The Progenitor Systemmentioning

confidence: 99%

Near-infrared Spectral Evolution of the Type Ia Supernova 2014J in the Nebular Phase: Implications for the Progenitor System

Diamond

Hoêflich

Hsiao

et al. 2018

ApJ

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“…When calculating modelled E(B − V ) curves above, SN templates were stretched so that the observed decline rate after interaction with dust matches that inferred for SN 2014J. In particular, following Galbany et al (2016) we averaged four different estimates in the literature (Tsvetkov et al 2014;Ashall et al 2014;Kawabata et al 2014;Marion et al 2015) and use ∆M 14J…”

Section: Sn 2014jmentioning

confidence: 99%

Estimating dust distances to Type Ia supernovae from colour excess time evolution

Bulla

Goobar

Amanullah

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present a new technique to infer dust locations towards reddened Type Ia supernovae and to help discriminate between an interstellar and a circumstellar origin for the observed extinction. Using Monte Carlo simulations, we show that the time-evolution of the light-curve shape and especially of the colour excess E(B − V ) places strong constraints on the distance between dust and the supernova. We apply our approach to two highly-reddened Type Ia supernovae for which dust distance estimates are available in the literature: SN 2006X and SN 2014J. For the former, we obtain a timevariable E(B − V ) and from this derive a distance of 27.5 +9.0 −4.9 or 22.1 +6.0 −3.8 pc depending on whether dust properties typical of the Large Magellanic Cloud (LMC) or the Milky Way (MW) are used. For the latter, instead, we obtain a constant E(B − V ) consistent with dust at distances larger than ∼ 50 and 38 pc for LMC− and MW−type dust, respectively. Values thus extracted are in excellent agreement with previous estimates for the two supernovae. Our findings suggest that dust responsible for the extinction towards these supernovae is likely to be located within interstellar clouds. We also discuss how other properties of reddened Type Ia supernovae -such as their peculiar extinction and polarization behaviour and the detection of variable, blue-shifted sodium features in some of these events -might be compatible with dust and gas at interstellar-scale distances.

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“…No such signatures were detected for SNe 1998bu and 2000cx (Lundqvist et al 2013), SN 2001el (Mattila et al 2005, SNe 2005am and 2005cf (Leonard 2007), SN 2012cg , SN 2013gy (Holmbo et al 2018), or SN 2017cbv (Sand et al 2018, nor were they detected by Graham et al (2017) in 8 other SNe Ia. The nearby SNe Ia 2011fe and 2014J were particularly well-studied events (Brown et al 2012;Munari et al 2013;Mazzali et al 2014;Foley et al 2014;Goobar et al 2014;Galbany et al 2016;Vallely et al 2016;Dhawan et al 2018), but they too showed no hydrogen emission in their late-time spectra Lundqvist et al 2015;Sand et al 2016).…”

Section: Introductionmentioning

confidence: 97%

ASASSN-18tb: a most unusual Type Ia supernova observed by TESS and SALT

Vallely

Fausnaugh

Jha

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present photometric and spectroscopic observations of the unusual Type Ia supernova ASASSN-18tb, including a series of SALT spectra obtained over the course of nearly six months and the first observations of a supernova by the Transiting Exoplanet Survey Satellite (TESS). We confirm a previous observation by Kollmeier et al. (2019) showing that ASASSN-18tb is the first relatively normal Type Ia supernova to exhibit clear broad (∼ 1000 km s −1 ) Hα emission in its nebular phase spectra. We find that this event is best explained as a sub-Chandrasekhar mass explosion producing M N i ≈ 0.3 M . Despite the strong Hα signature at late times, we find that the early rise of the supernova shows no evidence for deviations from a single-component power-law and is best fit with a moderately shallow power-law of index 1.69 ± 0.04. We find that the Hα luminosity remains approximately constant after its initial detection at phase +37 d, and that the Hα velocity evolution does not trace that of the Fe III λ4660 emission. These suggest that the Hα emission arises from a circumstellar medium (CSM) rather than swept up material from a non-degenerate companion. However, ASASSN-18tb is strikingly different from other known CSM-interacting Type Ia supernovae in a number of significant ways. Those objects typically show an Hα luminosity two orders of magnitude higher than what is seen in ASASSN-18tb, pushing them away from the empirical light curve relations that define "normal" Type Ia supernovae. Conversely, ASASSN-18tb exhibits a fairly typical light curve and luminosity for an underluminous or transitional SN Ia, with M R ≈ −18.1 mag. Moreover, ASASSN-18tb is the only SN Ia showing Hα from CSM interaction to be discovered in an early-type galaxy.

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SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

Cited by 16 publications

References 70 publications

Near-infrared Spectral Evolution of the Type Ia Supernova 2014J in the Nebular Phase: Implications for the Progenitor System

Near-infrared Spectral Evolution of the Type Ia Supernova 2014J in the Nebular Phase: Implications for the Progenitor System

Estimating dust distances to Type Ia supernovae from colour excess time evolution

ASASSN-18tb: a most unusual Type Ia supernova observed by TESS and SALT

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