Supernova 2014J at M82 – II. Direct analysis of a middle-class Type Ia supernova

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

doi:10.1093/mnras/stw1088

Cited by 6 publications

(5 citation statements)

References 58 publications

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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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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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“…Additionally, observational evidence for such progenitor systems has proven to be elusive. The nearby SNe Ia 2011fe and 2014J were particularly well-studied (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;Shappee et al 2017;Yang et al 2018), but no compelling evidence was found for the existence of non-degenerate companions Chomiuk et al 2012;Shappee et al 2013;Margutti et al 2014;Lundqvist et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Signatures of bimodality in nebular phase Type Ia supernova spectra

Vallely

Tucker

Shappee

et al. 2020

Monthly Notices of the Royal Astronomical Society

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One observational prediction for Type Ia supernova (SNe Ia) explosions produced through white dwarf-white dwarf collisions is the presence of bimodal velocity distributions for the 56 Ni decay products, although this signature can also be produced by an off-center ignition in a delayed detonation explosion. These bimodal velocity distributions can manifest as double-peaked or flat-topped spectral features in latetime spectroscopic observations for favorable viewing angles. We present nebular-phase spectroscopic observations of 17 SNe Ia obtained with the Large Binocular Telescope (LBT). Combining these observations with an extensive search of publicly available archival data, we collect a total sample of 48 SNe Ia and classify them based on whether they show compelling evidence for bimodal velocity profiles in three features associated with 56 Ni decay products: the [Fe II] and [Fe III] feature at ∼ 5300 Å, the [Co III] λ5891 feature, and the [Co III] and [Fe II] feature at ∼ 6600 Å. We identify 9 bimodal SNe in our sample, and we find that these SNe have average peak M V about 0.3 mag fainter than those which do not. This is consistent with theoretical predictions for explosions created by nearly head-on collisions of white dwarfs due to viewing angle effects and 56 Ni yields.

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“…SN 2014J in M82 is one of the nearest SN Ia in decades and has been extensively studied (e.g. Kelly et al 2014;Diehl et al 2014;Foley et al 2014;Ashall et al 2014;Vacca et al 2015;Galbany et al 2016;Vallely et al 2016). It is heavily reddened by host galaxy dust, but shows spectral features of a normal SN Ia (Amanullah et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Nebular spectroscopy of SN 2014J: Detection of stable nickel in near-infrared spectra

Dhawan

Flörs

Leibundgut

et al. 2018

A&A

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We present near infrared (NIR) spectroscopy of the nearby supernova 2014J obtained ∼450 d after explosion. We detect the [Ni II] 1.939 µm line in the spectra indicating the presence of stable 58 Ni in the ejecta. The stable nickel is not centrally concentrated but rather distributed as the iron. The spectra are dominated by forbidden [Fe II] and [Co II] lines. We use lines, in the NIR spectra, arising from the same upper energy levels to place constraints on the extinction from host galaxy dust. We find that that our data are in agreement with the high A V and low R V found in earlier studies from data near maximum light. Using a 56 Ni mass prior from near maximum light γ-ray observations, we find ∼0.05 M of stable nickel to be present in the ejecta. We find that the iron group features are redshifted from the host galaxy rest frame by ∼600 km s −1 .

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Supernova 2014J at M82 – II. Direct analysis of a middle-class Type Ia supernova

Cited by 6 publications

References 58 publications

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

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

Signatures of bimodality in nebular phase Type Ia supernova spectra

Nebular spectroscopy of SN 2014J: Detection of stable nickel in near-infrared spectra

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