Still Brighter than Pre-Explosion, SN 2012Z Did Not Disappear: Comparing Hubble Space Telescope Observations a Decade Apart

McCully, Curtis; Jha, Saurabh W.; Scalzo, Richard A.; Howell, D. Andrew; Foley, Ryan J.; Zeng, Yaotian; Liu, Zheng-Wei; Hosseinzadeh, Griffin; Bildsten, Lars; Riess, Adam G.; Kirshner, Robert P.; Marion, G. H.; Camacho-Neves, Yssavo

doi:10.48550/arxiv.2106.04602

Cited by 7 publications

(9 citation statements)

References 72 publications

(143 reference statements)

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“…Kromer et al 2015;Yamanaka et al 2015;Magee et al 2016), at least a fraction of them occur inside a helium-rich CSM (Magee et al 2019;Jacobson-Galán et al 2019), while none has been observed in an elliptical galaxy host (Foley et al 2013). Lastly, at least one nearby SN Iax, SN 2012Z, has been securely associated with a luminous blue progenitor (McCully et al 2014;Stritzinger et al 2015;Yamanaka et al 2015;McCully et al 2021), with properties similar to those inferred for our ONe models prior to collapse (Section 3).…”

Section: Shell Burning and Envelope Ejection Prior To Collapse Near-supporting

confidence: 76%

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Chanlaridis¹,

Antoniadis²,

Aguilera-Dena³

et al. 2022

Preprint

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Context. When stripped from their hydrogen-rich envelopes, stars with initial masses between ∼7 and 11 M develop massive degenerate cores and collapse. Depending on the final structure and composition, the outcome can range from a thermonuclear explosion, to the formation of a neutron star in an electron-capture supernova (ECSN). It has been recently demonstrated that stars in this mass range may be more prone to disruption than previously thought: they may initiate explosive oxygen burning when their central densities are still below ρ c 10 9.6 g cm −3 . At the same time, their envelopes expand significantly, leading to the complete depletion of helium. This combination makes them interesting candidates for Type Ia Supernovae-which we call (C)ONe SNe Ia-and might have broader implications for the formation of neutron stars via ECSNe. Aims. To constrain the observational counterparts of (C)ONe SNe Ia and the key properties that enable them, it is crucial to constrain the evolution, composition, and pre-collapse structure of their progenitors, as well as the evolution of these quantities with cosmic time. In turn, this requires a detailed investigation of the final evolutionary stages preceding the collapse, and their sensitivity to input physics.Methods. Here, we model the evolution of 252 single, non-rotating helium-stars covering the initial mass range 0.8-3.5 M , metallicities between Z = 10 −4 and 0.02, and overshoot efficiency factors from f OV = 0.0 to 0.016 across all convective boundaries. We use these models to constrain several properties of these stars, including their central densities, compositions and envelope masses at the time of explosive oxygen ignition, and the final outcome as a function of initial helium-star mass. We further investigate the sensitivity of these properties to mass-loss rate assumptions using an additional grid of 110 models with varying wind efficiencies. Results. We find that helium-star models with masses between ∼1.8 and 2.7 M are able to evolve onto 1.35-1.37 M (C)ONe cores that initiate explosive burning at central densities between log 10 (ρ c /g cm −3 ) ∼ 9.3 and 9.6. We constrain the amount of residual carbon retained after core carbon burning as a function of initial conditions, and conclude that it plays a critical role in determining the final outcome: Chandrasekhar-mass cores with residual carbon mass fractions of X min ( 12 C) 0.004 result in (C)ONe SNe Ia, while those with lower carbon mass fractions become ECSNe. We find that (C)ONe SNe Ia are more likely to occur at high metallicities, whereas at low metallicities ECSNe dominate. We constrain the relative ratio between (C)ONe SNe Ia and SNe Ib/c to be 0.17-0.30 at Z = 0.02, and 0.03-0.13 at Z ≤ 10 −3 . Conclusions. We conclude with a discussion on potential observational properties of (C)ONe SNe Ia and their progenitors. In the few thousand years leading to the explosion, at least some progenitors should be identifiable as luminous metal-rich supergiants, embedded in hydrogen-free circumstellar nebulae.

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Section: Shell Burning and Envelope Ejection Prior To Collapse Near-supporting

confidence: 76%

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Chanlaridis¹,

Antoniadis²,

Aguilera-Dena³

et al. 2022

Preprint

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“…These winds can be the dominant source of luminosity at late times (≈ 1 year post explosion) lasting for at least a decade. Recent Hubble Space Telescope (HST) observations of SN 2012Z revealed an excess in its late-time luminosity that could be a result of remnant-driven winds (McCully et al 2021). Late time HST observations of SN 2021fcg will be valuable in probing the nature of its bound remnant.…”

Section: What Is the Progenitor Of Sn 2021fcg?mentioning

confidence: 99%

Faintest of them all : ZTF 21aaoryiz/SN 2021fcg -- Discovery of an extremely low luminosity type Iax supernova

Karambelkar,

Kasliwal,

Maguire

et al. 2021

Preprint

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We present the discovery of ZTF 21aaoryiz/SN 2021fcg -an extremely low-luminosity Type Iax supernova. SN 2021fcg was discovered by the Zwicky Transient Facility in the star-forming galaxy IC0512 at a distance of ≈ 27 Mpc. It reached a peak absolute magnitude of M r = −12.66 ± 0.20 mag, making it the least luminous thermonuclear supernova discovered to date. The E(B-V) contribution from the underlying host galaxy is unconstrained. However, even if it were as large as 0.5 mag, the peak absolute magnitude would be M r = −13.78 ± 0.20 mag -still consistent with being the lowest luminosity SN. Optical spectra of SN 2021fcg taken at 37 and 65 days post maximum show strong [Ca II], Ca II and Na I D emission and several weak [Fe II] emission lines. The [Ca II] emission in the two spectra has extremely low velocities of ≈ 1300 and 1000 km s −1 respectively. The spectra very closely resemble those of the very low luminosity Type Iax supernovae SN 2008ha, SN 2010ae and SN 2019gsc taken at similar phases. The peak bolometric luminosity of SN 2021fcg is ≈ 2.5 +1.5 −0.3 × 10 40 erg s −1 which is a factor of three lower than that for SN 2008ha. The bolometric lightcurve of SN 2021fcg is consistent with a very low ejected nickel mass (M Ni ≈ 0.8 +0.4 −0.5 × 10 −3 M ). The low luminosity and nickel mass of SN 2021fcg pose a challenge to the picture that low luminosity SNe Iax originate from deflagrations of near M ch hybrid carbon-oxygen-neon white dwarfs. Instead, the merger of a carbon-oxygen and oxygen-neon white dwarf is a promising model to explain SN 2021fcg.

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“…SN 2012Z-S1) has been interpreted as a He-star companion to the exploding WD (McCully et al 2014;Liu et al 2015). Interestingly, late-time observations taken about 1400 days after the explosion by the Hubble Space Telescope have shown that SN 2012Z is brighter than the normal SN 2011fe by a factor of two at this epoch (McCully et al 2021). This excess flux is suggested to be a composite of several sources: the shock-heated companion, a bound remnant that could drive a wind, and light from the SN ejecta due to radioactive decay (McCully et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Signatures of a surviving helium-star companion in Type Ia supernovae and constraints on the progenitor companion of SN 2011fe

Liu,

Roepke,

Zeng

2022

Preprint

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Single-degenerate (SD) binary systems composed of a white dwarf and a non-degenerate helium (He)-star companion have been proposed as the potential progenitors of Type Ia supernovae (SNe Ia). The He-star companions are expected to survive the SN Ia explosion in this SD progenitor model. In the present work, we map the surviving He-star companion models computed from our previous three-dimensional hydrodynamical simulations of ejecta-companion interaction into the onedimensional stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA) to follow their long-term evolution to make predictions on their post-impact observational properties, which can be helpful for searches of such surviving He-star companions in future observations. By comparing with the very late-epoch light curve of the best observed SN Ia, SN 2011fe, we find that our surviving He-star companions become significantly more luminous than SN 2011fe about 1000 d after the maximum light. This suggests that a He star is very unlikely to be a companion to the progenitor of SN 2011fe.

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Still Brighter than Pre-Explosion, SN 2012Z Did Not Disappear: Comparing Hubble Space Telescope Observations a Decade Apart

Cited by 7 publications

References 72 publications

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Faintest of them all : ZTF 21aaoryiz/SN 2021fcg -- Discovery of an extremely low luminosity type Iax supernova

Signatures of a surviving helium-star companion in Type Ia supernovae and constraints on the progenitor companion of SN 2011fe

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