AN EXCESS OF MID-INFRARED EMISSION FROM THE TYPE Iax SN 2014dt

Fox, O.; Johansson, Joel; Kasliwal, M. M.; Andrews, Jennifer E.; Bally, John; Bond, Howard E.; Boyer, Martha L.; Gehrz, R. D.; Hélou, G.; Hsiao, E. Y.; Masci, Frank J.; Parthasarathy, M.; Smith, Nathan; Tinyanont, Samaporn; Dyk, Schuyler D. Van

doi:10.3847/2041-8205/816/1/l13

Cited by 42 publications

(55 citation statements)

References 41 publications

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“…The large optical depths of the relatively massive SN Iax bound envelopes result in very extended photospheres and low effective temperatures that cool to 1000−2000 K by ∼ 400 d. The IR detection of SN 2014dt at 300−400 d (Fox et al 2016) may be a common feature of SNe Iax and may be due to the low effective temperature of the photosphere, as opposed to, or in addition to, dust formation (Foley et al 2016).…”

Section: Post-sn Iax Windsmentioning

confidence: 99%

Wait for It: Post-Supernova Winds Driven by Delayed Radioactive Decays

Shen

Schwab

2017

ApJ

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In most astrophysical situations, the radioactive decay of 56 Ni to 56 Co occurs via electron capture with a fixed half-life of 6.1 days. However, this decay rate is significantly slowed when the nuclei are fully ionized because K-shell electrons are unavailable for capture. In this paper, we explore the effect of these delayed decays on white dwarfs (WDs) that may survive Type Ia and Type Iax supernovae (SNe Ia and SNe Iax). The energy released by the delayed radioactive decays of 56 Ni and 56 Co drives a persistent wind from the surviving WD's surface that contributes to the late-time appearance of these SNe after emission from the bulk of the SN ejecta has faded. We use the stellar evolution code MESA to calculate the hydrodynamical evolution and resulting light curves of these winds. Our post-SN Ia models conflict with late-time observations of SN 2011fe, but uncertainties in our initial conditions prevent us from ruling out the existence of surviving WD donors. Much better agreement with observations is achieved with our post-SN Iax bound remnant models, providing evidence that these explosions are due to deflagrations in accreting WDs that fail to completely unbind the WDs. Future radiative transfer calculations and wind models utilizing explosion simulations for more accurate initial conditions will extend our study of radioactively-powered winds from post-SN surviving WDs and enable their use as powerful discriminants among the various SN Ia and SN Iax progenitor scenarios.

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Section: Post-sn Iax Windsmentioning

confidence: 99%

Wait for It: Post-Supernova Winds Driven by Delayed Radioactive Decays

Shen

Schwab

2017

ApJ

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“…1) Before supernova explosion, the system experiences a common envelope wind phase. With the expansion and cooling of the CE material, dust may form around the progenitor system as observed in some normal and special SNe Ia (Lü et al 2013;Fox & Filippenko 2013;Silverman et al 2013;Johansson et al 2013;Fox et al 2016). The dust could redden the color of the candidate.…”

Section: The Surviving Companion In the Remnant Of Sn 1006mentioning

confidence: 99%

Subdwarf B stars as possible surviving companions in Type Ia supernova remnants

Meng

2018

Monthly Notices of the Royal Astronomical Society

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Although type Ia supernovae (SNe Ia) are so important in many astrophysical fields, a debate on their progenitor model is still endless. Searching the surviving companion in a supernova remnant (SNR) may distinguish different progenitor models, since a companion still exists in the remnant for the single-degenerate (SD) model, but does not for the double degenerate (DD) model. However, some recent surveys do not discover the surviving companions in the remnant of SN 1006 and Kepler's supernova, which seems to disfavor the SD model. Such a result could be derived from an incorrect survey target. Here, based on the common-envelope wind SD model for SNe Ia, in which the initial binary system consists of a white dwarf (WD) and a main-sequence (MS) star, we found that the companion at the moment of supernova explosion may be a MS, red-giant (RG) or subdwarf B (sdB) star if a spin-down timescale of less than 10 7 yr is assumed. We show the properties of the companions at the moment of supernova explosion, which are key clues to search the surviving companions in SNRs. Here, we suggest that the sdB star may be the surviving companion in some SNRs, even if the progenitor systems are the WD + MS systems. The SNe Ia with the sdB companions may contribute to all SNe Ia as much as 22%.

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“…The observations are performed in the 3.6 μm and 4.5 μm bands of the InfraRed Array Camera (IRAC, Fazio et al 2004) on board the warm Spitzer Space Telescope (Werner et al 2004;Gehrz et al 2007 events, SN 2014J and SN 2014dt, are discussed in detail in Johansson et al (2014) and Fox et al (2016),respectively.…”

Section: The Supernova Sample and Spitzer/irac Photometrymentioning

confidence: 99%

A Systematic Study of Mid-Infrared Emission From Core-Collapse Supernovae With Spirits

Tinyanont

Kasliwal

Fox

et al. 2016

ApJ

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We present a systematic study of mid-infrared emission from 141 nearby supernovae (SNe)observed with Spitzer/ IRAC as part of the ongoing SPIRITS survey. We detect 8 Type Ia and 36 core-collapse SNe. All TypeIa/Ibc SNebecome undetectable within threeyears of explosion, whereas 22±11% of TypeII SNecontinue to be detected. Five TypeII SNe are detected even two decades after discovery (SN 1974E, 1979C, 1980K, 1986J, and 1993J). Warm dust luminosity, temperature, and a lower limit on mass are obtained by fitting the two IRAC bands, assuming an optically thin dust shell. We derive warm dust masses between 10 −6 and 10 −2 M e and dust color temperatures between 200 and 1280 K. This observed warm dust could be pre-existing or newly created, but in either case represents a lower limit to the dust mass because cooler dust may be present. We present three case studies of extreme SNe.SN 2011ja (II-P) was over-luminous ([4.5] = −15.6 mag) at 900 days post explosion with increasing hot dust mass, suggesting either an episode of dust formation or intensifying circumstellar material (CSM) interactions heating up pre-existing dust. SN 2014bi (II-P) showed a factor of 10 decrease in dust mass over one month, suggesting either dust destruction or reduced dust heating. The IR luminosity of SN 2014C (Ib) stayedconstant over 800 days, possibly due to strong CSM interaction with anH-rich shell, which is rare among stripped-envelope SNe. The observations suggest that this CSM shell originated from an LBV-like eruption roughly 100 years pre-explosion. The observed diversity demonstrates the power of mid-IR observations of a large sample of SNe.

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AN EXCESS OF MID-INFRARED EMISSION FROM THE TYPE Iax SN 2014dt

Cited by 42 publications

References 41 publications

Wait for It: Post-Supernova Winds Driven by Delayed Radioactive Decays

Wait for It: Post-Supernova Winds Driven by Delayed Radioactive Decays

Subdwarf B stars as possible surviving companions in Type Ia supernova remnants

A Systematic Study of Mid-Infrared Emission From Core-Collapse Supernovae With Spirits

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