AT 2019qyl in NGC 300: Internal Collisions in the Early Outflow from a Very Fast Nova in a Symbiotic Binary*
               
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Jencson, J.; Andrews, Jennifer E.; Bond, Howard E.; Karambelkar, Viraj; Sand, David J.; Dyk, Schuyler D. Van; Blagorodnova, N.; Boyer, Martha L.; Kasliwal, Mansi M.; Lau, Ryan M.; Mohamed, S.; Williams, Robert E.; Whitelock, Patricia; Amaro, R.; Bostroem, K. A.; Dong, Yize; Lundquist, M.; Valenti, S.; Wyatt, S.; Burke, Jamie; De, Kishalay; Johansson, Joel; Rojas-Bravo, C.; Coulter, D. A.; Foley, R. J.; Gehrz, R. D.; Haislip, J.; Hiramatsu, D.; Howell, D. A.; Kilpatrick, C. D.; Masci, Frank J.; McCully, C.; Ngeow, Chow-Choong; Pan, Y. C.; Pellegrino, C.; Piro, Anthony L.; Kouprianov, V. V.; Reichart, D.; Rest, A.; Rest, S.; Smith, Nathan

doi:10.3847/1538-4357/ac1424

Cited by 4 publications

(4 citation statements)

References 169 publications

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“…We also discard PSN +204.332083−29.896833 in NGC 5236, which has minimal reported data and is outside of the mapped region of the galaxy. Finally, we remove three SNe (SN 1997bs, SN 2019krl, and SN 2019qyl) from our sample because of uncertainty in their type classification and the likelihood that they are instead nonterminal explosions (Adams & Kochanek 2015;Andrews et al 2021;Jencson et al 2021;Ransome et al 2021). This brings our sample size to 63 SNe within 31 galaxies.…”

Section: Methodsmentioning

confidence: 99%

Comparing the Locations of Supernovae to CO (2–1) Emission in Their Host Galaxies

Chen

Leroy

Lopez

et al. 2023

ApJ

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We measure the molecular gas environment near recent (<100 yr old) supernovae (SNe) using ∼1″ or ≤150 pc resolution CO (2–1) maps from the PHANGS–Atacama Large Millimeter/submillimeter Array (ALMA) survey of nearby star-forming galaxies. This is arguably the first such study to approach the scales of individual massive molecular clouds (M mol ≳ 105.3 M ⊙). Using the Open Supernova Catalog, we identify 63 SNe within the PHANGS–ALMA footprint. We detect CO (2–1) emission near ∼60% of the sample at 150 pc resolution, compared to ∼35% of map pixels with CO (2–1) emission, and up to ∼95% of the SNe at 1 kpc resolution, compared to ∼80% of map pixels with CO (2–1) emission. We expect the ∼60% of SNe within the same 150 pc beam, as a giant molecular cloud will likely interact with these clouds in the future, consistent with the observation of widespread SN–molecular gas interaction in the Milky Way, while the other ∼40% of SNe without strong CO (2–1) detections will deposit their energy in the diffuse interstellar medium, perhaps helping drive large-scale turbulence or galactic outflows. Broken down by type, we detect CO (2–1) emission at the sites of ∼85% of our 9 stripped-envelope SNe (SESNe), ∼40% of our 34 Type II SNe, and ∼35% of our 13 Type Ia SNe, indicating that SESNe are most closely associated with the brightest CO (2–1) emitting regions in our sample. Our results confirm that SN explosions are not restricted to only the densest gas, and instead exert feedback across a wide range of molecular gas densities.

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Section: Methodsmentioning

confidence: 99%

Comparing the Locations of Supernovae to CO (2–1) Emission in Their Host Galaxies

Chen

Leroy

Lopez

et al. 2023

ApJ

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“…The WD in V407 Cyg is at least 1.2 M e (Mikolajewska 2010), and may be as massive as 1.35-1.37 M e (Hachisu & Kato 2012). (2) AT 2019qyl is a nova with an O-rich AGB donor in the nearby Sculptor Group galaxy NGC 300 (Jencson et al 2021). Jencson et al (2021) estimated that the allowed range of the AGB star mass in AT 2019qyl is M 2 = 1.2-2.0 M e , with the best-fitting value is M 2 = 1.2 M e and the orbital period P  1800 days by assuming the mass ratio to be 1.…”

Section: Introductionmentioning

confidence: 99%

“…(2) AT 2019qyl is a nova with an O-rich AGB donor in the nearby Sculptor Group galaxy NGC 300 (Jencson et al 2021). Jencson et al (2021) estimated that the allowed range of the AGB star mass in AT 2019qyl is M 2 = 1.2-2.0 M e , with the best-fitting value is M 2 = 1.2 M e and the orbital period P  1800 days by assuming the mass ratio to be 1. In the present work, we found that the estimated parameters of AT 2019qyl can be covered based on the WD+AGB channel, also known as the AGB donor channel.…”

Section: Introductionmentioning

confidence: 99%

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The Progenitors of Type Ia Supernovae with Asymptotic Giant Branch Donors

Liu²,

Wang

2023

Res. Astron. Astrophys.

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Type Ia supernovae (SNe Ia) are among the most energetic events in the Universe. They are excellent cosmological distance indicators due to the remarkable homogeneity of their light curves. However, the nature of the progenitors of SNe Ia is still not well understood. In the single-degenerate model, a carbon-oxygen white dwarf (CO WD) could grow its mass by accreting material from an asymptotic giant branch (AGB) star, leading to the formation of SNe Ia when the mass of WD approaches to the Chandrasekhar-mass limit, known as the AGB donor channel. In this channel, previous studies mainly concentrate on the wind-accretion pathway for the mass-increase of the WDs. In the present work, we employed an integrated mass-transfer prescription for semidetached WD+AGB systems, and evolved a number of WD+AGB systems to the formation of SNe Ia through the Roche-lobe overflow process or the wind-accretion process. We provided the initial and final parameter spaces of WD+AGB systems for producing SNe Ia. We also provided the density distribution of circumstellar matter at the moment when the WD mass reaches the Chandrasekhar-mass limit. Moreover, we found that the massive WD+AGB sample AT 2019qyl can be covered by our final parameter space for producing SNe Ia, indicating that AT 2019qyl is a strong progenitor candidate of SNe Ia with AGB donors.

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Discovery of a probable very fast extragalactic nova in a symbiotic binary

Modiano

Wijnands

2022

A&A

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Very fast novae are novae that evolve exceptionally quickly (on timescales of only days). Due to their rapid evolution, very fast novae are challenging to detect and study, especially at early times. Here we report the discovery, made as part of our Transient UV Objects project, of a probable very fast nova in the nearby spiral galaxy NGC 300. We detected the rise to the peak (which are rarely observed for very fast novae) in the near-ultraviolet (NUV), with the first detection just ∼ 2 hours after the eruption started. The peak and early stages of the decay were also observed in UV and optical bands. The source rapidly decayed (two NUV magnitudes within 3.5 days), making it one of the fastest novae known. In addition, a likely quiescent counterpart was found in archival near-infrared Spitzer and VIRCAM images, but not in any deep optical and UV observations, indicating a very red spectral shape in quiescence. The outburst and quiescence properties suggest that the system is likely a symbiotic binary. We discuss this new transient in the context of very fast novae in general and specifically as a promising supernova Type Ia progenitor candidate, due to its very high inferred WD mass (∼ 1.35 M ⊙ ; determined by comparing this source to other very fast novae).

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AT 2019qyl in NGC 300: Internal Collisions in the Early Outflow from a Very Fast Nova in a Symbiotic Binary* †

Cited by 4 publications

References 169 publications

Comparing the Locations of Supernovae to CO (2–1) Emission in Their Host Galaxies

Comparing the Locations of Supernovae to CO (2–1) Emission in Their Host Galaxies

The Progenitors of Type Ia Supernovae with Asymptotic Giant Branch Donors

Discovery of a probable very fast extragalactic nova in a symbiotic binary

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