The Origin and Evolution of the Normal Type Ia SN 2018aoz with Infant-phase Reddening and Excess Emission

Ni, Yuan Qi; Moon, D. S.; Drout, M. R.; Polin, Abigail; Sand, David J.; González–Gaitán, S.; Kim, Sang Chul; Lee, Youngdae; Park, Hong Soo; Howell, D. Andrew; Nugent, P.; Piro, Anthony L.; Brown, P. J.; Galbany, L.; Burke, J.; Hiramatsu, D.; Hosseinzadeh, G.; Valenti, S.; Afsariardchi, Niloufar; Andrews, Jennifer E.; Antoniadis, John; Beaton, Rachael L.; Bostroem, Azalee; Carlberg, R. G.; Cenko, S. Bradley; Cha, Sang-Mok; Dong, Yize; Gal‐Yam, A.; Haislip, J.; Holoien, T. W. S.; Johnson, Sean D.; Kouprianov, V. V.; Lee, Yongseok; Matzner, Christopher D.; Morrell, N.; McCully, C.; Pignata, G.; Reichart, D.; Ryder, S. D.; Smith, Nathan; Wyatt, S.; Yang, S.

doi:10.3847/1538-4357/aca9be

Cited by 12 publications

(18 citation statements)

References 160 publications

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“…A striking aspect of SN 2022xkq's color evolution is its very red color immediately following explosion (until ∼ − 10 days before the time of B max ), which is especially notable in the (B − i) color curve, though it is present in all bands. The strong red color is somewhat similar to that observed in SN 2018aoz (Ni et al 2022(Ni et al , 2023a. However, SN 2022xkq is generally redder than SN 2018aoz, and there is no bright bump in SN 2022xkq as was observed in the very early light curve of SN 2018aoz.…”

Section: Photometric Propertiessupporting

confidence: 76%

“…This process has been suggested as an explosion mechanism for producing underluminous SNe Ia (Polin et al 2019;Gronow et al 2021). Further, double-detonation models are linked to early red excesses in SNe Ia (Jiang et al 2017;Ni et al 2023a; see Section 8.1 for further discussion). We compare the Polin et al (2019) double-detonation models to the observations of SN 2022xkq.…”

Section: Double Detonationmentioning

confidence: 93%

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Strong Carbon Features and a Red Early Color in the Underluminous Type Ia SN 2022xkq

Pearson,

Sand,

Lundqvist

et al. 2023

ApJ

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We present optical, infrared, ultraviolet, and radio observations of SN 2022xkq, an underluminous fast-declining Type Ia supernova (SN Ia) in NGC 1784 (D ≈ 31 Mpc), from <1 to 180 days after explosion. The high-cadence observations of SN 2022xkq, a photometrically transitional and spectroscopically 91bg-like SN Ia, cover the first days and weeks following explosion, which are critical to distinguishing between explosion scenarios. The early light curve of SN 2022xkq has a red early color and exhibits a flux excess that is more prominent in redder bands; this is the first time such a feature has been seen in a transitional/91bg-like SN Ia. We also present 92 optical and 19 near-infrared (NIR) spectra, beginning 0.4 days after explosion in the optical and 2.6 days after explosion in the NIR. SN 2022xkq exhibits a long-lived C i 1.0693 μm feature that persists until 5 days post-maximum. We also detect C ii λ6580 in the pre-maximum optical spectra. These lines are evidence for unburnt carbon that is difficult to reconcile with the double detonation of a sub-Chandrasekhar mass white dwarf. No existing explosion model can fully explain the photometric and spectroscopic data set of SN 2022xkq, but the considerable breadth of the observations is ideal for furthering our understanding of the processes that produce faint SNe Ia.

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Section: Photometric Propertiessupporting

confidence: 76%

Section: Double Detonationmentioning

confidence: 93%

Strong Carbon Features and a Red Early Color in the Underluminous Type Ia SN 2022xkq

Pearson,

Sand,

Lundqvist

et al. 2023

ApJ

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“…Underluminous SNe Ia with strong UV excesses include iPTF14atg (Cao et al 2015) and SN 2019yvq (Miller et al 2020;Siebert et al 2020;Burke et al 2021;Tucker et al 2021). MUSSES16D4 (Jiang et al 2017) and SN 2018aoz (Ni et al 2022(Ni et al , 2023b, on the other hand, show early red excesses. Normal Type Ia SN 2018oh (Dimitriadis et al 2019a;Li et al 2019;Shappee et al 2019) and overluminous (03fg-like) Type Ia SN 2021zny (Dimitriadis et al 2023) also show early excesses in their high-cadence unfiltered light curves from Kepler 2 and the Transiting Exoplanet Survey Satellite (TESS), respectively, although the color of this excess is not known.…”

Section: Introductionmentioning

confidence: 99%

The Early Light Curve of SN 2023bee: Constraining Type Ia Supernova Progenitors the Apian Way

Hosseinzadeh,

Sand,

Sarbadhicary

et al. 2023

ApJL

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We present very early photometric and spectroscopic observations of the Type Ia supernova (SN Ia) 2023bee, starting about 8 hr after the explosion, which reveal a strong excess in the optical and nearest UV (U and UVW1) bands during the first several days of explosion. This data set allows us to probe the nature of the binary companion of the exploding white dwarf and the conditions leading to its ignition. We find a good match to the Kasen model in which a main-sequence companion star stings the ejecta with a shock as they buzz past. Models of double detonations, shells of radioactive nickel near the surface, interaction with circumstellar material, and pulsational delayed detonations do not provide good matches to our light curves. We also observe signatures of unburned material, in the form of carbon absorption, in our earliest spectra. Our radio nondetections place a limit on the mass-loss rate from the putative companion that rules out a red giant but allows a main-sequence star. We discuss our results in the context of other similar SNe Ia in the literature.

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“…Excess emission has been identified within ∼5 days post-explosion in a few normal events (Marion et al 2016;Hosseinzadeh et al 2017;Jiang et al 2018Jiang et al , 2021Dimitriadis et al 2019Dimitriadis et al , 2023Deckers et al 2022;Sai et al 2022), and HV Si II and Ca II features, which are faster than the normal photospheric velocities (PVs) by 7000 km s −1 (Wang et al 2003;Gerardy et al 2004;Quimby et al 2006;Marion et al 2013;Silverman et al 2015), have been observed in a number of normal events before B-band maximum. In the case of the earliest Type Ia SN detected to date, SN 2018aoz, infant-phase excess emission during 1-12 hr since first light showed suppressed B-band flux attributed to line-blanket absorption by surface iron-peak elements (Ni et al 2022(Ni et al , 2023.…”

Section: Introductionmentioning

confidence: 97%

Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx

Ni,

Moon,

Drout

et al. 2023

ApJ

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SN 2021aefx is a normal Type Ia supernova (SN) showing excess emission and redward color evolution over the first ∼ 2 days. We present analyses of this SN using our high-cadence KMTNet multiband photometry, spectroscopy, and publicly available data, including first measurements of its explosion epoch (MJD 59529.32 ± 0.16) and onset of power-law rise (t PL = MJD 59529.85 ± 0.55; often called first light) associated with the main ejecta 56Ni distribution. The first KMTNet detection of SN 2021aefx precedes t PL by ∼ 0.5 hr, indicating presence of additional power sources. Our peak-spectrum confirms its intermediate Type Ia subclassification between core-normal and broad-Line, and we estimate an ejecta mass of ∼ 1.34 M ⊙. The spectral evolution identifies material reaching >40,000 km s−1 (fastest ever observed in Type Ia SNe) and at least two split-velocity ejecta components expanding homologously: (1) a normal-velocity (∼ 12,400 km s−1) component consistent with typical photospheric evolution of near-Chandrasekhar-mass ejecta; and (2) a high-velocity (∼ 23,500 km s−1) secondary component visible during the first ∼ 3.6 days post-explosion, which locates the component within the outer <16% of the ejecta mass. Asymmetric subsonic explosion processes producing a nonspherical secondary photosphere provide an explanation for the simultaneous appearance of the two components, and may also explain the excess emission via a slight 56Ni enrichment in the outer ∼ 0.5% of the ejecta mass. Our 300 days post-peak nebular-phase spectrum advances constraints against nondegenerate companions and further supports a near-Chandrasekhar-mass explosion origin. Off-center ignited delayed-detonations are likely responsible for the observed features of SN 2021aefx in some normal Type Ia SNe.

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The Origin and Evolution of the Normal Type Ia SN 2018aoz with Infant-phase Reddening and Excess Emission

Cited by 12 publications

References 160 publications

Strong Carbon Features and a Red Early Color in the Underluminous Type Ia SN 2022xkq

Strong Carbon Features and a Red Early Color in the Underluminous Type Ia SN 2022xkq

The Early Light Curve of SN 2023bee: Constraining Type Ia Supernova Progenitors the Apian Way

Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx

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