The Circumstellar Environments of Double-peaked, Calcium-strong Transients 2021gno and 2021inl

Jacobson-Galán, W. V.; Venkatraman, Padma; Margutti, R.; Khatami, David; Terreran, G.; Foley, R. J.; Angulo, Rodrigo; Angus, C.; Auchettl, Katie; Blanchard, P. K.; Bobrick, Alexey; Bright, J. S.; Brout, D.; Chambers, K.; Couch, C. D.; Coulter, D. A.; Clever, Karoli E.; Davis, Kyle W.; Boer, T. J. L. de; DeMarchi, L. M.; Dodd, Sierra A.; Jones, D. O.; Johnson, Jennifer A.; Kilpatrick, C. D.; Khetan, N.; Lai, Z.; Langeroodi, Danial; Lin, Chien-Cheng; Magnier, E. A.; Milisavljevic, Dan; Perets, Hagai B.; Pierel, Justin; Raymond, J. C.; Rest, S.; Rest, A.; Ridden-Harper, Ryan; Shen, Ken J.; Siebert, M. R.; Smith, C.; Taggart, K.; Tinyanont, Samaporn; Valdés, F.; Villar, A.; Wang, Q.; Yadavalli, S. K.; Zenati, Yossef; Zenteno, A.

doi:10.3847/1538-4357/ac67dc

Cited by 19 publications

(15 citation statements)

References 101 publications

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“…In the H-poor case, however, the radii are smaller (≈ 3×10 12 cm) and the envelope masses are larger (≈ 10 −1 M ). These values are more consistent with those estimated for Type Ib and Ca-rich transients with observed SCE (e.g., Yao et al 2020;Jacobson-Galán et al 2022).…”

Section: Best-fit Analytic Modelssupporting

confidence: 90%

“…Some objects that exist in the literature with both low ejecta and 56 Ni masses and observed SCE are peculiar SNe Ib as well as Ca-rich transients. However, it is difficult to reconcile the photospheric-phase spectra of SN 2020bio, which are most similar to those of other SNe IIb, with the spectra of these objects, which are often used to argue for a degenerate or ultra-stripped progenitor (Yao et al 2020;Jacobson-Galán et al 2022). Instead, it is more likely that SN 2020bio had a massive star progenitor more similar to the progenitors of other SNe IIb based on their similar spectral features.…”

Section: Discussionmentioning

confidence: 99%

“…Comparing observed SCE to analytical and numerical models is one of the only ways of directly measuring the radii and stellar structure of core-collapse progenitors from SN observations. This has been done for a handful of SNe IIb as well as SNe of other subtypes, including stripped-envelope Type Ib SNe (e.g., Modjaz et al 2009;Yao et al 2020), short-plateau Type II SNe (Hiramatsu et al 2021), and exotic Ca-rich transients (e.g., Jacobson-Galán et al 2020, 2022. Analytical and numerical modeling of double-peaked SNe IIb generally yield large radii progenitors (≈ 100-500 R ) with lowmass (≈ 10 −2 -10 −1 M ) extended envelopes (Piro et al 2021, and references therein).…”

Section: Introductionmentioning

confidence: 99%

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SN 2020bio: A Double-peaked Type IIb Supernova with Evidence of Early-time Circumstellar Interaction

Pellegrino¹,

Hiramatsu²,

Arcavi³

et al. 2023

Preprint

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We present photometric and spectroscopic observations of SN 2020bio, a double-peaked Type IIb supernova (SN) discovered within a day of explosion, primarily obtained by Las Cumbres Observatory and Swift. SN 2020bio displays a rapid and long-lasting initial decline throughout the first week of its light curve, similar to other well-studied Type IIb SNe. This early-time emission is thought to originate from the cooling of the extended outer envelope of the progenitor star that is shock-heated by the SN explosion. We compare SN 2020bio to a sample of other double-peaked Type IIb SNe to investigate its progenitor properties. Analytical model fits to the early-time emission give progenitor radius (≈ 100-1500 R ) and H-rich envelope mass (≈ 0.01-0.5 M ) estimates that are consistent with other Type IIb SNe. However, SN 2020bio displays several peculiarities, including: 1) weak H spectral features and narrow emission lines indicative of pre-existing circumstellar material; 2) an underluminous secondary light curve peak which implies a small amount of synthesized 56 Ni (M Ni ≈ 0.02 M ); and 3) lowluminosity nebular [O I] features. These observations are more consistent with a lower-mass progenitor (M ZAMS ≈ 12 M ) that was stripped of most of its H envelope before exploding. This study adds to the growing diversity in the observed properties of Type IIb SNe and their progenitors.

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Section: Best-fit Analytic Modelssupporting

confidence: 90%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

SN 2020bio: A Double-peaked Type IIb Supernova with Evidence of Early-time Circumstellar Interaction

Pellegrino¹,

Hiramatsu²,

Arcavi³

et al. 2023

Preprint

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“…Overall, the r − i colors (Figure 8) of the fca 1 and fca 2 models are consistent with the observed color evolution of CaSNe; these models also show some consistency to the B − V colors of the SNe Ia varieties shown in Figure 8 but are slightly bluer overall than SN 2019ehk's evolution. Left/Right: early-time absolute r-band light curves in the AB magnitude system of fca 1 (green curve), fca 2 (blue curve), and fca 3 (red curve) with respect to other classified Ca-rich transients (Perets et al 2010;Sullivan et al 2011;Kasliwal et al 2012;Lunnan et al 2017;De et al 2018;Jacobson-Galán et al 2020a, 2022. Peculiar, "calcium-strong" SN2016hnk (Galbany et al 2019;Jacobson-Galán et al 2020b) is also presented for reference (polygons).…”

Section: Comparison To Casne Observationsmentioning

confidence: 99%

“…Figure4. Left/Right: early-time absolute r-band light curves in the AB magnitude system of fca 1 (green curve), fca 2 (blue curve), and fca 3 (red curve) with respect to other classified Ca-rich transients(Perets et al 2010;Sullivan et al 2011;Kasliwal et al 2012;Lunnan et al 2017;De et al 2018;Jacobson-Galán et al 2020a, 2022. Peculiar, "calcium-strong" SN2016hnk(Galbany et al 2019;Jacobson-Galán et al 2020b) is also presented for reference (polygons).…”

mentioning

confidence: 99%

The Origins of Calcium-rich Supernovae From Disruptions of CO White Dwarfs by Hybrid He–CO White Dwarfs

Zenati

Perets

Jacobson-Galán

et al. 2023

ApJ

Self Cite

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Calcium-rich explosions are very faint (M B ∼ −15.5), type I supernovae (SNe) showing strong Ca lines, mostly observed in old stellar environments. Several models for such SNe have been explored and debated, but none were able to reproduce consistently the observed properties of Ca-rich SNe, nor their rates and host-galaxy distributions. Here we show that the disruptions of low-mass carbon–oxygen (CO) white dwarfs (WDs) by hybrid helium–CO (HeCO) WDs during their merger could explain the origin and properties of such SNe. We make use of detailed multidimensional hydrodynamical-thermonuclear (FLASH) simulations to characterize such explosions. We find that the accretion of CO material onto an HeCO-WD heats its He shell and eventually leads to its “weak” detonation and ejection and the production of a sub-energetic ∼1049 erg Ca-rich SN, while leaving the CO core of the HeCO-WD intact as a hot remnant WD, possibly giving rise to X-ray emission as it cools down. We model the detailed light curves and spectra of such explosions and find excellent agreement with the observations of Ia/c Ca-rich, and potentially Ib Ca-rich, SNe. We thereby provide a viable, consistent model for the origins of Ca-rich SNe. These findings can shed new light on the role of Ca-rich SNe in the chemical evolution of galaxies and the intracluster medium, and their contribution to the observed 511 Kev signal in the galaxy originating from positrons produced from 44Ti decay. Finally, the origins of such SNe points to the key role of HeCO-WDs as SN progenitors and their potential role as progenitors of other thermonuclear SNe including normal Ia.

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Supernova double-peaked light curves from double-nickel distribution

Orellana

Bersten

2022

A&A

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Among supernovae (SNe) of different luminosities, many double-peaked light curves (LCs) have been observed, representing a broad morphological variety. In this work, we investigate which of these can be modelled by assuming a double-peaked distribution of their radioactive material, as originally proposed for SN2005bf. The inner zone corresponds to the regular explosive nucleosynthesis and extends outwards, according to the usual scenario of mixing. The outer 56 Ni-rich shell may be related to the effect of jet-like outflows that have interacted with more distant portions of the star before the arrival of the SN shock. As the outer layer is covered by matter that is optically less thick, its energy emerges earlier and generates a first peak of radiation. To investigate this scenario in more detail, we have applied our hydrodynamic code that follows the shock propagation through the progenitor star and takes into account the effect of the γ-ray photons produced by the decay of the radioactive isotopes. We present a simple parametric model for the 56 Ni abundance profile and explore the consequences on the LC of individually varying the quantities that define this distribution, setting our focus onto the stripped-envelope progenitors. In this first study, we are interested in the applicability of this model to SNe that have not been classified as superluminous, thus, we have selected our parameter space accordingly. Then, within the same mathematical prescription for the 56 Ni-profile, we revisited the modelling process for a series of objects: SN2005bf, PTF2011mnb, SN2019cad, and SN2008D. In some cases, a decrease in the gamma ray opacity is required to fit the late time observations. We also discuss the other cases in which this scenario might be likely to explain the LC morphology. A steep initial decline in the observed bolometric LC within less than few days after the explosion becomes less feasible for this model, because it requires a large abundance of 56 Ni near the stellar surface, indicating a strongly inverted distribution. An initial bolometric rise before the two peaks seems more favourable for the double-nickel case, particularly as it can be difficult to explain through other scenarios, unless a combination of power sources is invoked.

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The Circumstellar Environments of Double-peaked, Calcium-strong Transients 2021gno and 2021inl

Cited by 19 publications

References 101 publications

SN 2020bio: A Double-peaked Type IIb Supernova with Evidence of Early-time Circumstellar Interaction

SN 2020bio: A Double-peaked Type IIb Supernova with Evidence of Early-time Circumstellar Interaction

The Origins of Calcium-rich Supernovae From Disruptions of CO White Dwarfs by Hybrid He–CO White Dwarfs

Supernova double-peaked light curves from double-nickel distribution

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