Near-infrared and Optical Observations of Type Ic SN 2020oi and Broad-lined Type Ic SN 2020bvc: Carbon Monoxide, Dust, and High-velocity Supernova Ejecta

Rho, Jeonghee; Evans, A.; Geballe, T. R.; Banerjee, D. P. K.; Hoêflich, P.; Shahbandeh, Melissa; Valenti, S.; Yoon, Sung Chul; Jin, Hyeong Min; Williamson, Marc; Modjaz, M.; Hiramatsu, D.; Howell, D. A.; Pellegrino, C.; Vinkó, J.; Cartier, R.; Burke, Jamie; McCully, C.; An, Hongjun; Cha, Hwa-Young; Pritchard, T.; Wang, X.; Andrews, Jennifer E.; Galbany, L.; Dyk, Schuyler van; Graham, M. L.; Блинников, С. И.; Joshi, Vishal; Pál, András; Kriskovics, L.; Ordasi, A.; Szakáts, R.; Vida, K.; Chen, Z.; Li, X.; JJ, Zhang; Yan, Shengyu

doi:10.3847/1538-4357/abd850

Cited by 39 publications

(59 citation statements)

References 147 publications

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“…He I features are found to be weaker/absent in SNe Ic (e.g. SN 2007gr: Hunter et al 2009; however, in addition to this, broadline SNe Ic exhibit weak signatures of C I (SN 2020bvc: Rho et al 2021), which indicate large envelope mass stripping in such events. Additionally, SNe Ib present stronger He I λ20 580 in comparison with that displayed in the NIR spectra of SNe Ic.…”

Section: Introductionmentioning

confidence: 89%

“…The spectra presented are in rest-frame wavelengths and also corrected for extinction using E(B − V) = 0.063 mag (Milisavljevic et al 2013), exhibiting a decrease in flux with wavelength, typically observed in SESNe. Line identifications of NIR spectra were done following Gerardy et al (2002), Hunter et al (2009), Banerjee et al (2018), andRho et al (2021). The vertical red bands denote regions of poor atmospheric transparency.…”

Section: Nir Spectroscopic Evolutionmentioning

confidence: 99%

“…: Gerardy et al 2002; SN 2007gr (Ic): Hunter et al 2009; LSQ13abf (Ib): Stritzinger et al 2020; iPTF13bvn (Ib): Fremling et al 2016; SN 2013ge (Ib/c): Drout et al 2016; SN 2016adj (IIb/Ib): Banerjee et al 2018; SN 2020oi (Ic) and SN 2020bvc (Ic):Rho et al 2021). In this section, we present NIR spectroscopy of SN 2012au based on spectra at two epochs (at −5 and +21.8 d since maximum) observed using SOFI on NTT-3.58m…”

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confidence: 99%

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Photometric, polarimetric, and spectroscopic studies of the luminous, slow-decaying Type Ib SN 2012au

Kumar

Anupama

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Optical, near-infrared (NIR) photometric and spectroscopic studies, along with the optical imaging polarimetric results for SN 2012au, are presented in this article to constrain the nature of the progenitor and other properties. Well-calibrated multiband optical photometric data (from –0.2 to +413 d since B-band maximum) were used to compute the bolometric light curve and to perform semi-analytical light-curve modelling using the minim code. A spin-down millisecond magnetar-powered model explains the observed photometric evolution of SN 2012au reasonably. Early-time imaging polarimetric follow-up observations (–2 to +31 d) and comparison with other similar cases indicate signatures of asphericity in the ejecta. Good spectral coverage of SN 2012au (from –5 to +391 d) allows us to trace the evolution of layers of SN ejecta in detail. SN 2012au exhibits higher line velocities in comparison with other SNe Ib. Late nebular phase spectra of SN 2012au indicate a Wolf–Rayet star as the possible progenitor for SN 2012au, with oxygen, He-core, and main-sequence masses of ∼1.62 ± 0.15 M⊙, ∼4–8 M⊙, and ∼17–25 M⊙, respectively. There is a clear absence of a first overtone of carbon monoxide (CO) features up to +319 d in the K-band region of the NIR spectra. Overall analysis suggests that SN 2012au is one of the most luminous slow-decaying Type Ib SNe, having comparatively higher ejecta mass (∼ 4.7–8.3 M⊙) and kinetic energy (∼ [4.8–5.4] × 1051 erg). Detailed modelling using mesa and the results obtained through stella and snec explosions also strongly support spin-down of a magnetar with mass of around 20 M⊙ and metallicity Z = 0.04 as a possible powering source of SN 2012au.

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Section: Introductionmentioning

confidence: 89%

Section: Nir Spectroscopic Evolutionmentioning

confidence: 99%

mentioning

confidence: 99%

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Photometric, polarimetric, and spectroscopic studies of the luminous, slow-decaying Type Ib SN 2012au

Kumar

Anupama

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Adopting a broken power law for the ejecta density structure, the properties of the SN ejecta are specified by the ejecta mass (M ej ), kinetic energy (E K ), and the power-law indices of the inner and outer density distributions in the ejecta velocity coordinate (v); the inner index is set to be 0, and the outer one is denoted as n (ρ SN ∝ v −n ). We adopt M ej = 1M , E K = 10 51 ergs, and n = 10, being roughly consistent with the optical light curve modeling (Rho et al 2021). We emphasize that the details of these parameters on the ejecta properties are not important for our purpose, which is to demonstrate the need for the non-smooth CSM as argued in Section 3 in a model-independent way.…”

Section: Light Curve Models and The Csm Environmentmentioning

confidence: 68%

“…The recent development of high-cadence surveys now allows multi-wavelength follow-up observations of SNe in the infant phase (Bellm et al 2019;Graham et al 2019). SN Ic 2020oi in the nearby galaxy M100 (∼ 15 Mpc) was discovered on 7 Jan 2020, 13:00:54 (UT) in a very infant phase (∼ 1 day after the putative explosion date; 6 Jan 2020, JD 58854.0 ± 1.5) (Förster et al 2020;Horesh et al 2020;Siebert et al 2020;Rho et al 2021). In this paper, we present the data from our ALMA observations for SN 2020oi (Section 2).…”

Section: Introductionmentioning

confidence: 99%

The final months of massive star evolution from the circumstellar environment around SN Ic 2020oi

Maeda,

Chandra,

Matsuoka

et al. 2021

Preprint

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We present the results of ALMA band 3 observations of a nearby type Ic supernova (SN) 2020oi. Under the standard assumptions on the SN-circumstellar medium (CSM) interaction and the synchrotron emission, the data indicate that the CSM structure deviates from a smooth distribution expected from the steady-state mass loss in the very vicinity of the SN ( ∼ < 10 15 cm), which is then connected to the outer smooth distribution ( ∼ > 10 16 cm). This structure is further confirmed through the light curve modeling of the whole radio data set as combined with data at lower frequency previously reported. Being an explosion of a bare carbon-oxygen (C+O) star having a fast wind, we can trace the mass-loss history of the progenitor of SN 2020oi in the final year. The inferred nonsmooth CSM distribution corresponds to fluctuations on the sub-year time scale in the mass-loss history toward the SN explosion. Our finding suggests that the pre-SN

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Nebular phase properties of supernova Ibc from He-star explosions

Hillier

Sukhbold

Woosley

et al. 2021

A&A

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Following our recent work on Type II supernovae (SNe), we present a set of 1D nonlocal thermodynamic equilibrium radiative transfer calculations for nebular-phase Type Ibc SNe starting from state-of-the-art explosion models with detailed nucleosynthesis. Our grid of progenitor models is derived from He stars that were subsequently evolved under the influence of wind mass loss. These He stars, which most likely form through binary mass exchange, synthesize less oxygen than their single-star counterparts with the same zero-age main sequence (ZAMS) mass. This reduction is greater in He-star models evolved with an enhanced mass loss rate. We obtain a wide range of spectral properties at 200 d. In models from He stars with an initial mass > 6 M⊙, the [O I] λλ 6300, 6364 is of a comparable or greater strength than [Ca II] λλ 7291, 7323 – the strength of [O I] λλ 6300, 6364 increases with the He-star initial mass. In contrast, models from lower mass He stars exhibit a weak [O I] λλ 6300, 6364, strong [Ca II] λλ 7291, 7323, and also strong N II lines and Fe II emission below 5500 Å. The ejecta density, which is modulated by the ejecta mass, the explosion energy, and clumping, has a critical impact on gas ionization, line cooling, and spectral properties. We note that Fe II dominates the emission below 5500 Å and is stronger at earlier nebular epochs. It ebbs as the SN ages, while the fractional flux in [O I] λλ 6300, 6364 and [Ca II] λλ 7291, 7323 increases with a similar rate as the ejecta recombine. Although the results depend on the adopted wind mass loss rate and pre-SN mass, we find that He-stars of 6–8 M⊙ initially (ZAMS mass of 23–28 M⊙) match the properties of standard SNe Ibc adequately. This finding agrees with the offset in progenitor masses inferred from the environments of SNe Ibc relative to SNe II. Our results for less massive He stars are more perplexing since the predicted spectra are not seen in nature. They may be missed by current surveys or associated with Type Ibn SNe in which interaction power dominates over decay power.

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Near-infrared and Optical Observations of Type Ic SN 2020oi and Broad-lined Type Ic SN 2020bvc: Carbon Monoxide, Dust, and High-velocity Supernova Ejecta

Cited by 39 publications

References 147 publications

Photometric, polarimetric, and spectroscopic studies of the luminous, slow-decaying Type Ib SN 2012au

Photometric, polarimetric, and spectroscopic studies of the luminous, slow-decaying Type Ib SN 2012au

The final months of massive star evolution from the circumstellar environment around SN Ic 2020oi

Nebular phase properties of supernova Ibc from He-star explosions

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