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REVIEW 3 major objections 4 minor 142 references

Wild behaviour near the finish line: the Type Ibn SN 2020able and its stratified environment

T0 review · 3 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read This paper argues that the Type Ibn SN 2020able exploded in a stratified, three-layer circumstellar shell, with a compact shocked region, a dense inner shell ejected by a discrete pre-SN eruption similar to SN 2006jc, and an outer shell…

desk verdict A well-observed Ibn with a plausible stratified CSM, but the pre-SN eruption claim rests on an untested assumption about line broadening and needs a direct test. read the letter →

arxiv 2608.07661 v1 pith:YYCLC6AM submitted 2026-08-07 astro-ph.HE

L. Tartaglia , E. Cappellaro , G. Valerin , A. Pastorello , S. Benetti , A. Reguitti , L. Tomasella , P. Lundqvist
show 24 more authors
K. Misra A. Gangopadhyay R. Dastidar B. Ailawadhi Dimple B. Kumar V. K. Jha M. Singh N. Elias-Rosa C. P. Gutiérrez D. A. Howell D. Hiramatsu C. Pellegrino J. Andrews D. J. Sand N. Smith J. Pearson S. Wyatt P. Ochner Y.-Z. Cai J. Burke C. McCully M. Newsome E. Padilla Gonzalez
This is my paper · ORCID
classification astro-ph.HE
keywords TypeIbnsupernovaSN2020ablecircumstellarmediumstratifiedenvironmentWolf-Rayetprogenitorpre-supernovaeruptionelectronscatteringlightcurves
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

SN 2020able, a Type Ibn supernova, exploded inside a stratified circumstellar medium whose separate layers record different mass-loss episodes at the end of its progenitor's life. Using dense UV/optical photometry and spectroscopy, the paper shows that ejecta–circumstellar interaction powered the bright peak (about $4.4\times10^{43}$ erg s$^{-1}$) but lasted only a few days, after which the transient evolved as freely expanding ejecta. The central claim is that the un-shocked environment contains three distinct regions: a compact shocked shell, a dense helium-rich inner shell at $R>9.3\times10^{14}$ cm with electron density about $1.4\times10^{9}$ cm$^{-3}$ and Thomson optical depth about 6.5, and an extended outer shell reaching about $3.3\times10^{15}$ cm and expanding at about $1.2\times10^{3}$ km s$^{-1}$. The dense inner shell's implied mass-loss rate is too high for a steady Wolf-Rayet wind, so the paper concludes it was produced by a discrete pre-supernova eruptive event similar to the one seen in SN 2006jc, while the outer shell's velocity points to a late WN-to-WC Wolf-Rayet progenitor.

What carries the argument

The argument is carried by the interpretation of the constant FWHM (about $3\times10^{3}$ km s$^{-1}$) of the early high-ionization lines (N III, He II, C III) as electron-scattering broadening in an optically thick shell, following the line-profile models of Huang & Chevalier (2018). This converts a measured width into a Thomson optical depth $\tau_{\rm es}\sim6.5$, and with an assumed shell geometry, temperature, and filling factor, into an electron density $n_{\rm e}\sim1.4\times10^{9}$ cm$^{-3}$ and a shell mass near $0.02\,M_\odot$. The companion measurement is the P Cygni absorption velocity ($\sim1.2\times10^{3}$ km s$^{-1}$), which gives the shell's true expansion velocity and is roughly one-third of the scattering FWHM; the ratio between the two is what exposes the mass-loss rate as too high for a steady wind. The time evolution of the narrow He I absorption equivalent width, which drops sharply at about day 47 and disappears by day 70, locates the inner and outer radii of the outer shell, completing the three-layer picture.

What would settle it

Take early-time (before day 16) spectra at resolving power $R>4000$ and measure the resolved profiles of He II 4686 and N III 4634/4641: electron-scattering broadening should produce symmetric profiles with exponential wings and a FWHM that stays near $3\times10^{3}$ km s$^{-1}$ regardless of wavelength, while kinematic broadening should show asymmetric or structured profiles tied to the roughly $1.2\times10^{3}$ km s$^{-1}$ P Cygni velocity. If the constant FWHM dissolves into narrower kinematic components, the dense-shell density, the $0.02\,M_\odot$ mass, and the inferred eruptive mass-loss rate collapse.

Watch

Extended reading notes

Core claim

The paper concludes that SN 2020able possessed a stratified circumstellar environment with three distinct regions at different distances from the progenitor. The innermost region is a shocked, compact shell (outer radius about $3\times10^{13}$ cm) that powered a brief ejecta–CSM interaction within the first few days and produced the high peak luminosity; this shell is too small and short-lived to shape the later evolution. Beyond it, a dense He-rich shell lies at $R>9.3\times10^{14}$ cm, with Thomson optical depth $\tau_{\rm es}\sim6.5$, electron density $n_{\rm e}\sim1.4\times10^{9}$ cm$^{-3}$, and a mass near $0.02\,M_\odot$, inferred from the constant FWHM of the early high-ionization lines interpreted as electron-scattering broadening. Because maintaining such density in a steady wind would require a mass-loss rate of about $8.7\times10^{-2}\,M_\odot$ yr$^{-1}$, inconsistent with radiation-driven wind theory for Wolf-Rayet stars, the paper argues this inner shell was ejected by a discrete pre-SN eruptive event similar to SN 2006jc. The outermost component, spanning roughly $2.2\times10^{15}$ to $3.3\times10^{15}$ cm and expanding at about $1.2\times10^{3}$ km s$^{-1}$, matches the escape velocity of Wolf-Rayet stars, favoring a late WN-to-WC progenitor; the ejecta overtake this shell around day 47, when the narrow He I absorptions suddenly weaken.

Load-bearing premise

Everything hangs on the assumption that the constant $\sim3\times10^{3}$ km s$^{-1}$ width of the early high-ionization lines is electron scattering in a shell with a specific geometry, temperature, and clumping factor; if that width instead comes from gas simply moving at a range of speeds, the inferred density, shell mass, and eruptive mass-loss rate would be far lower.

Editorial extensions

If this is right

  • The luminous peak of SN 2020able was powered by ejecta–CSM interaction confined to the first few days and to a region smaller than about $3\times10^{13}$ cm; after that, the light curve is powered by the ejecta themselves, not by ongoing interaction.
  • The dense inner shell was ejected by a discrete eruptive episode beginning roughly 300 days before explosion, expelling about $0.02\,M_\odot$ at an average rate near $0.7\,M_\odot$ yr$^{-1}$ over about 10 days, similar to the outburst that preceded SN 2006jc.
  • The outer shell's expansion velocity of about $1.2\times10^{3}$ km s$^{-1}$ is consistent with the escape velocity of Wolf-Rayet stars, making a late WN-to-WC star the most viable progenitor for SN 2020able.
  • The non-LTE radiative-transfer models of Dessart et al. (2022), built for low-mass helium stars in binaries, reproduce the narrow-line phase but fail to reproduce the broad features seen after about day 43, indicating that the late spectra come from the inner ejecta of a more massive stripped-envelope star.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the electron-scattering interpretation holds, the same conversion of constant FWHM to Thomson optical depth could be applied to other Type Ibn SNe with early high-ionization lines to map their pre-SN mass-loss histories, but only after kinematic broadening is excluded by higher-resolution spectra.
  • A single narrow-line spectrum of an interacting transient can mix light from shells ejected by different mechanisms; for objects like SN 2020able, the absence of ongoing interaction at late times means the narrow lines are a fossil record of the CSM, not evidence of current energy input.
  • Archival limits rule out a pre-explosion outburst brighter than about $M_{\rm bol}=-14$ in the two years before the explosion, so the inferred eruption was either fainter than that or produced a shell that only became visible after the SN exploded; deeper pre-explosion monitoring of nearby Ibn candidates could test whether such $\sim0.02\,M_\odot$ eruptions are common.
  • The slow rise and slow decline of SN 2020able, compared with faster Ibn SNe, may indicate that its early excess came from a dense inner shell rather than an extended wind; this stratification could be the reason the rise-time/decline-rate plane of Type Ibn SNe is so spread out.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper presents a comprehensive spectrophotometric dataset for the Type Ibn SN 2020able, from to 7 to 98 days after explosion, and uses it to argue that the transient's environment is stratified into three distinct regions: an inner shocked shell traced by the early light-curve excess and MOSFiT modelling (M_CSM ~ 0.6 Msun, R_out ~ 3.1e13 cm), a dense un-shocked He-rich shell at R ~ 9.3e14 cm with n_e ~ 1.4e9 cm^-3 and mass ~ 0.02 Msun, and a more extended outer shell at R ~ 2.2e15 - 3.3e15 cm expanding at ~ 1.2e3 km/s. The paper concludes that the inner un-shocked shell was produced by a discrete pre-SN eruptive event similar to SN 2006jc, while the outer shell is consistent with a late WN/WC Wolf-Rayet wind. The analysis combines light-curve fitting with MOSFiT, SED blackbody fits, line-profile fitting of the high-ionisation features, and EW evolution of the narrow He I absorptions, in comparison with a sample of Type Ibn/Icn supernovae.

Significance. If the conclusions hold, SN 2020able is one of the best-documented cases of a stratified CSM in a Type Ibn SN, with early high-cadence data that directly constrain the geometry and mass-loss history of the progenitor. The paper is commendable for its transparent handling of model degeneracies, its release of light curves and posterior distributions via Zenodo, and its explicit discussion of alternative interpretations. The central stratification picture has independent qualitative support from the constant FWHM of the high-ionisation lines, the EW drop timing, and the P Cygni velocities, which are observables rather than outputs of the light-curve fit. However, the quantitative claim of a discrete eruptive event with a specific mass and mass-loss rate rests on a single, insufficiently tested assumption about the line-broadening mechanism, so the significance of the strongest conclusion is currently not established.

major comments (3)
  1. [Section 2.3] The conversion of the constant FWHM of about 3e3 km/s into a Thomson optical depth tau_es ~ 6.5 is the linchpin of the eruptive-CSM claim, but the paper does not convincingly exclude kinematic broadening. The He I P Cygni absorption minima at about 1.2e3 km/s and the BVZI at about 1.8e3 km/s provide a natural kinematic scale: a shell or wind with velocities up to ~1.8e3 km/s can produce an emission FWHM of ~3e3 km/s with tau_es << 1. The paper's cited arguments for electron scattering - the symmetry of the profiles and the FWHM-to-absorption ratio (paragraph beginning 'A more stringent constraint for the local density') - are not discriminating tests, since Huang & Chevalier (2018) show that a range of optical depths and kinematic configurations can produce symmetric profiles. This assumption is load-bearing because the derived n_e ~ 1.4e9 cm^-3, M_dense ~ 0.02 Msun, and M_dot ~ 0.7 Msun/yr, and hence the conclusion that a steady WR wind is ruled out (Abstract; Section 3), all follow from it. I request a direct test separating the two mechanisms, such as a quantitative comparison of the full observed line profiles with Huang & Chevalier (2018) models under both the high-tau and low-tau kinematic interpretations, or an independent density estimate from recombination/forbidden line ratios. Until this is provided, the eruptive-episode conclusion should be presented as one of two plausible interpretations rather than a demonstrated result.
  2. [Section 2.3 (paragraph beginning 'The geometric extent of the shell')] The shell radii used in the mass estimate are not uniquely determined. The paper derives R_in ~ 2.2e15 cm and R_out ~ 3.3e15 cm by associating the EW drop at about +47 d with the ejecta overtaking the shell's inner boundary and the disappearance at about +70 d with its outer boundary. However, the text itself immediately acknowledges that the absorption may instead be diluted in the blue wing of the emerging broad He I emission. If dilution is the cause, the EW timing does not measure the shell's physical extent, and the adopted thickness Delta_R ~ 1.3e15 cm - which enters the density n_e = tau_es/(sigma_T Delta_R) and thus the mass M_dense ~ 0.02 Msun - is not robust. I ask the authors to model the dilution scenario and quantify how the inferred radii, density, and mass change, or to provide an independent geometric constraint that does not rely on the EW drop interpretation.
  3. [Section 2.2, Table C.2 and Figs. C.2/C.3] The claim that the early interaction is geometrically and temporally confined (Abstract; Section 3) rests on the MOSFiT csmni result that the shocked shell's outer radius is R_out ~ 3.1e13 cm. The text acknowledges that R0 and rho_CSM have broad, strongly covariant posteriors spanning more than an order of magnitude, and the corner plots show non-Gaussian distributions. The quoted R_out is computed from the posterior medians without propagating the full covariance, and the alternative pure-csm model, though disfavored by the authors, places the shell at R0 ~ 35.5 AU with low density. To make the confinement claim quantitative, I request a demonstration that the derived R_out is robust to the degeneracies (e.g., by computing R_out over the full posterior and showing its distribution), or a revision of the claim to explicitly state that it is model-dependent.
minor comments (4)
  1. [Figure 3 caption] The caption reads 'at 2 fit' and 't 2 evolution'; these should be 't^2 fit' and 't^2 evolution' for the power-law fit, and the meaning of 'at 2' is unclear.
  2. [Section 2.3] The electron density for the dense inner shell is quoted as n_e ~ 1.4e9 cm^-3 in the paragraph following 'Taking tau_es = 6.5' and as n_e ~ 7.5e8 cm^-3 in the next paragraph; please clarify which definition (Delta_R = 3.1e13 cm from the first estimate versus Delta_R ~ 1.3e15 cm from the EW-determined thickness) corresponds to each value and keep the notation consistent.
  3. [Section 2.3 and Figure 9] The text says the multi-component fits adopt Lorentzian profiles to follow the electron-scattering wings, but the caption of Figure 9 states that a Gaussian absorption was used to reproduce the overall profile of He I 5876; please state the actual profile choices explicitly and consistently.
  4. [Section 2.3] The relation between FWHM and tau_es is cited to Figure 5 of Huang & Chevalier (2018), but the paper does not reproduce the relation or give the exact formula used; since the tau_es = 6.5 value is central, please include the relevant curve or equation in an appendix.

Circularity Check

1 steps flagged · score 3.0 of 10

Only minor circularity: the constant-FWHM fit is used to rule out FWHM evolution; the central stratified-CSM/eruptive-shell result is not circular.

  1. fitted input called prediction [Section 2.3, paragraphs around Fig. 9 and the following paragraph on the constant FWHM]
    "the overall profiles are well-reproduced assuming a constant FWHM of approximately≃3×10 3 km s−1 at all times, leaving only the peak wavelengths and line fluxes as free parameters. ... A compact, nearby shell being swept up by the rapidly expanding SN ejecta would have introduced a shocked component, thus modifying the FWHM within the first 16 days, which is ruled out by our fitting procedure."

    The constancy of the FWHM is an input to the fit: the fit is performed 'assuming a constant FWHM ... at all times'. The paper then presents the absence of FWHM evolution as a result ('ruled out by our fitting procedure') that excludes a shocked, swept-up component. A constant-FWHM fit cannot by itself rule out a model with time-varying FWHM; that would require fitting and rejecting the varying-FWHM alternative. The same constancy is visible in Fig. 9 and therefore has independent observational support, so the circularity is partial and mostly in the wording.

full rationale

The paper's central conclusion—that SN 2020able exploded inside a stratified CSM with a compact shocked shell, a dense inner unshocked shell at R≳9.3×10^14 cm, and an outer shell at ~2.2–3.3×10^15 cm, with the inner shell produced by an SN 2006jc-like eruption—is not a circular derivation. The dense-shell density and mass are obtained by applying the external Huang & Chevalier (2018) electron-scattering relation to the observed constant FWHM ≈ 3000 km/s and to radii derived from P Cygni velocities and the EW drop/disappearance times. That mapping is model-dependent (geometry, T_e, filling factor), but it is not equivalent to the conclusion by construction: the FWHM is an observed quantity, and the τ_es → n_e → M_dense → Mdot chain is a forward calculation with stated assumptions. An alternative kinematic-broadening interpretation would lower the derived mass and mass-loss rate, but that is a physical modeling degeneracy, not a circularity. The self-citations (Tartaglia et al. 2020, 2025) are used for line-formation mechanism and profile shape and are not the load-bearing step. The one genuine circular element is in Sect. 2.3: the multi-component fit is performed 'assuming a constant FWHM', and the paper then says a swept-up shocked component 'modifying the FWHM within the first 16 days' is 'ruled out by our fitting procedure'. The assumed constancy is being used as evidence against FWHM evolution. Because the constancy is also directly visible in Fig. 9, this does not invalidate the central result, but the sentence as written is a fitted input presented as a conclusion. Overall: partial, minor circularity in presentation; central claims remain independent of any fitted parameter or self-citation chain.

Assumptions & free parameters 13 free parameters · 6 assumptions · 0 invented entities

The paper's central scenario rests on the MOSFiT light-curve fit (several correlated free parameters) combined with a model-dependent electron-scattering interpretation of the line profiles and a single, acknowledged interpretation of the EW drop. No new physical entities are postulated. The eruptive event is inferred, not directly observed, since archival non-detections rule out outbursts brighter than about -14 mag in the two years before explosion.

free parameters (13)
  • M_ej (MOSFiT csmni) = 1.315 (+0.062, -0.068) Msun
    Fitted to the UV/optical light curves with MOSFiT; drives the post-peak decline.
  • E_k (MOSFiT csmni) = 2.9e50 erg (log10 Ek = 0.077)
    Fitted ejecta kinetic energy.
  • M_CSM (MOSFiT csmni) = 0.573 (+0.013, -0.014) Msun
    Fitted interacting shell mass; a key input for the compact interaction region claim.
  • R0 (MOSFiT csmni) = 0.25 AU (16-84%: 0.1-0.6 AU)
    Inner radius of the interacting shell; posterior spans about an order of magnitude, and the compactness claim rests on the model choice.
  • rho_CSM (MOSFiT csmni) = 9.3e-9 g cm^-3 (posterior spans roughly 2 dex)
    Fitted CSM density; used with M_CSM to infer the shell outer radius.
  • M_Ni56 (MOSFiT csmni) = 0.0315 (+0.0043, -0.0038) Msun
    Fitted nickel mass; needed in addition to interaction to reproduce the light curve.
  • n (ejecta density profile index) = 6.6 (prior 6-10)
    Fitted outer ejecta density profile index; deviation from n = 10 is justified by violent pre-explosion mass loss.
  • T_min (temperature floor) = 7499 K
    Fitted temperature floor, near the helium recombination temperature.
  • A_V (host extinction) = 0.147 mag
    Fitted line-of-sight extinction; consistent with Na I D equivalent widths.
  • Explosion epoch = JD 2459184.46 +/- 0.43
    Adopted midpoint between last non-detection and first detection; sets all phases.
  • Filling factor f for CSM clumping = 0.1 (assumed)
    Assumed to convert electron-scattering column to mass; central to the dense-shell mass estimate of about 0.02 Msun.
  • Radiative efficiency epsilon = about 30% (assumed; 26% upper limit from archival limits)
    Used to estimate the interaction luminosity at +16 days and the 2-3% contribution to Lbol.
  • Electron temperature T_e = 2.0e4 K (assumed)
    Adopted for the He recombination coefficient and the Huang & Chevalier FWHM-to-tau_es mapping.
assumptions (6)
  • domain assumption The MOSFiT csmni analytical model describes the light curve.
    The interpretation of the early peak as ejecta-CSM interaction plus 56Ni decay relies on this model (Villar et al. 2017; Chatzopoulos et al. 2013), with the native limitation s <= 2 motivating the wind profile.
  • domain assumption Line broadening is dominated by electron scattering in the dense shell.
    The FWHM-to-tau_es conversion follows Huang & Chevalier (2018) for an expanding, scattering shell; if kinematic broadening contributes, the derived density and mass are not valid.
  • domain assumption The EW drop at +47 days marks the ejecta overtaking the shell.
    The authors use this to derive R_in = 2.2e15 cm and R_out = 3.3e15 cm, but also note that the absorption could be diluted by emerging broad He I emission (Section 2.3).
  • domain assumption The Galbany et al. (2016) metallicity gradient applies to this host galaxy.
    The host abundance at the SN position (8.28 dex) is extrapolated from the central value using a statistical gradient for SN Ib/c hosts.
  • standard math Standard cosmology with H0 = 73 km/s/Mpc.
    Adopted for luminosity distance; matches the SN Ibn comparison literature.
  • domain assumption Na I D equivalent width to reddening relation (Poznanski et al. 2012).
    Used to estimate the host extinction contribution from resolved Na I D features.

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Cite this review

Pith. "Pith review of Wild behaviour near the finish line: the Type Ibn SN 2020able and its stratified environment." pith.science (2026). https://pith.science/paper/YYCLC6AM

@misc{pith2026260807661,
  author       = {Pith},
  title        = {Pith review of: Wild behaviour near the finish line: the Type Ibn SN 2020able and its stratified environment},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YYCLC6AM}},
  note         = {Machine review of arXiv:2608.07661}
}
abstract

We present spectrophotometric observations of the Type Ibn supernova SN~2020able, along with a comprehensive analysis and modelling of its evolution. The transient occurred in SDSS J092602.93+243115.1, a faint host galaxy characterised by significantly sub-solar metallicity ($12+\log(\rm{O/H})\simeq8.28\,\rm{dex}$). The early photometric evolution and high peak luminosity ($L_{peak}\simeq4.4\times10^{43}\,\rm{erg}\,\rm{s^{-1}}$) indicate an efficient conversion of ejecta kinetic energy into radiation via interaction with the circumstellar medium. Light-curve modelling suggests that this interaction involves ejecta with a mass of $M_{\rm{ej}}\simeq1.3\,M_{\odot}$ impacting a shell of $M_{\rm{CSM}}\simeq0.6\,M_{\odot}$. However, interaction is found to be geometrically and temporally confined within a few days after explosion, with the later evolution of the transient being dominated by the free expansion of the ejecta. Spectroscopic analysis reveals a complex, stratified circumstellar environment. In addition to the innermost shocked region, we identify two additional He-rich shells: a dense inner one ($n_{\rm{e}}\simeq1.4\times10^{9}\,\rm{cm^{-3}}$) located at $R\gtrsim9.3\times10^{14}\,\rm{cm}$, and a more extended outer component reaching $R_{out}\simeq3.3\times10^{15}\,\rm{cm}$ and expanding at approximately $1.2\times10^3\,\rm{km}\,\rm{s^{-1}}$. The physical parameters of the former suggest it was produced by a discrete pre-supernova eruptive event similar to that of SN~2006jc, which expelled approximately $1.8\times10^{-2}\,M_{\odot}$ of material. Conversely, the expansion velocity of the outermost shell is consistent with the escape velocity of WR stars, pointing towards a late WN to WC-type progenitor as the most viable candidate for SN~2020able.

Figures

Figures reproduced from arXiv: 2608.07661 by the authors.

Figure 1
Figure 1. Colour image of SN 2020able and its host galaxy, obtained com￾bining g−, r− and i−band data obtained on 2021 January 21 with the 2.0 m Liverpool Telescope. The transient is the bright source in the mid￾dle of the inset. nario, the ejecta collide with a massive, He-rich CSM shell pre￾viously ejected through binary interaction or a non-terminal nu￾clear flash. Notably, their simulations show that the late-time spectra… view at source ↗
Figure 3
Figure 3. Early evolution of the gri light curves of SN 2020able and the R−band light curve of SN 2010al, along with a t 2 fit to the derived fluxes. To highlight the early excess, we also show the best fit obtained removing the first one/two points. When extrapolating the flux to zero, both yield explosion dates that occur after the SN discovery (reported using open squares and diamonds). available soon after discovery, conf… view at source ↗
Figure 5
Figure 5. Decline rates vs. rise times for the sample of [PITH_FULL_IMAGE:figures/full_fig_p004_5.png] view at source ↗
Figures from the paper (6 more)
Figure 6
Figure 6. Figure 6: Multi-band light curves of SNe 2020able and 2010al along with an ensemble of models generated by MOSFiT. Light curves have been vertically displaced by the indicated offsets. Rest-frame phases refer to the estimated explosion epoch. He i lines at +98 days, and NH = 3.1…
Figure 7
Figure 7. Figure 7: Evolution of the photospheric radius and the bolometric lumi￾nosity as derived by fitting a blackbody to the SED of SN 2020able. Rest-frame phases refer to the estimated explosion epoch. action scenario. In this framework, interaction contributes to the transient lumin…
Figure 8
Figure 8. Figure 8: Early spectroscopic evolution of SN 2020able at t < +16 days along with a line identification of the main emission features. He i lines are reported with their corresponding rest wavelengths. The ⊕ symbol marks the position of the O2 telluric feature (Band A) around 75…
Figure 9
Figure 9. Figure 9: Left: Multi-component fit to the N iii+He ii and Ciii+He i regions. A Gaussian absorption was used to reproduce the overall profile of He i λ5876. The widths and peaks of the features remain constant throughout the evolution of the high-ionisation feature, with a FWHMv…
Figure 10
Figure 10. Figure 10: Left: Spectroscopic evolution of SN 2020able at t > +17 days. Middle: Zoom-in around He i λ5876 showing the evolution of its narrow absorption feature. Right (top): Evolution of the EW of the He i λ5876 narrow absorption showing a sudden drop at t ≳ +47 days. Right (b…
Figure 11
Figure 11. Figure 11: Comparison of optical spectra of SN 2020able with non-LTE radiative-transfer models from Dessart et al. (2022). Spectra were nor￾malised to their flux at 5500 Å. v ≃ 1.2 × 103 km s−1 , derived from the P Cygni minima of He i and N iii λ4100, is typical of steady winds…

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Reviewed August 11, 2026 · model on record in the stance chip above.