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REVIEW 3 major objections 4 minor 109 references

SN 2022erq's extraordinary luminosity and slow decline are powered by ejecta–CSM interaction, not radioactive decay, and its progenitor's mass-loss rate escalated from about 0.04 to 0.6 solar masses per year in the final decades before expl

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The superluminous Type Ia supernova SN 2022erq was powered by ejecta crashing into a ~3-solar-mass circumstellar shell, implying the progenitor's mass-loss rate escalated from ~0.04 to ~0.6 solar masses per year in its final decades.

T0 review reviewed 2026-08-02 challenge →

load-bearing objection SN 2022erq is the earliest confirmed Ia-CSM with dense multi-band data to 1350 d; the central interaction-powered claim is solid, but the headline 0.04→0.6 M_sun/yr escalation rests on bolometric inversion assumptions that need systematic sensitivity tests. the 3 major comments →

arxiv 2607.06338 v3 pith:TA6TZGYU submitted 2026-07-07 astro-ph.HE

SN 2022erq: A Superluminous Thermonuclear Supernova with Escalating Preexplosion Mass Loss

Qian Zhai , Jujia Zhang , Xiaofeng Wang , A. Pastorello , Alexei V. Filippenko , J\'ozsef Vink\'o , Thomas G. Brink , Yunkun Han
show 46 more authors
G. Valerin N. Elias Rosa Yongzhi Cai Weili Lin Yi Yang WeiKang Zheng Xiangcun Meng Chengyuan Wu Liping Li Zeyi Zhao J. Craig Wheeler Jose L. Prieto Jialian Liu Gaici Li Shengyu Yan Fangzhou Guo C. P. Guti\'errez E. Kankare Peter Lundqvist S. Moran A. Reguitti I. Salmaso M. D. Stritzinger S. Williams J.-W. Zhao D.-D Shi Jianrong Shi Z.-H. Peng Tengfei Song Yongyuan Xiang Attila B\'odi Borb\'ala Cseh \'Agoston Horti-D\'avid Csilla Kalup Levente Kriskovics R\'eka K\"onyves-T\'oth Andr\'as P\'al B\'alint Seli \'Ad\'am S\'odor R\'obert Szak\'ats P. A. Mazzali T. Kravtsov K. Matilainen T. M. Reynolds L. Galbany Bo Wang
This is my paper
classification astro-ph.HE
keywords supernovaeType Ia supernovaecircumstellar mediummass losssuperluminous supernovaeH-alpha emissionwhite dwarf progenitorslight curves
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The reading

This paper reports on SN 2022erq, a thermonuclear supernova whose peak luminosity is roughly ten times that of a normal Type Ia. It argues that this extreme brightness does not come from radioactive nickel but from the shock wave of the explosion converting kinetic energy into light as it plows through a dense hydrogen-rich shell of circumstellar material. By combining the strength of narrow hydrogen emission with the evolution of the bolometric light curve, the authors reconstruct the pre-explosion mass-loss history: the mass-loss rate rose from about 0.04 to about 0.6 solar masses per year over the final decades, building a shell of about 3 solar masses extending to about 3.5×10^16 cm. This matters because it directly implicates a white dwarf with a nondegenerate companion as the progenitor and shows that some of the brightest thermonuclear supernovae owe their luminosity to environment rather than to an unusually powerful explosion.

Core claim

The central claim is that SN 2022erq is an Ia-CSM event, a thermonuclear supernova interacting with hydrogen-rich circumstellar material, and that its light curve is dominated by long-lived ejecta–circumstellar interaction rather than radioactive decay. Applying the standard peak-luminosity–nickel-mass relation would require an implausible nickel mass of about 6 solar masses, ruling out radioactive decay as the power source. Instead, the authors model the post-peak decline as the shock's kinetic energy being converted into radiation with roughly 50 percent efficiency. Inverting the bolometric light curve yields a circumstellar density profile that steeply declines with radius (ρ ∝ r^{-3.7}),

What carries the argument

The central device is the inversion of the bolometric light curve, L = ε dEkin/dt = 2πε ρ(r) r² v³, which converts the observed luminosity into a circumstellar density profile. The shock velocity is taken from the width of the broad Hα component, parameterized as v_sh ∝ t^{0.15}, and the kinetic-to-radiative efficiency ε is set to about 50 percent, consistent with the ratio of radiated energy to the canonical ejecta kinetic energy of about 1.4 foe. Independent density estimates come from the narrow Hα flux, which probes the outer, unshocked wind. The steep power-law density profile (index ~3.6) is then translated into a mass-loss history by assuming a constant wind speed of 180 km/s, so that

Load-bearing premise

The reconstruction of the mass-loss history rests on assuming that the circumstellar wind had a constant speed of 180 km/s and was spherically symmetric; if the wind velocity evolved with time or the shell is clumpy or asymmetric, the derived escalation and total mass could change substantially.

What would settle it

A direct measurement of the circumstellar density profile, for example from late-time radio or X-ray emission of the shock, would test the claim: if that profile does not match the steep ρ ∝ r^{-3.7} power law inferred from the bolometric light curve, the escalating-path-to-explosion interpretation would be wrong. Alternatively, detecting resolved absorption features from the wind at multiple epochs could reveal whether the wind speed was constant.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

If this is right

  • If true, the brightest Type Ia-like supernovae can be powered mainly by circumstellar interaction, so luminosity-based cosmological calibrations must account for such contamination.
  • The derived mass-loss escalation of about a factor of 15 over decades places strong constraints on binary evolution models, favoring a brief, violent ejection episode shortly before explosion.
  • The young host environment (about 100 Myr) and the massive shell point to a white dwarf with an intermediate-mass companion, a channel that current population synthesis may underestimate.
  • The event demonstrates that early spectroscopic classification (within days) can identify Ia-CSM events, so future wide-field surveys should find more such objects.
  • The success of this analytic inversion suggests that bolometric light curves of interacting supernovae can be used to reconstruct progenitor mass-loss histories.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the wind speed varied with time, the absolute timing of the mass-loss escalation would shift, so the 0.04→0.6 M_sun/yr history is model-dependent; a direct measurement of velocity stratification could resolve this.
  • The steep density profile could also be produced by an asymmetric or clumpy shell, which would change the mass estimate; polarimetric observations during the interaction phase could test sphericity.
  • The same inversion method could be applied to other Ia-CSM events to see whether escalating mass loss is common or unique to this event.
  • If the underlying explosion is super-Chandrasekhar, the assumed ejecta kinetic energy and efficiency would change, which would alter the absolute density scale.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. SN 2022erq is presented as the earliest spectroscopically confirmed Type Ia-CSM supernova, discovered about 1.8 days after explosion and followed for about 1350 days. From multi-band photometry and spectroscopy the authors derive a peak bolometric luminosity of about 8e43 erg/s, an unusually slow post-peak decline, and an IGE-rich/IME-weak spectrum with persistent narrow H-alpha. They argue that Arnett's law would require roughly 6 Msun of 56Ni, ruling out radioactive decay as the dominant power source, and that ejecta-CSM interaction supplies most of the luminosity. Using the Ofek et al. (2013) narrow-H-alpha formula they infer a wind velocity of about 180 km/s and a mass-loss rate near 0.04 Msun/yr; inverting the bolometric light curve they derive rho proportional to r^-3.66, which they translate into an escalating mass-loss rate reaching about 0.6 Msun/yr in the final years and a total CSM mass of about 3 Msun. They conclude that the progenitor is a white dwarf with an intermediate-mass companion that underwent escalating late-stage mass loss.

Significance. If the quantitative reconstruction holds, the paper is a valuable addition to the rare Ia-CSM class: it has the earliest spectra, dense photometry, a clean host environment, and one of the few attempts to reconstruct a pre-explosion mass-loss history for this class. The central claim that CSM interaction, not 56Ni decay, dominates the luminosity is well supported by three independent observational arguments: the Arnett-limit inconsistency, the persistent narrow Balmer lines, and the slow post-peak decline. The extensive dataset and the machine-readable tables and spectra are concrete assets. The quantitative mass-loss history is the least secure part because it depends on a single-zone inversion with several hand-tuned parameters, and the H-alpha data do not independently corroborate the steep density profile as presented. This weakness does not undermine the classification or the interaction-dominance claim, but it does affect the headline 'escalating mass loss' result.

major comments (3)
  1. [Sections 5.2 and 5.3] The claimed 'broad consistency' between the H-alpha and bolometric diagnostics is not supported when the H-alpha emission is referred to the instantaneous shock radius. The Ofek et al. formula used in Section 5.2 is the recombination luminosity of a wind outside an inner radius r; for a local mass-loss rate Mdot_eff = 4 pi r^2 rho v_wind it gives L_Halpha proportional to Mdot_eff^2 / (r v_wind^2). At tau about 77 d, the adopted v_sh(t) = 2800 t^0.15 gives r_sh about 3e15 cm, so the H-alpha point at this epoch measures Mdot_eff about 0.04 Msun/yr at that radius, i.e. rho about 1.2e-14 g/cm3. The bolometric profile rho proportional to r^-3.66 normalized to the quoted inner value (about 0.6 Msun/yr near 1.5e15 cm) implies Mdot_eff proportional to r^-1.66 and predicts Mdot_eff(3e15 cm) about 0.1-0.2 Msun/yr, a factor 3-5 above the H-alpha value. Moreover, the two H-alpha epochs (4.5e-2 and 3
  2. [Section 5.3] The derivation of s = 3.59 from the post-peak slope alpha = -1.46 is called an 'independent check,' but it is not independent: both quantities are derived from the same bolometric light curve, and the Moriya et al. (2013) relation is an analytic approximation of the same inversion with an assumed ejecta index n about 10. It verifies only internal consistency of the power-law model. In addition, the inversion of Eq. (2) assumes a single, time-independent epsilon = 0.5. That value is calibrated from the total radiated energy divided by a canonical 1.4 foe, but the instantaneous conversion efficiency is not measured; the two-epoch v_sh(t) parameterization and the 40-330 d phase boundaries are also unquantified inputs. The resulting 0.04 to 0.6 Msun/yr escalation therefore has no formal error budget. The authors should either propagate these systematic uncertainties or present the mass-loss
  3. [Sections 5.2 and 5.3] The total CSM mass and outer radius are derived with two different velocity assumptions. The H-alpha mass of about 2.4 Msun assumes a constant 180 km/s wind over about 60 yr, while the bolometric mass of about 3 Msun comes from the r^-3.66 profile; the near-agreement of the two numbers is therefore not an independent confirmation. Also, the outer CSM radius of about 3.5e16 cm is obtained from an 'ejecta velocity' of 10,000 km/s, whereas the CDS velocities used in Section 5.3 are 5,400-5,900 km/s; the latter gives r about 2e16 cm over 400 d, closer to the 1.6e16 cm bolometric extent. A single, clearly defined interaction radius should be used consistently in both diagnostics.
minor comments (4)
  1. [Section 5.2] The parameter beta in the Ofek et al. formula is not defined; please state its assumed value or give the reference for the adopted normalization.
  2. [Figure 13] Please specify the phase range over which the L proportional to t^-1.46 fit is performed; 'post-peak' is ambiguous for a light curve with such a long, nearly flat evolution.
  3. [Section 5.1] The SED-derived stellar metallicity log(Z/Zsun) = -2.13 (about 0.7% solar) is remarkably low, far below the gas-phase R23 value; a sentence discussing whether this result is robust to the BayeSED prior choices would be helpful.
  4. [Section 2.3] Minor typographical issues: 'NaiD' should read 'Na I D'; in Section 4.1, 'overlay Hbeta and Hgamma absorption' would read more clearly as 'overlaid by Hbeta and Hgamma absorption.'

Circularity Check

1 steps flagged

Mild circularity in the 'independent check' of the density slope: it reuses the same bolometric light curve; the main mass-loss reconstruction is otherwise a disclosed model inversion.

specific steps
  1. fitted input called prediction [Section 5.3, after Eq. (2) inversion, paragraph 'A power-law fit to these numerical results...']
    "As an independent check, we fit the post-peak bolometric luminosity with L∝t^α, obtaining α=−1.46. Using the analytic model of T. J. Moriya et al. (2013)... we derive s=3.59, corresponding to ρ_CSM ∝ r^{−3.59}, in good agreement with the numerical result."

    The 'numerical result' s=3.66 is obtained by inverting Eq. (2) with the same observed bolometric L(t), v_sh(t), and r_sh(t). The 'independent check' fits a power law to the same post-peak L(t) and converts that fitted α into s via the Moriya et al. scaling relation. Both routes use the same light curve as input under the same interaction model, so the agreement is a self-consistency test rather than an independent confirmation. It cannot independently validate the steep density slope or the derived escalation of the mass-loss rate.

full rationale

The central mass-loss reconstruction is a model inversion rather than a circular derivation: Eq. (2) combines an assumed kinetic-to-radiative efficiency ε≈50%, a shock-velocity parameterization v_sh(t)=v1 t^0.15 calibrated from two measured broad-Hα FWHMs, and the observed bolometric L(t) to infer ρ_CSM(r); the Mdot history then follows from the stated steady-wind assumption v_wind=180 km/s with an explicit caveat that a time-varying wind would change the absolute timing. The Hα narrow-line flux is an independent observable and is not used to set the bolometric density normalization. No load-bearing self-citation or uniqueness argument is present. The only notable circular element is the 'independent check' in Section 5.3: the analytic s=3.59 is derived from a power-law fit to the same post-peak bolometric light curve that produced the numerical density profile, so the agreement adds no new evidence. This is a minor overstatement, not a central circularity; the headline escalation could stand or fall on the bolometric inversion alone.

Axiom & Free-Parameter Ledger

5 free parameters · 7 axioms · 0 invented entities

The central claim depends mostly on standard astrophysical machinery (shock interaction, recombination lines, SED fitting) rather than new entities. The main free parameters are the conversion efficiency ε, the assumed constant wind velocity, the shock-velocity parameterization, and the interaction-phase boundaries. These are reasonable but not independently calibrated, and no systematic uncertainties are propagated into the quoted CSM mass and mass-loss rates.

free parameters (5)
  • ε (kinetic-to-radiative conversion efficiency) = 0.5
    Section 5.3: total radiated energy ~0.7 foe divided by assumed 1.4 foe ejecta kinetic energy. Directly scales the inferred CSM density and mass.
  • v_wind = 180 km/s
    Measured from H-alpha P-Cygni absorption minimum (Section 5.2), but assumed constant over the entire decades-long mass-loss history; used to convert radius to pre-explosion time and to convert density to mass-loss rate.
  • v_sh(t) parameterization = v1=2800 km/s, exponent 0.15
    Section 5.3: fitted to the broad H-alpha component FWHM at only two epochs (τ≈77 and 147 d), then integrated to obtain r_sh(t). A different deceleration law changes the density profile.
  • Interaction phase boundaries = τ≈40 d to τ≈330 d
    Section 5.3: chosen as 'when the luminosity has passed its peak' and 'when the shock reaches the inner ejecta' (rapid decline). Changing these endpoints changes the integrated CSM mass.
  • Host SED stellar-population age = log(t_age/yr)=8.02
    Section 5.1: BayeSED fit to Pan-STARRS photometry; supports the young-environment claim but depends on assumed SFH, IMF, dust law, and nebular emission model.
axioms (7)
  • domain assumption CSM is spherically symmetric for mass estimates.
    Section 5.2 notes 'for a spherical geometry (or less if the CSM is aspherical or clumpy)'; Section 5.3 uses spherical integration to obtain 3 M_sun.
  • domain assumption Forward-shock kinetic energy dissipation is the sole power source with constant efficiency ε.
    Equation (2) in Section 5.3 assumes L = ε dEkin/dt with constant ε; radioactive input and reverse-shock contributions are neglected.
  • domain assumption Ejecta follow a standard Chandrasekhar-mass SN Ia density profile with n≈10 and total kinetic energy 1.4 foe.
    Section 5.3 adopts M_ej~1.4 M_sun, v~10^4 km/s, and n≃10 from Matzner & McKee 1999 and Kasen 2010; used for the analytic s–α relation and the ε calibration.
  • domain assumption The narrow H-alpha luminosity follows the Ofek et al. (2013) recombination relation for a steady wind with constant velocity.
    Section 5.2 uses L_Hα ≈ 2×10^39 Mdot^2 ... to derive 0.04 M_sun/yr; assumes a wind-density profile and recombination-dominated emission.
  • domain assumption The CSM was produced by a steady wind with constant velocity, so pre-explosion time is t=r/v_wind and Mdot=4πr^2ρv_wind.
    Section 5.3–5.4: this is the link that converts the steep density profile into the 'escalating mass-loss' conclusion; the paper acknowledges the timescale caveat if wind speed varies.
  • domain assumption Host SED modeling assumptions (BC03 SSP, Chabrier IMF, exponentially declining SFH, Calzetti dust, nebular emission) are valid for the dwarf host.
    Section 5.1 uses BayeSED3 with these choices to derive age ~105 Myr, stellar metallicity ~0.7% solar, and A_V~0.046 mag.
  • domain assumption R23 index calibrations yield reliable gas-phase metallicity.
    Section 5.1: 12+log(O/H)=8.45±0.05 from the R23 index at τ≈488 d, used as evidence of subsolar gas metallicity.

reviewed 2026-08-02 · how reviews work

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Cite this review

Pith. "Pith review of SN 2022erq: A Superluminous Thermonuclear Supernova with Escalating Preexplosion Mass Loss." pith.science (2026). https://pith.science/paper/TA6TZGYU

@misc{pith2026260706338,
  author       = {Pith},
  title        = {Pith review of: SN 2022erq: A Superluminous Thermonuclear Supernova with Escalating Preexplosion Mass Loss},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/TA6TZGYU}},
  note         = {Machine review of arXiv:2607.06338}
}
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read the original abstract

We present a photometric and spectroscopic study of the superluminous Type Ia supernova SN 2022erq. Its early spectra, dominated by iron-group elements with weak intermediate-mass features, might indicate highly efficient nuclear burning, broadly similar to that inferred for some overluminous SNe Ia. The rapid emergence and persistence of narrow Balmer emission lines superposed on this iron-rich spectrum provide clear evidence of long-lived interaction with a hydrogen-rich circumstellar medium (CSM), establishing SN 2022erq as a member of the rare Ia-CSM class. SN 2022erq reached a peak bolometric luminosity of about 8 x 10^43 erg/s and exhibited an exceptionally slow post-peak decline, indicating that its light curve is dominated by long-duration ejecta-CSM interaction. By combining H-alpha diagnostics with bolometric light-curve modeling, we reconstruct the pre-explosion mass-loss history of the progenitor. The mass-loss rate escalated by one order of magnitude over the final decades, rising from about 0.04 to about 0.6 solar masses per year. This surge produced a massive, extended CSM shell of about 3 solar masses out to about 3.5 x 10^16 cm. The young stellar environment (about 100 Myr) together with this substantial, extensive CSM points to a progenitor system consisting of a white dwarf and an intermediate-mass companion that underwent increasing mass loss prior to explosion.

Figures

Figures reproduced from arXiv: 2607.06338 by \'Ad\'am S\'odor, \'Agoston Horti-D\'avid, Alexei V. Filippenko, Andr\'as P\'al, A. Pastorello, A. Reguitti, Attila B\'odi, B\'alint Seli, Borb\'ala Cseh, Bo Wang, Chengyuan Wu, C. P. Guti\'errez, Csilla Kalup, D.-D Shi, E. Kankare, Fangzhou Guo, Gaici Li, G. Valerin, I. Salmaso, J. Craig Wheeler, Jialian Liu, Jianrong Shi, Jose L. Prieto, J\'ozsef Vink\'o, Jujia Zhang, J.-W. Zhao, K. Matilainen, Levente Kriskovics, L. Galbany, Liping Li, M. D. Stritzinger, N. Elias Rosa, P. A. Mazzali, Peter Lundqvist, Qian Zhai, R\'eka K\"onyves-T\'oth, R\'obert Szak\'ats, Shengyu Yan, S. Moran, S. Williams, Tengfei Song, Thomas G. Brink, T. Kravtsov, T. M. Reynolds, Weikang Zheng, Weili Lin, Xiangcun Meng, Xiaofeng Wang, Yi Yang, Yongyuan Xiang, Yongzhi Cai, Yunkun Han, Zeyi Zhao, Z.-H. Peng.

Figure 1
Figure 1. Figure 1: Optical and NIR light curves of SN 2022erq. Dotted and dashed vertical lines mark the explosion epoch and the time of B- band maximum, respectively. The data presented in this work are supplemented with public photometry from ZTF and ATLAS. The early-time rise in the gri- bands is fitted with a power-law (fireball) model. In this work, we present SN 2022erq, a superlumi￾nous (Mr ≈ −21 mag) thermonuclear tr… view at source ↗
Figure 1
Figure 1. Figure 1: Optical and NIR light curves of SN 2022erq. Dotted and dashed vertical lines mark the explosion epoch and the time of B- band maximum, respectively. The data presented in this work are supplemented with public photometry from ZTF and ATLAS. The early-time rise in the gri- bands is fitted with a power-law (fireball) model. LAS discovery on March 11.59 in the same band, this provides an initial constraint on… view at source ↗
Figure 2
Figure 2. Figure 2: Spectral sequence of SN 2022erq. Epochs marked on the right side of each spectrum are relative to the adopted explosion date. Dashed and dotted lines mark the rest-frame wavelengths of features originating from the SN and the host galaxy, with identifications labeled above and below the spec￾trum, respectively. All spectra have been corrected for the host redshift and smoothed with bin sizes chosen accordi… view at source ↗
Figure 2
Figure 2. Figure 2: Spectral sequence of SN 2022erq. Epochs marked on the right side of each spectrum are relative to the adopted explosion date. Dashed and dotted lines mark the rest-frame wavelengths of features originating from the SN and the host galaxy, with identifications labeled above and below the spec￾trum, respectively. All spectra have been corrected for the host redshift and smoothed with bin sizes chosen accordi… view at source ↗
Figure 3
Figure 3. Figure 3: The B-, g-, and r/R-band light curves of SN 2022erq compared with representative events: SNe Ia-CSM (SNe 2005gj, 2018evt; G. Aldering et al. 2006; J. L. Prieto et al. 2007; Y. Yang et al. 2023; L. Wang et al. 2024), SC candidates (SNe 2007if, 2009dc; R. A. Scalzo et al. 2010; S. Taubenberger et al. 2011; M. Hicken et al. 2012; J. M. Silverman et al. 2012; B. E. Stahl et al. 2019), 91T-like SNe (SNe 1991T, … view at source ↗
Figure 4
Figure 4. Figure 4: Peak r/R-band luminosity (M r/R max ) vs. duration above half-maximum luminosity (T1/2) in the rest frame. The sample includes normal, 91T-like, SC candidate, and CSM-interaction SNe Ia from J. M. Silverman et al. (2013); Y. Sharma et al. (2023). emission from the shocked CSM, e.g., Hα emission, (Y. Sharma et al. 2023) [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The g−r color evolution of SN 2022erq compared to representative objects, including a sample of SNe Ia and Ia-CSM from Y. Sharma et al. (2023), as well as several other well-studied transients. All comparison objects have been corrected for reddening. observations precludes a precise constraint on the onset of its CSM-interaction phase. When re-observed from t ≳ +120 d onward, SN 2018evt exhibited a lumino… view at source ↗
Figure 6
Figure 6. Figure 6: Spectral comparison of SN 2022erq near max￾imum brightness with SNe Ia-CSM (SNe 2002ic, 2005gj, 2018evt), SC candidates (SNe 2007if, 2009dc), 91T-like (SNe 1991T, 2011hr), normal SN Ia SN 2011fe (J. T. Parrent et al. 2012), and SN IIn SN 2010jl (N. Smith et al. 2012). Thin dotted lines mark rest-frame wavelengths; thick lines indi￾cate features at a blueshift of 10,000 km s−1 . All spectra are dereddened. … view at source ↗
Figure 7
Figure 7. Figure 7: Spectral comparison of SN 2022erq with SNe 1991T, 2007if, and 2011hr. Luminosity scaling factors, where applied, are noted after the phase. Thin dotted lines indicate the rest-frame wavelengths of spectral lines, while thick lines show their positions at a blueshift of 10,000 km s−1 . 4000 5000 6000 7000 8000 9000 Rest-Frame Wavelength (Å) Log(L λ) + o ffset 22erq(31d) 22erq(36d) 22erq(64d) 22erq(71d) 22er… view at source ↗
Figure 8
Figure 8. Figure 8: SN 2022erq compared with SN Ia-CSM SNe 2002ic, 2005gj, and 2018evt, following the same matching procedure applied in [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 10
Figure 10. Figure 10: A comparison of the pre-explosion host-galaxy photometric SED, the SED-derived model spectrum of the stellar population, and the late-time spectrum of SN 2022erq at τ ≈ 488 d (continuum-corrected to match the host SED). Dashed lines mark rest-frame wavelengths of spectral lines. the local environment. Applying the R23 index (H. A. Kobulnicky & L. J. Kewley 2004), defined as ([O ii] λ3727 + [O iii] λλ4959,… view at source ↗
Figure 11
Figure 11. Figure 11: Multi-Gaussian fits to the Hα and Paα lines of SN 2022erq. The spectra with higher spectral resolution and S/N were selected to enable a robust decomposition of the line profiles. The instrumental FWHM is ∼ 210 km s−1 for the optical spectra and ∼ 150 km s−1 for the NIR spectrum. 2000 1000 0 1000 2000 3000 4000 5000 Velocity relative to He I 10830 (km s 1 ) N o r m a liz e d F + o ffs e t 13d 35d 88d 103d… view at source ↗
Figure 9
Figure 9. Figure 9: A phase-averaged spectrum of SN 2022erq at τ ≈ 126 d, constructed from adjacent optical and NIR obser￾vations, is compared with those of SNe 2018evt and 2010jl (T. Zhang et al. 2012; H. J. Borish et al. 2015). Dashed lines indicate the rest-frame wavelengths of the spectral lines. 4000 5000 6000 7000 8000 Rest-frame Wavelength (Å) L o g ( F ) H HH H H H [OII] [OIII] [SII] [NII] Ca II Ca II IRT Observed Spe… view at source ↗
Figure 12
Figure 12. Figure 12: Spectral features normalized and displayed in the velocity space at selected phases. The left panel shows the He I λ10, 830 and Paγ lines, while the right panel presents the Paα line. Vertical lines indicate velocities of 0 km s−1 (dashed) and −180 km s−1 (dash-dotted) relative to host galaxy. and Ca ii absorption. The prominent discrepancy lies in the strong gas emission lines (e.g., from O, S, N) presen… view at source ↗
Figure 13
Figure 13. Figure 13: shows the bolometric light curve of SN 2022erq, derived from blackbody fits to the observed SED spanning the u–K bands. Light curves in individ￾ual filters were interpolated onto a common time grid, and blackbody fits were performed only when at least four filters had detections; no extrapolation was applied to epochs with missing bands. The figure also shows quasi-bolometric luminosities from direct flux… view at source ↗
Figure 14
Figure 14. Figure 14: CSM density profile of SN 2022erq. Red stars show densities inferred from the bolometric light curve, with a power-law fit ρCSM ∝ r −s (black line). Black diamonds mark independent density estimates from the narrow Hα line flux. Coloured dash/dotted curves show steady-wind profiles ρ = M /˙ (4πr2 vwind) for different mass-loss rates, as￾suming a constant wind velocity vwind = 180 km s−1 . The top axis giv… view at source ↗
Figure 14
Figure 14. Figure 14: CSM density profile of SN 2022erq. Red stars show densities inferred from the bolometric light curve, with a power-law fit ρCSM ∝ r −s (black line). Black diamonds mark independent density estimates from the narrow Hα line flux. Coloured dash/dotted curves show steady-wind profiles ρ = M /˙ (4πr2 vwind) for different mass-loss rates, as￾suming a constant wind velocity vwind = 180 km s−1 . The top axis giv… view at source ↗

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Works this paper leans on

109 extracted references · 2 linked inside Pith

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This paper was first reviewed by deepseek-v4-flash on August 2, 2026.