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REVIEW 3 major objections 5 minor 83 references

Weak sodium absorption does not mean little dust: Type Ib SN 2024vjc is heavily reddened anyway.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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SN 2024vjc is substantially dust-attenuated (E(B-V)~0.45–0.8 mag) despite weak Na I D absorption that would imply only ~0.18 mag, a clear counterexample to that common diagnostic.

T0 review reviewed 2026-07-30 challenge →

load-bearing objection Solid multi-method case study of a Type Ib with high host reddening and weak Na I D; the counterexample is real enough to publish, but the “independent diagnostics” are more correlated than the abstract claims. the 3 major comments →

arxiv 2607.23690 v1 pith:RAJ6MKCB submitted 2026-07-26 astro-ph.HE

Dust Without Na I D Trace: The Case of Highly Attenuated Type Ib SN 2024vjc

Javier Silva-Farf\'an , Keiichi Maeda , Andrea Pastorello , Hanindyo Kuncarayakti , Takashi Nagao , Giorgio Valerin , Andrea Reguitti , Dino Pierluigi Fugazza
show 14 more authors
Giuliano Pignata Jesper Sollerman Chris Ashall Tom\'as E. M\"uller-Bravo Joseph P. Anderson Claudia P. Guti\'errez Priscila J. Pessi Erkki Kankare Niko Pyykkinen Mariusz Gromadzki Ting-Wan Chen Thomas M. Reynolds Irene Salmaso Avishay Gal-Yam
This is my paper
classification astro-ph.HE
keywords Type Ib supernovaestripped-envelope supernovaehost-galaxy attenuationNa I D absorptiondust extinctionBalmer decrementH II regionscore-collapse supernovae
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

Dust between us and a supernova changes how bright and how red it looks, so getting the dust right is essential before anyone can trust the explosion’s true energy or the local galaxy environment. A common shortcut is to treat weak or missing narrow sodium (Na I D) absorption as proof that host-galaxy dust is negligible. This paper follows Type Ib supernova SN 2024vjc for about 130 days and shows that shortcut fails here. Sodium barely appears, which by the usual calibration would imply only modest reddening, yet the light-curve colors, spectral shape relative to normal Type Ib events, blackbody temperature and radius checks, and the Balmer decrement from nearby ionized gas all point to substantial dust, roughly E(B−V) of 0.45 to 0.8 mag. Late spectra also reveal a young star-forming region at the site, offering a physical reason sodium can be ionized away while dust still dims the light. The case is offered as a concrete counterexample and a warning that attenuation for core-collapse events needs several independent checks, not sodium alone.

Core claim

SN 2024vjc is a normal-looking Type Ib supernova that suffers substantial host attenuation (E(B−V) ~ 0.45–0.8 mag from color templates, color-curve evolution, spectral dereddening, and the Balmer decrement) even though Na I D is weak or absent and the standard sodium calibration returns only ~0.18 mag. It is therefore a clear counterexample to the assumption that weak sodium means negligible host dust.

What carries the argument

Cross-check of independent attenuation estimators against Na I D equivalent width: SN color templates and 0–20 day color-curve excess, continuum matching by dereddening an early spectrum to a low-reddening Type Ib comparison, SuperBol blackbody temperature/radius consistency with helium line-forming radii, and the Hα/Hβ Balmer decrement from the underlying H II region, with late-time narrow lines and blue continuum excess supporting local photoionization of sodium.

Load-bearing premise

That SN 2024vjc is intrinsically an ordinary Type Ib, so its red colors and continuum are almost entirely dust rather than an unusually cool or peculiar explosion.

What would settle it

Show that after careful multi-method analysis SN 2024vjc remains intrinsically much cooler and fainter than normal Type Ib events even when dust is minimized, or obtain high-resolution spectra and environment maps proving there is little dust along the line of sight while sodium stays weak.

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

If this is right

  • Absence of Na I D in SESN spectra can no longer be read as automatic proof of low host reddening.
  • Intrinsic luminosities, nickel masses, and temperatures for stripped-envelope supernovae need multi-diagnostic dust corrections, not sodium alone.
  • Young H II regions near explosion sites can suppress neutral sodium while dust still attenuates the light.
  • A hidden tail of highly reddened SESNe may be under-counted if samples are filtered or corrected only with Na I D.
  • Balmer decrements and SN color/spectral methods can disagree with Na I D in a scale-dependent way that maps dust near the progenitor versus larger ISM scales.

Where Pith is reading between the lines

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

  • Routine classification pipelines that flag ‘low extinction’ from non-detections of Na I D may systematically misplace the faint, red end of the SESN luminosity function.
  • Photoionization of sodium in star-forming sites may be common enough that Na I D–E(B−V) relations calibrated on SNe Ia should be treated as upper limits on reliability for core-collapse events.
  • Spatially resolved IFU maps of sodium, calcium, and dust continuum at SESN sites would cleanly separate ionization from true dust-poor gas.
  • If the high-attenuation tail is real and missed, volumetric rates and binary-channel demographics for stripped-envelope supernovae need upward revision at the dusty end.
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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 / 5 minor

Summary. The manuscript presents multi-band optical/NIR photometry (ATLAS, REM, SPECULOOS, VST, EFOSC2) and 11 epochs of optical spectroscopy of the Type Ib SN 2024vjc, followed to ~130 days post-explosion. The central claim is that SN 2024vjc is heavily attenuated by host dust (E(B−V) ≈ 0.45–0.8 mag from SN color templates, color-curve evolution, spectral dereddening against SN 2012au, and the H II-region Balmer decrement), while showing only a marginal Na I D detection whose Poznanski et al. (2012) calibration yields E(B−V) ≈ 0.18 mag. The object thus constitutes a counterexample to the assumption that weak/absent Na I D implies negligible host attenuation. The authors propose that photoionization of neutral sodium by the radiation field of a young H II region at the explosion site — supported by narrow Hα, [N II], Hβ emission and a late-time blue continuum excess — explains the discrepancy. Consistency checks (photospheric vs. excitation temperature; blackbody radius vs. He line-forming radius) favor the high-attenuation interpretation over an intrinsically cool, faint SN.

Significance. If the result holds, this is a methodologically important cautionary case: it demonstrates in a single well-observed object that the Na I D EW diagnostic can fail badly for SESNe embedded in young H II regions, complementing the SNe Ia result of Phillips et al. (2013) and the population-level trend in Barbarino et al. (2021) and Gutiérrez et al. (2026). Strengths include a genuinely multi-facility, 130-day photometric/spectroscopic dataset; a set of physics-based cross-checks (excitation vs. blackbody temperature; photospheric vs. He line-forming radius) that do not depend on color templates; direct environmental evidence (narrow Hα/[N II]/Hβ, blue continuum excess) supporting the proposed photoionization mechanism; and a falsifiable population-level prediction (a hidden subpopulation of obscured SESNe) framed honestly as an open question. Data availability via WISeREP and machine-readable photometry is commendable. The work is unlikely to settle the frequency of such objects, but a documented counterexample is, as the authors argue, sufficient to retire the diagnostic's universal use.

major comments (3)
  1. [§5.1, Table 4] §5.1, Table 4: The three SN-based estimates (0.667±0.501, 0.57±0.09, 0.767+0.033/−0.032) share a single premise — that SN 2024vjc's intrinsic SED follows canonical SESN templates — so they are correlated measurements of one systematic, not three independent confirmations. This matters because the manuscript itself supplies reasons to doubt the premise: the unusually flat r−i evolution at 0–20 d (§5.1) and the high He I λ5876 velocities (§4.1). The headline range 0.45–0.8 mag and the abstract's claim of 'multiple, independent attenuation diagnostics' should be revised accordingly. A concrete fix: propagate the full scatter (not just the median) of the A_V^host=0 T18 subsample as a systematic floor on E(B−V) from the color methods, so the reader can see how much of the 0.5–0.8 range survives intrinsic-color diversity. The genuinely SN-independent anchors (Balmer decrement, T_exc vs T_BB, R
  2. [§5.1, Eq. (1), Fig. 13] §5.1, Eq. (1), Fig. 13: The spectral-dereddening estimate E(B−V)=0.767±0.033 carries a purely statistical uncertainty and relies on SN 2012au as the unreddened reference — an object the paper itself describes as more energetic, engine-powered, with larger blueshifts and line widths (§4, Milisavljevic et al. 2013). Since this is the highest estimate and sets the upper end of the quoted 0.45–0.8 mag range, robustness should be demonstrated by repeating the SSR analysis with at least one alternative reference (SN 2016bau is the obvious choice given the flattened-spectrum match in Fig. 8), or by assigning a systematic uncertainty estimated from the spread across references. The peak-normalization step (which removes the A_V constraint and leaves only the degeneracy ridge) should also be discussed as a limitation on the absolute scale.
  3. [§5.2, §6.1] §5.2 and §6.1: The 'counterexample' framing rests on adopting the Poznanski et al. (2012) calibration (E(B−V)=0.18), but the Turatto et al. (2003) branch applied to the same measured EW gives 0.444±0.044 — in agreement with the Balmer decrement and only ~1.5σ below the color-evolution value. The manuscript reports this but does not draw the consequence: the discrepancy is not simply 'Na I D underestimates the dust'; it is that no single EW–E(B−V) relation is consistent with all diagnostics simultaneously, and the anomalous D2/D1≈1 ratio (saturation or He I λ5876 contamination) means the EW itself is unreliable here. The strongest defensible version of the claim should be stated explicitly in §6.1 and the abstract, since a reader could otherwise conclude the counterexample evaporates under a defensible calibration choice.
minor comments (5)
  1. [§5.3] §5.3/Table 6: The Balmer decrement rests on a single faint Hβ line ((7.42±1.04)×10⁻¹⁹ erg s⁻¹ cm⁻²) plus assumed Case B. Please state the detection significance and the sensitivity of E(B−V)_Balmer to departures from Case B (e.g., collisional excitation in a low-density region), and reiterate that this sightline need not coincide with the SN's (the chance-projection caveat in §6.3 is welcome).
  2. [§5.4] §5.4/Table 5: The T_BB and R_BB<R_He checks assume a pure blackbody (unity dilution factor), which is approximate for SESN photospheres. A sentence quantifying how a realistic dilution factor (e.g., 0.7–0.9) would shift the no-extinction T_BB≈4100 K and the radius constraint would strengthen this argument.
  3. [§5.2] §5.2: Please clarify whether the marginal Na I D detection at 6.25 Å resolution could include a Galactic component blended with the redshifted host doublet (MW A_V=0.037 mag suggests it is negligible, but this should be stated).
  4. [§4] §4, first paragraph: the rescaling of the −13 d GMOS-S spectrum to match the EFOSC2 continuum slope is ad hoc; please state the size of the correction and confirm it does not affect the Na I D continuum fit in Fig. 14.
  5. [Various] Abstract: 'the commonly assumption' → 'the common assumption'. §2.5: 'Environmentn' typo. §3, final paragraph: the sentence 'we do not attempt a quantitative assessment of how common or statistically significant this feature is therefore lies beyond the scope' is ungrammatical. Ion notation is inconsistent (Siii/Hei vs Si II/He I). Table 6 reports 12+log(O/H)=8.5539±0.0181 — four decimal places is excessive given the calibration scatter of the N2 diagnostic.

Circularity Check

2 steps flagged

Mild circularity: color/SED-template E(B-V) and the subsequent 'normal T/L once dereddened' checks are largely the same assumption restated, not independent confirmations; Balmer and morphology anchors keep the central claim from collapsing.

specific steps
  1. fitted input called prediction [§5.1 color methods → §5.4 SuperBol / Table 5 / Fig. 15]
    "In summary, the comparison with the intrinsic color templates of M. D. Stritzinger et al. (2018) gives E(B−V) = 0.667±0.501 mag, while the color curve fitting method based on M. R. Drout et al. (2011) yields E(B−V) = 0.57±0.09 mag. ... As the assumed host attenuation increases, the inferred peak luminosity rises by a factor of ∼4.5, the blackbody temperature at g-band peak shifts to higher values (reaching ∼6400 K for E(B−V)host = 0.59 mag ...). The extinction-corrected luminosity and temperature are consistent with those of typical stripped-envelope supernovae"

    E(B-V) is fitted so that observed colors/continuum match assumed intrinsic SESN templates. Applying that same E(B-V) in SuperBol then 'predicts' normal T_BB and peak L versus the T18 Ib sample. For a Planck-like SED, color excess and temperature excess are linked through the extinction law; restoring template colors largely forces T and M back into the normal locus. The T/L agreement is therefore statistically forced by the color-derived input, not an independent prediction.

  2. self definitional [§5.1 spectral SSR dereddening; §7 conclusions item 1]
    "We de-redden the earliest spectrum of SN 2024vjc using a CCM89 attenuation curve... We compare SN 2024vjc with SN 2012au, which is previously shown to exhibit a similar spectral morphology at early epochs and is known to suffer little to no host-galaxy attenuation. ... This yields E(B−V) = 0.767+0.033−0.032 mag. ... A normal SN Ib with the high attenuation provides a consistent picture for essentially all the observed features except only for the Na ID absorption, providing the most straightforward interpretation."

    Intrinsic normality of the continuum shape is assumed by matching to SN 2012au (chosen for line-morphology similarity); E(B-V) is defined as the CCM89 scaling that minimizes continuum SSR against that reference. Declaring that high attenuation then yields a 'normal SN Ib' continuum is true by construction of the fit. The ±0.033 error is only the SSR contour; the paper notes the comparison-object systematic is 'difficult to quantify,' so the precise high E(B-V) and the 'normal after correction' claim are two faces of the same template assumption—correlated with the photometric color methods, not a third independent derivation.

full rationale

This is an empirical observational paper, not a first-principles derivation, so classical definitional circularity is limited. The load-bearing move is: assume SN 2024vjc has a canonical SESN/Ib intrinsic SED (Stritzinger templates, T18 A_V=0 color curve, continuum match to SN 2012au), attribute the entire red excess to host dust, then treat the restored normal luminosity and blackbody temperature under that same E(B-V) as further support. For a near-blackbody optical SED those steps are highly correlated by construction—fitting E(B-V) to match template colors/continuum forces T_BB and M_peak toward the template locus once an extinction law is adopted. The paper still presents color templates, color evolution, spectral SSR dereddening, and SuperBol T/L as a battery of agreeing diagnostics (Table 4, §5.4, §7). That overstates independence within the SN-based cluster and is mild fitted-input / self-definitional circularity. It is not fatal: flattened-spectrum morphology vs SN 2016bau, He I velocities, the R_BB < R_He inequality direction, T_exc ≫ continuum T without dust, the Balmer decrement, and the late-time H II lines are not pure restatements of the color fit, and the headline counterexample (weak Na I D vs high attenuation) does not reduce to Na I D by construction. Score 3 reflects correlated SN-based legs presented as multiple proofs, with real external anchors still present.

Axiom & Free-Parameter Ledger

5 free parameters · 6 axioms · 0 invented entities

The claim rests on standard SN photometry/spectroscopy practice, empirical SESN intrinsic-color priors, extinction-curve and Balmer Case B assumptions, and the Poznanski Na I D calibration as the foil. No new physical entities; free choices are mainly which comparison SN, R_V, and which E(B-V) summary value to adopt.

free parameters (5)
  • Host E(B-V) summary value used in figures (0.59 mag) = 0.59±0.09 mag (color evolution 0–20 d)
    Chosen representative from color-evolution method among a 0.45–0.77 range; shifts absolute magnitudes and SuperBol tracks.
  • Host R_V in photometric conversions = 3.1
    Fixed to 3.1 (MW-like) when converting E(r−i) to E(B-V); spectral grid allows R*_V variation but photometry does not fully free it.
  • SSR spectral dereddening grid best-fit A*_V, R*_V = A*_V=2.6, R*_V=3.4 → E(B-V)≈0.767
    Peak-normalized continuum match to SN 2012au; E(B-V)=A*/R* along ΔSSR≤1 contour.
  • SYN++ photospheric and excitation temperatures = T_phot≳4300 K (no host); T_exc~10000 K
    Adjusted to match flattened and non-flattened early spectrum; T_phot~4300 K without host dust used as lower limit; T_exc~10000 K.
  • Explosion epoch from early ATLAS o-band fireball fit = 60559.5±1.5 MJD
    t_exp sets rise times and phases for all comparisons.
axioms (6)
  • domain assumption Intrinsic SESN color templates / low-A_V CSP-I subsample represent the true unreddened color evolution of a normal SN Ib.
    Load-bearing for Drout/Stritzinger-style E(B-V) in §5.1; paper notes flatter r−i may increase uncertainty.
  • domain assumption CCM89 extinction curve (and MW-like R_V for photometry) applies to the host dust along this line of sight.
    Used for Galactic correction, host conversions, and spectral dereddening grid (§2.1, §5).
  • domain assumption Case B recombination Hα/Hβ=2.86 yields host E(B-V) from the +123 d H II region lines.
    §5.3 Balmer decrement following Domínguez et al. (2013) coefficients.
  • domain assumption Poznanski et al. (2012) EW(Na I D)–E(B-V) relation is the standard benchmark being tested (with Turatto et al. 2003 as alternate).
    §5.2; central foil for the counterexample claim.
  • domain assumption Blackbody SED and R_BB≈R_phot must lie below the He I line-forming radius under homologous expansion.
    §5.4 SuperBol consistency argument favoring E(B-V)≳0.45.
  • ad hoc to paper Polynomial continuum and double-Gaussian modeling give a usable Na I D EW despite possible He I contamination and D2/D1≈1.
    Only detection is −13 d GMOS; paper flags caution but still quotes E(B-V)~0.18.

reviewed 2026-07-30 · how reviews work

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Cite this review

Pith. "Pith review of Dust Without Na I D Trace: The Case of Highly Attenuated Type Ib SN 2024vjc." pith.science (2026). https://pith.science/paper/RAJ6MKCB

@misc{pith2026260723690,
  author       = {Pith},
  title        = {Pith review of: Dust Without Na I D Trace: The Case of Highly Attenuated Type Ib SN 2024vjc},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/RAJ6MKCB}},
  note         = {Machine review of arXiv:2607.23690}
}
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abstract

Understanding dust attenuation toward extragalactic transients is critical for recovering their intrinsic properties and probing the local environments of distant galaxies. A popular diagnostic is the Na I D absorption equivalent width widely applied to extragalactic transients. In this paper, we present early-time optical and near-infrared observations of the Type Ib supernova (SN) SN 2024vjc, followed for $\sim$130 days post-explosion. SN~2024vjc exhibits only weak Na~I~D absorption, indicating only a modest host attenuation with $E (B-V)_{\rm host} \sim 0.18$ mag; if this argument were applied, SN~2024vjc would be a peculiar, faint, and red SN Ib while showing the light-curve shape and spectral evolution broadly consistent with those of canonical SNe Ib. We show that this is not the case; SN-based diagnostics (intrinsic color templates, color-curve evolution, and spectral dereddening) together with the Balmer decrement indicate substantial attenuation, $E(B-V) \sim 0.45$ $-$ $0.8$\,mag. The weak Na I D absorption may result from photoionization of neutral sodium by the intense radiation field of a young H$_{2}$ region at the explosion site; this scenario is directly supported by the detection of narrow H$_{\alpha}$, [N$_{2}$], and H$_{\beta}$ emission lines and a blue continuum excess in late-time spectroscopy. SN~2024vjc represents a clear counterexample to the commonly assumption that weak or absent Na I D absorption implies negligible host-galaxy attenuation, and highlights the importance of employing multiple, independent attenuation diagnostics.

Figures

Figures reproduced from arXiv: 2607.23690 by Andrea Pastorello, Andrea Reguitti, Avishay Gal-Yam, Chris Ashall, Claudia P. Guti\'errez, Dino Pierluigi Fugazza, Erkki Kankare, Giorgio Valerin, Giuliano Pignata, Hanindyo Kuncarayakti, Irene Salmaso, Javier Silva-Farf\'an, Jesper Sollerman, Joseph P. Anderson, Keiichi Maeda, Mariusz Gromadzki, Niko Pyykkinen, Priscila J. Pessi, Takashi Nagao, Thomas M. Reynolds, Ting-Wan Chen, Tom\'as E. M\"uller-Bravo.

Figure 1
Figure 1. Figure 1: Legacy Survey DR10 (DECam) g/r/z color composite image of NGC 438, host galaxy of SN 2024vjc. The nucleus of NGC 438 is marked by a cyan cross, while the location of SN 2024vjc is indicated by a red circle. 2.3. REM photometry Follow-up observations of SN 2024vjc were carried out with the Rapid Eye Mount (REM) telescope (G. Chincarini et al. 2003) at La Silla Observatory. Data were obtained using both avai… view at source ↗
Figure 2
Figure 2. Figure 2: Multi-band optical and NIR light curves of the Type Ib supernova SN 2024vjc corrected by MW attenuation. Photometry is shown for the u, B, V, g, r, i, z, o, c, J, H, K-bands, color-coded by band as indicated in the legend. Marker shapes represent different facilities: ATLAS (squares), REM (circles), SPECULOOS (diamonds), VST/OmegaCAM (upward triangles), and EFOSC (pentagons). Open markers of the correspond… view at source ↗
Figure 3
Figure 3. Figure 3: Left: Peak absolute r-band magnitude versus rise time. Right: Peak absolute r-band magnitude versus decline rate parameter ∆m15(r). The comparison sample comprises SESNe from the T18 sample, color-coded by subtype (IIb: blue, Ib: orange, Ic: green, Ic-BL: red). Galactic extinction has been corrected for using the E. F. Schlafly & D. P. Finkbeiner (2011) dust maps with RV = 3.1; no host-galaxy correction is… view at source ↗
Figure 4
Figure 4. Figure 4: Absolute NIR light curves of SN 2024vjc compared to the T18 sample. The left and right panels show the J (pink points) and H (blue points) bands, respectively, as a function of days since g-band maximum. Black and gray stars show SN 2024vjc without host-galaxy extinction correction and corrected for E(B − V )host = 0.59 mag respectively [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: compares the r −i color evolution of SN 2024vjc with the T18 sample. As with the light-curve comparison, we use T18 color curves that are corrected only for Galactic extinction. SN 2024vjc is systematically redder than the comparison objects at all epochs. Around maximum light, the color reaches r − i ≈ 0.4 mag, already exceeding the bulk of the sample, and it evolves to values ≳ 0.6 mag at later phases. T… view at source ↗
Figure 6
Figure 6. Figure 6: Time series of the observed optical spectra of SN 2024vjc. The gray shaded region marks the telluric O2 A-band at ∼7600 ˚A. Vertical colored lines indicate the rest-frame wavelengths of key spectral features; absorption minima appear blueshifted by the photospheric velocity (see 9 for the He λ5876 velocity evolution). similar epochs; the spectra are remarkably similar at all phases, with the only notable d… view at source ↗
Figure 7
Figure 7. Figure 7: Spectral comparison of SN 2024vjc against two reference SNe Ib at similar phases. Left: SN 2024vjc (orange) compared with the intrinsically faint SN 2007Y (green) at four matched epochs (−14, +5, +21, and +39 d). Right: SN 2024vjc compared with SN 2012au (purple) at two matched early epochs (−14 and +5 d), with the W-shaped feature around ∼ 6300 ˚A shared by both objects highlighted in red. In both panels,… view at source ↗
Figure 8
Figure 8. Figure 8: The flattened spectra of SN 2024vjc (blue) at four epochs, compared with those of SN 2016bau (red) at similar phases. 4.1. He I λ5876 velocity evolution [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Left: Velocity space profiles of the He I λ5876 line (the red vertical line indicates the rest wavelength). Spectra are color coded by phase relative to peak brightness; the colored-dotted lines mark the absorption minima determined from the polynomial fits. Right: Temporal evolution of the He I λ5876 absorption velocity. Gray points show the CSP-I Type Ib sample from T18, while filled circles show SN 2024… view at source ↗
Figure 10
Figure 10. Figure 10: Top: SYN++ synthetic spectrum (red) compared with the flattened earliest spectrum for SN 2024vjc (blue). Ions used in this simulation are: He I, O I, Si II, Ca II, and Fe II. Bottom: Contribution of each ion (black) to the SYN++ final spectrum (red) [PITH_FULL_IMAGE:figures/full_fig_p013_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Comparison of the observed -14 day spectrum of SN 2024vjc (black) with SYN++ synthetic spectra for photospheric temperatures of 4300 K (red). No host extinction is assumed in this figure [PITH_FULL_IMAGE:figures/full_fig_p013_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: r − i color evolution of SN 2024vjc compared to the CSP-I SESNe sample of T18. Light blue circles show the full CSP-I sample, and dark blue circles highlight the subset of CSP-I SESNe with negligible host-galaxy attenuation (A host V = 0). The gray solid line shows the median color curve of the full sample, while the red solid line and shaded band show the median and 1σ envelope of the intrinsic (no host … view at source ↗
Figure 13
Figure 13. Figure 13: Left panel: Comparison of the earliest available spectra of SN 2024vjc and SN 2012au. The observed spectrum of SN 2024vjc is shown in semi-transparent blue, while the best fitting de-reddened spectrum is shown in orange. The earliest spectrum of SN 2012au, which suffers from minimal attenuation, is shown in green for comparison. Right panel: Two-dimensional map of the sum of squared residuals (SSR) comput… view at source ↗
Figure 14
Figure 14. Figure 14: Top: Observed GMOS-S spectrum of SN 2024vjc around the Na i D region (5820–5960 ˚A). The red curve shows the degree-3 polynomial continuum fit, derived from the flanking regions 5850–5885 ˚A and 5898–5930 ˚A (shaded orange). The blue shaded region marks the fitting window used for the double-Gaussian model. Vertical dotted lines indicate the rest wavelengths of Na i D2 (5889.95 ˚A, magenta) and D1 (5895.9… view at source ↗
Figure 15
Figure 15. Figure 15: presents the resulting pseudo-bolometric light curve and blackbody parameters under the five host￾attenuation assumptions considered. Without host attenuation, SN 2024vjc reaches a peak luminosity of ∼ 7.5 × 1041 erg s−1 , with a blackbody temperature of ∼ 4100 K at g-band peak that gradually decreases afterward, and a blackbody radius of ∼ 26000 R⊙ at g-band peak. As the assumed host attenuation increase… view at source ↗
Figure 16
Figure 16. Figure 16: The +123 d observed spectrum is shown in gray (raw) and black (smoothed). The de-reddened spectrum, corrected assuming E(B −V ) = 0.59 mag with a RV = 3.1 CCM89 extinction law, is shown in light blue (raw) and blue (smoothed); both spectra are normalized to unity in the 5400–5600 ˚A region and offset. Vertical dashed lines mark the rest-frame wavelengths of Hβ λ4861 (blue dashed), [O III] λ5007 (green das… view at source ↗
Figure 17
Figure 17. Figure 17: Emission line fits to the +123 d GMOS-S spectrum of SN 2024vjc. Left: Hβ λ4861 fitted with a single Gaussian (red curve). Center: The feature near 5007 ˚A fitted with a single Gaussian (red curve); we caution that its width appears inconsistent with an H II region [O III] λ5007 identification. Right: The Hα + [N II] complex fitted simultaneously with a physically constrained triple Gaussian model (red cur… view at source ↗
Figure 18
Figure 18. Figure 18: Summary of the host-galaxy color excess estimates for SN 2024vjc obtained using different methods. Black points indicate the inferred E(B − V )host values, with horizontal error bars representing the associated uncertainties (see [PITH_FULL_IMAGE:figures/full_fig_p024_18.png] view at source ↗

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83 extracted references · 9 canonical work pages · 1 internal anchor

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