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The Hawaii Infrared Supernova Study (HISS): Spectroscopic Data Release 1

T0 review · 3 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read This paper releases 90 near-infrared spectra of 48 transients and argues that the sample reveals unburnt carbon, core structure, carbon monoxide, and a helium-based split among Type II supernovae that optical spectra cannot show.

desk verdict A useful NIR spectral data release whose main science claim about strong vs weak SNe II is confounded by epoch; the data itself is the real contribution. read the letter →

arxiv 2505.18507 v1 pith:UDIOV2RW submitted 2025-05-24 astro-ph.HE

K. Medler , C. Ashall , M. Shahbandeh , J. M. DerKacy , W. B. Hoogendam , D. O. Jones , B. J. Shappee , J. T. Hinkle
show 4 more authors
C. M. Pfeffer E. Baron P. Hoeflich E. Hsiao
This is my paper
classification astro-ph.HE
keywords supernovaenear-infraredspectroscopyspectroscopicdatareleaseTypeIacore-collapsecarbonmonoxideheliumlinesnebularphase
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

The paper's project releases the first batch of a Hawaii-based infrared supernova survey: 90 near-infrared spectra (0.7–2.5 μm) of 48 transient events, gathered over three years with two ground-based spectrographs. The central claim is that this is one of the largest multi-type NIR transient samples available, and that these spectra do scientific work optical data cannot. The paper demonstrates four diagnostics: detecting unburnt carbon in young Type Ia supernovae, measuring core structure of core-collapse supernovae from nebular line widths, tracking the CO first overtone in carbon-rich ejecta, and separating 'strong' from 'weak' Type II supernovae by the helium line's pseudo-equivalent width. If the release is reliable, it gives the community a public benchmark sample for infrared-era follow-up and for testing spectral templates across phases and types.

What carries the argument

The carrying mechanism is the released spectral sample itself, organized around a set of NIR diagnostic features that are stronger and less blended than their optical counterparts. The main objects are the C I 1.0693 μm feature for unburnt carbon in SNe Ia; the He I 1.083 μm line, whose pseudo-equivalent width and high-velocity component separate strong from weak SNe II; nebular emission profiles (He I/Pa-gamma, O I/Fe I, Pa-beta, Si I) fitted with Lorentzians to yield core FWHMs; and the CO first overtone (2.3–2.5 μm) as a ground-based molecular probe of dust formation. These features carry the argument because each is presented as a measurement that optical spectroscopy cannot make cleanly.

What would settle it

Compare the flux-calibrated HISS spectrum of one object to simultaneous ground-based NIR photometry of the same object; if the integrated spectrum disagrees with the photometry by more than the photometric uncertainty in a wavelength-dependent way, the release's quantitative claims lose support.

Watch

Extended reading notes

Core claim

The discovery claim is that a coherent NIR spectral library of this breadth can be assembled and that it already resolves physics that is heavily blended in the optical. On the paper's own terms, DR1 contains 90 spectra of 48 objects—17 SNe Ia, 15 SNe II, 8 stripped-envelope SNe, 6 interacting SNe, 1 TDE, and 1 SLSN-I—reduced systematically and released publicly. The paper reports that template comparisons match well, and it identifies four NIR-only results: a clear detection of unburnt C I 1.0693 μm in the 91bg-like SN 2021qvv; nebular SNe II line widths that place the hydrogen envelope at higher velocity than the iron core except where iron is blended outward; CO first-overtone emission between 2.3 and 2.5 μm in four core-collapse SNe; and a He I 1.083 μm pseudo-equivalent-width dichotomy that splits five SNe II into 'strong' (pEW exceeding 50 Å) and 'weak' groups.

Load-bearing premise

The entire quantitative use of the release rests on the assumption that the wavelength and flux calibration is unbiased, but no arc-lamp calibration or uncertainty estimate is provided for the largest subset of spectra.

Editorial extensions

If this is right

  • The 90 released spectra substantially increase the public NIR transient sample and give template builders a multi-type, multi-epoch benchmark.
  • Pre-maximum SNe Ia spectra show at least three shapes of the 1 μm feature (flat, V, and W), so early-time diversity in outer ejecta is measurable and can be tied to explosion models.
  • Nebular NIR line FWHMs in SNe II let observers estimate the velocity structure of the ejecta core and identify mixing or asymmetry of iron-group material.
  • Ground-based CO first-overtone detections in four core-collapse SNe show that molecular formation and dust precursors can be monitored without space-based facilities.
  • The He I 1.083 μm pseudo-equivalent-width boundary at 50 Å offers a practical way to split SNe II into two groups that likely correspond to different progenitor and circumstellar configurations.

Reading between the lines

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

  • If the calibration holds, the same spectra could be used to build quantitative early-time SNe Ia templates before about -5 days, a phase the paper notes is under-sampled.
  • The He I pEW dichotomy suggests a testable prediction: 'weak' SNe II in this sample should decline more slowly in luminosity than 'strong' ones, a link the paper states but does not verify with light curves here.
  • The CO detections at about +269 and +289 days imply significant CO survival; a radiative-transfer model of these spectra could constrain CO mass and temperature and predict when dust should form.
  • Comparing the released NIR line velocities with optical velocities of the same objects at the same epochs would provide a straightforward external check on the wavelength calibration.
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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 / 5 minor

Summary. The paper presents the first data release of the Hawaii Infrared Supernova Study (HISS), comprising 90 near-infrared spectra (0.7–2.5 μm) of 48 transient events obtained with Keck-II/NIRES and IRTF/SpeX between 2021 and 2024. The sample includes Type Ia, Type II, stripped-envelope, and interacting SNe, plus one TDE and one SLSN-I. The authors describe the observations and reduction pipelines (Pypeit and Spextool), present the full spectral atlas, compare representative spectra to existing templates, and highlight four science applications: detection of unburnt carbon in SNe Ia, measurement of nebular line widths in SNe II, identification of the CO first overtone, and a proposed dichotomy in SNe II based on the He I 1.083 μm pseudo-equivalent width. The spectra are publicly released via WISeREP.

Significance. If the calibration and data products are validated, HISS DR1 is a valuable community resource that materially increases the number of publicly available NIR transient spectra, complementing larger samples such as CSP II and KITS. A particular strength is that the paper does not derive its scientific conclusions from the templates it compares against; the template comparison is used only for benchmarking, so there is no circularity concern despite overlapping authorship. The four science highlights are presented as demonstrations of the dataset's utility, and several are genuinely novel for a data release paper (e.g., the epoch-resolved He I pEW behavior). The release of the spectra through WISeREP is a concrete, reproducible contribution. However, the quantitative support for at least one headline result and the calibration reproducibility need strengthening before the paper can be accepted.

major comments (3)
  1. [§3.1, §3.2, §9] The strong/weak SNe II classification is epoch-confounded. SN2021tiq is classified as the sole weak SN II based on pEW = 27.95 Å at +57.58 d, but the same object at +123.91 d has pEW = 135.13 Å, which exceeds the paper's own 50 Å strong threshold. The four strong SNe are observed at +61 to +84 d, so the comparison is not epoch-matched. No pEW uncertainties, continuum-fitting prescription, or epoch-correction are provided. Because this dichotomy is listed in the abstract and conclusions as one of the four key science results, the current data do not support the claimed weak category or the associated high-velocity helium interpretation. The authors should either restrict the classification to a narrow phase bin, apply a phase correction, or explicitly reframe this as a single-epoch tentative observation rather than a supported dichotomy.
  2. [§5.4] The NIRES flux calibration and telluric correction rely on custom Python scripts that are not released, and no uncertainty estimates or photometric cross-checks are provided for the final flux calibration. Since the paper encourages quantitative use (pEW, FWHM, velocities), the absence of calibration validation or error spectra limits the reproducibility and reliability of derived quantities. The authors should release the reduction scripts and provide at least one validation check (e.g., comparison with photometry or repeat observations of the same object), and clearly state whether error arrays are included in the WISeREP data files.
  3. [§5.4] The mass-loss rate for SN2020aekp (Mdot ≈ 10^-3 M_sun/yr, M_CSM ≈ 1 M_sun) is derived from a single Pa-beta FWHM (102 ± 15 km/s) using equations from Yang et al. (2023) with assumed expansion velocity (7000 km/s), spherical geometry, and 20% kinetic-to-radiation conversion efficiency, but no uncertainty propagation or discussion of systematic errors is given. This quantitative claim should be presented as an illustrative estimate with the stated assumptions and a caveat that the derived values carry large unquantified uncertainties.
minor comments (5)
  1. [§4.6] The caption refers to 'SN2020fpl' but the text and Table A1 consistently identify the object as SN2021fpl; please correct the typo.
  2. [§5] The text says uncertainties on t_max were determined from photometric cadence and the fitting procedure, but no uncertainty values are reported in Table A1 or elsewhere, so phase uncertainties cannot be assessed by users.
  3. [§6.1] The Gaussian smoothing is described as 'sigma value of 3' but the units (pixels, wavelength bins, or velocity) are not specified; please state the smoothing scale explicitly.
  4. [Abstract] The sBV template-matching procedure is described only qualitatively ('the template spectra that most accurately reproduce the features'); please specify the matching metric or fitting procedure used to select the adopted sBV value.
  5. [Abstract] The claim that this is 'one of the largest NIR samples of transients available to the astrophysical community' is difficult to reconcile with the larger CSP II (909 spectra) and KITS (274 spectra) samples cited in the introduction; please rephrase to 'one of the largest publicly available NIR samples of transients spanning multiple types' or similar.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: HISS DR1 is a data release whose templates and classification benchmarks are external comparisons, not inputs that force the released spectra.

full rationale

The central deliverable is a set of 90 reduced NIR spectra obtained from raw Keck-II/NIRES and IRTF/SpeX observations, reduced with Pypeit and Spextool. The four science highlights are identifications and measurements made on those spectra, not outputs of a model fitted to the same spectra. The template comparisons in Section 6 use templates from Lu et al. (2023), Davis et al. (2019), and Shahbandeh et al. (2022), which have overlapping authorship, but the paper uses them as external benchmarks for visual comparison rather than deriving the spectra from them. The sBV matching in Section 6.1 is explicitly a tuning step ('the sBV value was varied between 0 and 1.5 to construct an array of template spectra for each epoch'), and the paper does not present the resulting match as a prediction; it merely displays the best-matching template. The §7.4 'strong' vs 'weak' SNe II classification applies the pEW threshold from Davis et al. (2019) to five objects; this is a reproduction of an existing classification scheme on new data, not a circular derivation. The notable weakness that SN2021tiq has pEW = 27.95 Å at +57.6 d but 135.13 Å at +123.9 d is an epoch-confounding and measurement-validity concern, not a circularity: it does not reduce a predicted quantity to an input. No fitted parameter is renamed as a prediction, no uniqueness theorem is imported from the authors' prior work, and no ansatz is smuggled in via citation. The paper is largely self-contained as a spectroscopic data release, so the circularity score is low.

Assumptions & free parameters 4 free parameters · 4 assumptions · 0 invented entities

The paper introduces no new physical entities. Its central claims rest on standard astrophysical assumptions (extinction law, classification from TNS), well-documented reduction software, and prior spectral templates. The main free parameters are tuning and assumption values used in the demonstrative analyses, which do not affect the core data release.

free parameters (4)
  • sBV template matching range = 0 to 1.5
    For SNe Ia template comparison in Section 6.1, sBV was varied over 0 to 1.5 to construct template spectra that match the observed data; this is a tuning parameter, not an independently measured quantity.
  • Gaussian smoothing sigma = 3 pixels
    All spectra were smoothed with a Gaussian filter using sigma=3 (Section 5); this is a processing choice, not a physical parameter.
  • Expansion velocity for SN2020aekp mass-loss rate = 7000 km/s
    Section 5.4: a typical SNe Ia expansion velocity of about 7000 km/s is assumed when applying equations 3-6 from Yang et al. (2023) to derive the mass-loss rate for SN2020aekp; this is not measured for this object.
  • Kinetic-to-radiation conversion efficiency = 20%
    Section 5.4: the mass-loss rate estimate assumes a conversion efficiency between kinetic energy and radiation of about 20%, following Yang et al. (2023).
assumptions (4)
  • domain assumption Milky Way extinction correction with Rv=3.1
    Section 5: spectra are corrected for Milky Way extinction assuming Rv=3.1 (Schlafly & Finkbeiner 2011); host galaxy extinction is not corrected, with the justification that the effect is minimal in the NIR.
  • domain assumption TNS classifications are reliable
    Section 4: the SN type for each object is taken from the classification reports on the Transient Name Server without independent verification.
  • domain assumption Template line identifications from prior literature
    Sections 5 through 7: spectral feature identifications rely on line lists and template spectra from Marion et al. (2009), Davis et al. (2019), Shahbandeh et al. (2022), and related works.
  • domain assumption Distance-limited sample D<=125 Mpc
    Section 2.2: targets were selected to be within 125 Mpc, with exceptions for rare luminous events; this introduces a selection bias that is stated but not corrected for.

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Cite this review

Pith. "Pith review of The Hawaii Infrared Supernova Study (HISS): Spectroscopic Data Release 1." pith.science (2026). https://pith.science/paper/UDIOV2RW

@misc{pith2026250518507,
  author       = {Pith},
  title        = {Pith review of: The Hawaii Infrared Supernova Study (HISS): Spectroscopic Data Release 1},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/UDIOV2RW}},
  note         = {Machine review of arXiv:2505.18507}
}
abstract

We present the first data release of the Hawaii Infrared Supernova Study (\textit{HISS}), consisting of a large sample of near-infrared (NIR) spectra, $0.7 - 2.5 \mathrm{\mu m}$, obtained with the Keck-II/NIRES and IRTF/SpeX spectrographs. This sample is comprised of 90 NIR spectra of 48 transient events, spanning from hours after explosion to $\geq + 350$ days. Acquired over three years (2021-2024), this data release includes 17 Type Ia SNe, 15 Type II SNe, 8 Stripped Envelope SNe, 6 interacting SNe, 1 TDE, and 1 SLSN-I. These spectra were all systematically reduced using either the \textsc{Python}-based reduction code \textsc{Pypeit} or the \textsc{IDL}-based \textsc{Spextool} and constitute one of the largest NIR samples of transients available to the astrophysical community. We show the utility of NIR spectra and identify the key spectral features across multiple types of SNe. We show how both early-time and nebular-phase NIR spectra can be used to investigate the physics of the explosion, and to reveal the properties of the progenitor. With the addition of this dataset, the number of publicly available NIR spectra spanning multiple transient types has been substantially increased. In its next phase, \textit{HISS} will leverage target-of-opportunity spectral observations and NIR imaging from telescopes on Maunakea. Expanding the NIR dataset of SNe is vital to the transient community, particularly in light of the increasing emphasis on the infrared regime following the recent launch of the \textit{James Webb Space Telescope} and the forthcoming launch of the \textit{Nancy Grace Roman Space Telescope}.

Figures

Figures reproduced from arXiv: 2505.18507 by the authors.

Figure 1
Figure 1. Left: The total number of objects observed in DR1 categorized by supernova types and sub-types. Right: The number of spectra obtained for each spectral classification and subtype. which published a sample of 41 spectra obtained from 28 normal SNe Ia, ii) the Carnegie Supernova Project II (CSP II; Phillips et al. 2019; Hsiao et al. 2019; Davis et al. 2019; Ashall et al. 2021; Hoogendam et al. 2022; Shahbandeh et al. … view at source ↗
Figure 2
Figure 2. Left: Phase distribution relative to epoch of maximum light in the 𝑔/𝑜-bands for SNe Ia, SNe II, SE-SNe, Interacting SNe and other objects. Right: Redshift distribution of the objects observed by HISS. Vertical dashed lines denote the median phase and redshift for the different classifications observed in this data release. by a model NIR spectrum of an A0V star adjusted for the at￾mospheric conditions at Maunakea. … view at source ↗
Figure 3
Figure 3. NIR spectra of four SNe representing a typical evolution of SNe Ia, SNe II and SNe IIb. These objects possessed the largest temporal range in DR1. Strong features are labeled based on previous studies of NIR SNe (Marion et al. 2009; Davis et al. 2019; Shahbandeh et al. 2022; Ashall et al. 2019a), with the label located at the rest wavelength of the line [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: Comparison of SN 2021rhu, SN 2022hrs, and SN 2022ihz to the spectral template constructed using the data presented in (Lu et al. 2023). Spectra are shown in rest wavelength, and the gray regions denote telluric regions. The 𝑠𝐵𝑉 values used in constructing the template …
Figure 5
Figure 5. Figure 5: Similar to [PITH_FULL_IMAGE:figures/full_fig_p011_5.png]
Figure 6
Figure 6. Figure 6: Similar to [PITH_FULL_IMAGE:figures/full_fig_p012_6.png]
Figure 7
Figure 7. Figure 7: Structure of the C i 1.0693 𝜇m line observed in the pre-peak NIR spectra of SNe Ia. The rest wavelength of the C i 1.0693 𝜇m and Mg ii 1.0927 𝜇m lines are given by the dashed vertical lines. The spectra are divided into three groups and col￾or-coded according to the st…
Figure 8
Figure 8. Figure 8: Nebular-phase emission features of the He i 1.083 𝜇m / Pa𝛾 1.094 𝜇m, O i 1.129 𝜇m / Fe i 1.142 𝜇m, Pa𝛽 1.282 𝜇m, and Si i 1.644 𝜇m lines of the three SNe II SN 2020jfo, SN 2020qmp and SN 2022acko. Features were fitted with either a single or double Lorentzian function …
Figure 9
Figure 9. Figure 9: Average FWHM of the strong nebular phase emission lines across the 4 spectra of SNe 2020jfo, 2020qmp, and 2022acko. The hydrogen envelope is located at larger velocities than all lines except the Fe i 1.142 𝜇m line, which are brought up significantly by SN 2020jfo and …
Figure 10
Figure 10. Figure 10: The CO first overtone can be identified in ground-based NIR spectra of CC-SNe in the weeks to months following maximum light. CO was not identified in all SNe shown; those SNe with confident identification of CO are marked with a ∗. spectively suggesting significant a…
Figure 11
Figure 11. Figure 11: Line profile of the He i 1.083 𝜇m feature, used in determining the strength of the SN II. All spectra were taken between +50−130 days after maximum light, when the absorption component was still visible. Left: Strong SNe II SN 2022mit, SN 2022dml, SN 2021qvr, and SN 2…

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Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

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