Pith. sign in

REVIEW 3 major objections 4 minor 2 cited by

Type Ia SN 2019ein: New Insights into the Similarities and diversities among High-Velocity SNe Ia

T0 review · 3 major / 4 minor · reviewed 2026-08-14 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read SN 2019ein, caught within days of explosion, shows that high-velocity Type Ia supernovae are not a one-parameter family and that their outer ejecta match delayed-detonation models.

desk verdict A genuinely useful early-time HV SN Ia dataset with a plausible velocity-evolution claim; the TARDIS stratification is suggestive but model-dependent and the abstract should be toned down. read the letter →

arxiv 1908.03001 v3 pith:6ANPYR6H submitted 2019-08-08 astro-ph.HE

Miho Kawabata , Keiichi Maeda , Masayuki Yamanaka , Tatsuya Nakaoka , Koji Kawabata , Ryo Adachi , Hiroshi Akitaya , Umut Burgaz
show 33 more authors
Hidekazu Hanayama Takashi Horiuchi Ryohei Hosokawa Kota Iida Fumiya Imazato Keisuke Isogai Ji-an Jiang Noriyuki Katoh Hiroki Kimura Masaru Kino Daisuke Kuroda Hiroyuki Maehara Kazuya Matsubayashi Kumiko Morihana Katsuhiro Murata Takashi Nagao Masafumi Niwano Daisaku Nogami Motoki Oeda Tatsuharu Ono Hiroki Onozato Masaaki Otsuka Tomoki Saito Mahito Sasada Kazuki Shiraishi Haruki Sugiyama Kenta Taguchi Jun Takahashi Kengo Takagi Seiko Takagi Masaki Takayama Miyako Tozuka Kazuhiro Sekiguchi
This is my paper · ORCID
classification astro-ph.HE
keywords TypeIasupernovaehigh-velocitySN2019einbroad-linespectralsynthesislightcurvesdelayeddetonationsupernovastructure
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 2019ein, a high-velocity (HV), broad-line Type Ia supernova, was caught within days of explosion and monitored from about 2 days after the estimated explosion date. Its rapid decline ($\Delta$ m15(B)=1.36±0.02 mag) and short rise time (15.37±0.55 days) place it in a previously poorly sampled part of the HV class. The paper shows that the pre-maximum speed of the Si II velocity decrease correlates with the light-curve decline rate, not only with the maximum-light velocity, so the HV class is not a one-parameter family. Spectral synthesis of the earliest spectra reveals an outer O-Ne-C burning layer extending to at least 25,000–30,000 km/s with no unburnt carbon below 30,000 km/s, similar to the HV SN 2002bo and different from the NV SN 2011fe, and this structure is consistent with the delayed-detonation scenario.

What carries the argument

The argument is carried by early-time spectroscopy combined with one-dimensional spectral synthesis modeling. The model assumes a power-law density structure normalized to the W7 model at 17,000 km/s and a two-layer composition: an O-Ne-C burning layer (O=0.68, Ne=0.025, Mg=0.1, Si=0.2, S=0.025, Ca=5e-4) and an unburnt C+O layer (C=0.5, O=0.475, Ne=0.025). By varying the velocity of the burnt/unburnt interface and the carbon mass fraction in the burning layer, the authors constrain the interface to lie above ~30,000 km/s and the carbon fraction to ≤4% near 20,000 km/s. A two-Gaussian decomposition of the Si II line is used to show that a high-velocity feature does not contaminate the photospheric component, and the photospheric velocities at the two earliest epochs (20,000 and 17,000 km/s) anchor the structural inference.

What would settle it

A decisive test: obtain an early-time spectrum (within ~4 days of explosion) of another fast-declining HV SN Ia; if it shows a strong C II absorption below 30,000 km/s, or Si II velocities that do not track the decline rate, the paper's two-parameter picture and the proposed outer structure would be contradicted.

Watch

Extended reading notes

Core claim

SN 2019ein is a broad-line HV Type Ia supernova with $\Delta$ m15(B)=1.36±0.02 and a rise time of 15.37±0.55 days. Its Si II lambda6355 velocity reached ~20,000 km/s at 12 days before maximum and declined rapidly and smoothly to ~13,000 km/s at maximum. The paper argues that this evolution shows that the speed of spectral evolution in HV SNe depends on the light-curve decline rate as well as on the maximum-light velocity. Spectral synthesis of the spectra at 3.7 and 5.7 days after the explosion, using a two-layer composition (O-Ne-C burning interior and unburnt C+O exterior) with a power-law density normalized to the W7 model at 17,000 km/s, shows that the O-Ne-C burning layer extends to at least 25,000–30,000 km/s and that no unburnt carbon exists below ~30,000 km/s, with a carbon mass fraction at ~20,000 km/s of at most 4% (conservatively 10%). This structure is shared with the prototypical HV SN 2002bo, despite their different $\Delta$ m15(B), and differs from the O-Ne-C layer confined to 13,300–19,400 km/s in the NV SN 2011fe. The resulting relation between 56Ni mass (or $\Delta$ m15) and the extent of the O-Ne-C burning layer is proposed as a key constraint on the explosion mechanism.

Load-bearing premise

The inferred outer structure assumes the ejecta are spherically symmetric with a power-law density normalized to a standard model at 17,000 km/s and a composition of just two unmixed layers; if the actual density slope, mixing, or composition differs, the derived interface velocity and carbon limit would change.

Editorial extensions

If this is right

  • The high-velocity class of Type Ia supernovae is not described by a single parameter; the pre-maximum spectral evolution encodes both the maximum-light velocity and the decline rate.
  • The outer ejecta of HV SNe share an O-Ne-C burning layer extending to high velocities with no unburnt carbon below 30,000 km/s, independent of Delta m15(B).
  • This outer structure is consistent with the delayed-detonation explosion scenario and disfavors a pure-deflagration (W7-like) outer composition.
  • The relation between 56Ni mass (or Delta m15) and the extent of the O-Ne-C burning layer gives a new observational constraint on explosion models.
  • The lack of an early excess over the fireball model places an upper limit of 4.3–7.6 R_sun on the companion radius, effectively excluding a line-of-sight red giant companion.

Reading between the lines

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

  • If early-time spectra of additional HV SNe with a range of decline rates confirm the extended O-Ne-C burning layer, the HV/NV dichotomy may reflect different transition densities in the delayed detonation, and the correlation between 56Ni mass and burning extent could be broken by asphericity or viewing angle.
  • Applying the same two-layer spectral modeling to a larger sample of SNe Ia would produce a map of burnt/unburnt interface velocity versus decline rate, providing a direct test of the proposed constraint.
  • The two-parameter behavior found here hints that standardized-candle corrections for Type Ia supernovae might need to incorporate pre-maximum velocity evolution independently of decline rate, potentially reducing scatter in cosmological distance estimates.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

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. This paper presents BVRI/g'JHKs/Swift-UVOT photometry and optical spectroscopy of SN 2019ein starting about two days after the estimated explosion, together with light-curve fits and spectral analysis. The authors classify SN 2019ein as a High-Velocity (HV) and Broad-Line SN Ia with Delta m15(B)=1.36±0.02 and a short rise time of 15.37±0.55 days. They find that the Si II 6355 velocity reached about 20,000 km/s at -12 days and declined rapidly to about 13,000 km/s at maximum light, and they argue that the pre-maximum velocity evolution of HV SNe Ia depends on the decline rate as well as on the maximum-light velocity. Using two early spectra and the TARDIS spectral synthesis code, they infer an outer composition with O-Ne-C burning material extending to at least 25,000-30,000 km/s and no unburnt C+O below about 30,000 km/s, similar to their reading of SN 2002bo and different from SN 2011fe, and they discuss the implications for delayed-detonation and sub-Chandrasekhar explosion models.

Significance. The data set is valuable: very early multi-band coverage of an HV SN Ia with relatively large Delta m15 is rare, and the photometric and spectroscopic measurements are carefully reduced with uncertainties reported. If the velocity-evolution claim holds, it is an important addition to the evidence that the HV class is not a one-parameter family. The compositional inference, if secure, would connect the nickel-mass/decline-rate sequence to the radial extent of burning products and would discriminate among explosion mechanisms. The TARDIS section is transparent about its simplifying assumptions, and the authors explicitly write that 'there is no guarantee that the spectral synthesis model provides a unique solution.' However, the paper's broader significance depends on the robustness of the outer-structure inference, and that robustness is not yet demonstrated because the constraints are derived from one-at-a-time variations around a fixed density and composition ansatz.

major comments (3)
  1. [§4.2 (Figs. 11 and 12)] The conclusion that the O-Ne-C burning layer extends to at least 25,000-30,000 km/s and that there is no unburnt C+O below about 30,000 km/s is not yet robust, because it is obtained by varying one parameter at a time around a fixed model: a power-law density normalized to W7 at 17,000 km/s with the W7 slope continued beyond 20,000 km/s, fixed mass fractions in two discrete layers, and no mixing. The paper itself admits that the spectral synthesis model does not provide a unique solution. The carbon upper limit is explicitly placed only near the photosphere at about 20,000 km/s, while the 'no unburnt carbon below 30,000 km/s' statement rests on the inferred interface velocity, which is sensitive to the assumed density slope and to the adopted photospheric velocities of 20,000 and 17,000 km/s at the two modeled epochs. Because the comparison with SN 2002bo and SN 2011fe and the subsequent explosion-mechanism discussion depend on these specific boundaries, this non-uniqueness is load-bearing rather than cosmetic. I ask the authors to test the sensitivity of the interface and carbon constraints to (i) the outer density power-law index, (ii) the assumed photospheric velocities within a plausible range such as ±2,000 km/s, and (iii) modest mixing between the two layers, or alternatively to reformulate the main conclusions so that they are explicitly conditional on the adopted two-layer model.
  2. [§4.2-4.3] The comparison of the outer structure of SN 2019ein with that of SN 2002bo (Stehle et al. 2005) and SN 2011fe (Mazzali et al. 2014) compares a TARDIS-based parameterization for 2019ein with structures derived using different spectral synthesis codes, different density profiles, and different fitting strategies. It is therefore unclear whether the reported 'strikingly different' structure relative to SN 2011fe, and the claimed similarity to SN 2002bo, reflect astrophysical differences or systematic differences in the modeling approaches. Please either apply the same TARDIS setup to the early spectra of the comparison objects, or soften the comparative claim so that it is stated as a qualitative statement that the two-layer parameterization fitting SN 2019ein is hard to reconcile with the published stratification of SN 2011fe.
  3. [§3.3 and §4.1] The claim that the pre-maximum Si II velocity evolution of HV SNe is 'more strongly correlated with Delta m15(B)' and that HV SNe 'do not form a one-parameter family' is based on one newly observed object and a small literature sample, with no quantitative correlation analysis. The velocity-gradient values in §3.3 place SN 2019ein within the range of other HV SNe, and SN 2002er, the closest decline-rate comparator, is itself a transitional HV/NV object. Please add a statistical test or partial-correlation analysis of the HV sample relating pre-maximum velocity evolution, maximum-light velocity, and Delta m15(B), or revise the wording to present this as a suggestive trend rather than an established property. As written, the two-parameter claim is not yet supported beyond the level of an example.
minor comments (4)
  1. [Abstract] The abstract contains a typo: 'Bload Line' should be 'Broad Line'.
  2. [§2.2] The sentence 'A lot of the spectroscopic observation is listed in Table 5' should read 'The log of the spectroscopic observations is given in Table 5'.
  3. [§4.2] In the sentence 'The velocities found here is even higher', the verb should agree with the plural subject: 'The velocities found here are even higher'.
  4. [Figures 11 and 12] In the provided version of the manuscript, the panel labels in Figures 11 and 12 appear garbled; please verify that the published figure labels are legible.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the central photometric, spectroscopic, and spectral-fit constraints are derived from new data, and the model-dependence of the TARDIS setup is explicitly acknowledged rather than hidden.

full rationale

The paper's principal empirical results (rise time, Delta m15, Si II velocity evolution, HV/BL classification) come from new photometry and spectroscopy compared with published samples, not from assumptions that already contain those conclusions. The TARDIS spectral modeling in Section 4.2 does adopt an assumed two-layer O-Ne-C/unburnt composition and a W7-normalized power-law density, but the key constraints (burnt/unburnt interface above about 30,000 km/s and carbon fraction below about 4% near 20,000 km/s) are obtained by explicitly varying those parameters and comparing the synthetic Si II profile to the observed spectra, so they are not equal to the model inputs by construction. The paper even states in Section 4.2 that 'there is no guarantee that the spectral synthesis model provides a unique solution,' which is an honest robustness caveat rather than a circular step. The later conclusion that the structure resembles delayed-detonation models is a model-comparison inference based on the data-constrained interface location, not a self-citation chain or an ansatz smuggled in as an external uniqueness theorem. No load-bearing self-citation is used, and no prediction is merely a renamed fitted parameter. The model dependence and non-uniqueness are real scientific limitations, but they are not circularity in the sense of the derivation reducing to its own inputs.

Assumptions & free parameters 4 free parameters · 6 assumptions · 0 invented entities

The central composition claim rests on a chain of model inputs rather than directly measured quantities: the fireball-based explosion epoch, the W7-normalized power-law density structure, the two-layer composition with delayed-detonation mass fractions, and the hand-chosen photospheric velocities. The velocity-evolution claim rests on the assumption that the single-Gaussian Si II velocity tracks the photosphere without significant high-velocity-feature contamination, which the paper tests with a two-Gaussian decomposition. These assumptions are reasonable but not independently verified for SN 2019ein. No new physical entities are introduced.

free parameters (4)
  • Explosion epoch MJD = 58602.87 ± 0.55
    Fitted by the fireball model f ∝ t^2 to early BVRI light curves in Section 4.1; sets the phases of the early spectra and the rise time.
  • Photospheric velocity at -11.5 days (TARDIS) = 20,000 km/s
    Chosen in the TARDIS model in Section 4.2 to match the earliest spectrum; sets the inner boundary of the modeled outer layer.
  • Photospheric velocity at -9.5 days (TARDIS) = 17,000 km/s
    Same as above for the second spectrum; defines the velocity range over which the O-Ne-C layer is probed.
  • Outer density power-law slope
    Assumed above 17,000 km/s with normalization to W7 at the inner boundary; the paper does not specify the index, and the inferred interface velocity depends on it. This is a chosen input rather than a fitted value.
assumptions (6)
  • domain assumption The fireball model (f ∝ t^2) with a common explosion epoch across bands describes the early rise.
    Used in Section 4.1 to derive the explosion date MJD 58602.87 and rise time 15.37 days. This is a standard approximation for SN Ia early light curves; some SNe require broken power laws, and the paper finds no deviation after about two days post-explosion.
  • domain assumption The ejecta are spherically symmetric and in homologous expansion, permitting 1D TARDIS synthesis.
    Adopted for the spectral synthesis in Section 4.2; ignores clumping and asymmetry that may be present in HV SNe.
  • ad hoc to paper The outer composition is described by two discrete layers (O-Ne-C burning and unburnt C+O) with fixed mass fractions taken from delayed-detonation models.
    The composition inputs in Section 4.2 (O=0.68, Ne=0.025, Mg=0.1, Si=0.2, S=0.025, Ca=5e-4 for the burning layer; C=0.5, O=0.475, Ne=0.025 for the unburnt layer) are taken from delayed-detonation nucleosynthesis models, not derived from the data. This is the main model assumption behind the inferred interface velocity and carbon fraction.
  • domain assumption The W7 model provides the density normalization at 17,000 km/s and a representative density structure beyond.
    Used in Section 4.2. The paper notes the outermost density structure is diverse across models and that the adopted structure is within model predictions, but the constraint on the burnt/unburnt interface depends on this choice.
  • domain assumption SN 2019ein obeys the standard SN Ia luminosity-width and color relations for distance and extinction estimation.
    Used in Section 3.2 to derive E(B-V)_host = 0.09 and distance modulus 32.95, superseding the less certain NED distance of 32.20. If the standardization does not apply, the derived absolute luminosity and companion radius upper limit change.
  • domain assumption The photospheric component of Si II lambda6355 keeps a constant FWHM equal to the maximum-light value over the early epochs.
    Used in Section 3.4 for the two-Gaussian decomposition that rules out significant high-velocity-feature contamination. The FWHM is fixed following the SN 2012fr analysis; if the photospheric line broadens or narrows with time, the high-velocity-feature contribution could be underestimated.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Type Ia SN 2019ein: New Insights into the Similarities and diversities among High-Velocity SNe Ia." pith.science (2026). https://pith.science/paper/6ANPYR6H

@misc{pith2026190803001,
  author       = {Pith},
  title        = {Pith review of: Type Ia SN 2019ein: New Insights into the Similarities and diversities among High-Velocity SNe Ia},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6ANPYR6H}},
  note         = {Machine review of arXiv:1908.03001}
}
read the original abstract

We present optical observations of type Ia supernova (SN) 2019ein, starting at 2 days after the estimated explosion date. The spectra and the light curves show that SN 2019ein belongs to the High-Velocity (HV) and Bload Line groups with relatively rapid decline in the light curves (Delta m15(B) = 1.36 +- 0.02 mag) and the short rise time (15.37 +- 0.55 days). The Si II 6355 velocity, associated with a photospheric component but not with a detached high-velocity feature, reached ~ 20,000 km s-1 at 12 days before the B-band maximum. The line velocity however decreased very rapidly and smoothly toward the maximum light, where it was ~ 13,000 km s-1 as relatively low among HV SNe. This indicates that the speed of the spectral evolution of HV SNe Ia is correlated not only to the velocity at the maximum light, but also to the light curve decline rate like the case for Normal-Velocity (NV) SNe Ia. Spectral synthesis modeling shows that the outermost layer at > 17,000 km s-1 is well described by the O-Ne-C burning layer extending to at least 25,000 km s-1, and there is no unburnt carbon below 30,000 km s-1; these properties are largely consistent with the delayed detonation scenario, and are shared with the prototypical HV SN 2002bo despite the large difference in Delta m15(B). This structure is strikingly different from that derived for the well-studied NV SN 2011fe. We suggest that the relation between the mass of 56Ni (or Delta m15) and the extent of the O-Ne-C burning layer provides an important constraint on the explosion mechanism(s) of HV and NV SNe.

Figures

Figures reproduced from arXiv: 1908.03001 by the authors.

Figure 1
Figure 1. R-band image of SN 2019ein and the comparison stars taken with the Kanata telescope / HOWPol on MJD 58615.7 (2019 May 12). in IRAF17, without subtracting the galaxy template. For the data in the first few days, we have checked the contamination from the host galaxy by subtracting the SDSS images from our images. Within the uncertainty set by the difference in the photometric filters, the result of this exercise agre… view at source ↗
Figure 2
Figure 2. Multi-band light curves of SN 2019ein. The different symbols denote data that were obtained using different instruments (see the figure legends). The light curve of each band is shifted vertically as indicated in the figure. We adopted MJD 58618.24 ± 0.07 as day zero. For comparison, we show the light curves of SN 2002bo with solid lines (Benetti et al. 2004; Krisciunas et al. 2004). 0 1 2 3 4 5 -20 -10 0 10 20 30 4… view at source ↗
Figure 3
Figure 3. B-band light curve of SN 2019ein. For comparison, we plot those of SNe 2002bo (Benetti et al. 2004; Krisciunas et al. 2004), 2002dj (Pignata et al. 2008), 2002er (Pignata et al. 2004), and 2011fe (Zhang et al. 2016). The inset panel shows the light curves expanded around the maxi￾mum light. 3.3. Spectral Properties [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figures from the paper (7 more)
Figure 4
Figure 4. Figure 4: Spectral evolution of SN 2019ein (black lines). The epoch for each spectrum is indicated on the right outside the panel. For comparison, we plot the spectra of SNe 2002bo (blue lines; Benetti et al. 2004, Blondin et al. 2012). 0 10 20 30 40 50 60 100 200 02bo 02dj 02er…
Figure 5
Figure 5. Figure 5: Pseudo equivalent widths of Si ii λ6355 and Si ii λ5792. The comparison samples are from Silverman et al. (2012a). Note that the Broad Line and Core Normal classes correspond to the HV and NV classes. days since the discovery, which is likely ∼ 2.4 days since the explo…
Figure 7
Figure 7. Figure 7: Evolution of Si ii λ6355 line profile of SN 2019ein as shown in velocity space. For comparison, we show the spectra of SNe 2012fr (Childress et al. 2013), 2002bo (Benetti et al. 2004; Blondin et al. 2012), 2002er (Kotak et al. 2005), 2002dj (Pignata et al. 2008), 2004d…
Figure 8
Figure 8. Figure 8: Evolution of pseudo equivalent width v.s. velocity of Si ii λ6355 for SN 2019ein. For comparison, we plot those of SNe 2002bo (Benetti et al. 2004; Blondin et al. 2012; Silverman et al. 2012a), 2002dj (Pignata et al. 2008), 2002er (Kotak et al. 2005; Silverman et al. 2…
Figure 10
Figure 10. Figure 10: Optical light curves of SN 2019ein in the early phase. We also plot the discovery magnitude (the cross symbol, Tonry et al. 2019) and the data obtained by ZTF taken from the Transient Name Server. The red and blue open circles denote data in the r and g bands, respect…
Figure 11
Figure 11. Figure 11: Comparison of the observed spectra at −11.5 and −9.5 days (gray lines) to the synthesized spectra (red lines) calculated with TARDIS. These observed spectra are corrected for the MW and the host galaxy extinction. SN 2019ein has more extended distribution of the O-Ne-…
Figure 12
Figure 12. Figure 12: Comparison between the observed Si ii λ6355 at −11.5 days (gray line) and the synthesized spectra. The observed spectrum is corrected for the MW and the host galaxy extinction. (a) Shown here are models with different velocities at the interface between the burnt and …

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 2 Pith papers

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

  1. A Simulation Based Inference Approach to Modelling of Type Ia Supernova Populations

    astro-ph.CO 2026-07 conditional novelty 6.0 of 10

    A simulation-based inference pipeline (Stjörnumál) fits SN Ia dust and intrinsic scatter models to DES 5-year data, enabling fast Bayesian model comparison across seven SN Ia population models.

  2. Constraints on Dark Energy Models Using Late Universe Probes

    astro-ph.CO 2025-06 conditional novelty 4.0 of 10

    Using late-universe probes only, the authors find all dark energy models remain within 1-2 sigma of Lambda CDM, which wins the Bayesian model comparison, and confirm that DESI's LRG1 and LRG2 points drive the dynamica...

Reference graph

Works this paper leans on

89 extracted references · 75 canonical work pages · cited by 2 Pith papers

  1. [1]

    2014, in Society of Photo-Optical Instru mentation Engineers (SPIE) Conference Series, V ol

    Akitaya, H., et al. 2014, in Society of Photo-Optical Instru mentation Engineers (SPIE) Conference Series, V ol. 9147, Proc. SPIE, 91474O

    2014

  2. [2]

    2015, ApJS, 219, 12

    Alam, S., et al. 2015, ApJS, 219, 12

    2015

  3. [3]

    2004, MNRAS, 349, 1344 —

    Altavilla, G., et al. 2004, MNRAS, 349, 1344 —. 2007, A&A, 475, 585

    2004

  4. [4]

    Arnett, W. D. 1982, ApJ, 253, 785

    1982

  5. [5]

    C., & Armandro ff, T

    Barden, S. C., & Armandro ff, T. 1995, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 2476, Fiber Optics in Astronomical Applications, ed. S. C. Barden, 56–6 7 24 http://www.nhn.ou.edu/˜suspect/ 25 http://wiserep.weizmann.ac.il/

    1995

  6. [6]

    1994, in Society of Photo-Optical Instrumentati on Engineers (SPIE) Conference Series, V ol

    Groves, L. 1994, in Society of Photo-Optical Instrumentati on Engineers (SPIE) Conference Series, V ol. 2198, Instrumentation in Astronomy VIII, ed. D. L. Crawford & E. R. Craine, 87–97

    1994

  7. [7]

    2005, ApJ, 623, 1011 —

    Benetti, S., et al. 2005, ApJ, 623, 1011 —. 2004, MNRAS, 348, 261

    2005

  8. [8]

    B., et al

    Bianco, F. B., et al. 2011, ApJ, 741, 20

    2011

Show all 89 references
  1. [9]

    2012, AJ, 143, 126

    Blondin, S., et al. 2012, AJ, 143, 126

    2012

  2. [10]

    S., et al

    Bloom, J. S., et al. 2012, ApJL, 744, L17

    2012

  3. [11]

    2006, PASP, 118, 560

    Branch, D., et al. 2006, PASP, 118, 560

    2006

  4. [12]

    A., Landsman, W., Holland, S

    Breeveld, A. A., Landsman, W., Holland, S. T., Roming, P ., Kuin, N. P . M., & Page, M. J. 2011, in American Institute of Physics Conferen ce Series, V ol. 1358, American Institute of Physics Conference Series, ed. J. E

    2011

  5. [13]

    A., Hiramatsu, D., & McCull y, C

    Burke, J., Arcavi, I., Howell, D. A., Hiramatsu, D., & McCull y, C. 2019, Transient Name Server AstroNote, 8, 1

    2019

  6. [14]

    R., et al

    Burns, C. R., et al. 2011, AJ, 141, 19

    2011

  7. [15]

    J., et al

    Childress, M. J., et al. 2013, ApJ, 770, 29

    2013

  8. [16]

    2018, ApJ, 859, 24 Di Stefano, R., & Kilic, M

    Contreras, C., et al. 2018, ApJ, 859, 24 Di Stefano, R., & Kilic, M. 2012, ApJ, 759, 56

    2018

  9. [17]

    2019, ApJL, 870, L1

    Dimitriadis, G., et al. 2019, ApJL, 870, L1

    2019

  10. [18]

    2008, MNRAS, 384, 107

    Elias-Rosa, N., et al. 2008, MNRAS, 384, 107

    2008

  11. [19]

    2010, A&A, 514, A53

    Kromer, M. 2010, A&A, 514, A53

    2010

  12. [20]

    Foley, R. J. 2012, ApJ, 748, 127

    2012

  13. [21]

    J., et al

    Foley, R. J., et al. 2012, ApJ, 744, 38

    2012

  14. [22]

    J., & Kasen, D

    Foley, R. J., & Kasen, D. 2011, ApJ, 729, 55

    2011

  15. [23]

    J., Sanders, N

    Foley, R. J., Sanders, N. E., & Kirshner, R. P . 2011, ApJ, 742, 89

    2011

  16. [24]

    Ganeshalingam, M., Li, W., & Filippenko, A. V . 2011, MNRAS, 416, 2607

    2011

  17. [25]

    2007, A&A, 471, 527

    Garavini, G., et al. 2007, A&A, 471, 527

    2007

  18. [26]

    L., et al

    Gerardy, C. L., et al. 2004, ApJ, 607, 391

    2004

  19. [27]

    2015, ApJ, 799, 106

    Goobar, A., et al. 2015, ApJ, 799, 106

    2015

  20. [28]

    2012, ApJL, 756, L4

    Hachisu, I., Kato, M., & Nomoto, K. 2012, ApJL, 756, L4

    2012

  21. [29]

    T., et al

    Hayden, B. T., et al. 2010, ApJ, 712, 350

    2010

  22. [30]

    2018, arXiv e-prints, arXiv:1809.01359

    Holmbo, S., et al. 2018, arXiv e-prints, arXiv:1809.01359

    2018 arXiv

  23. [31]

    2017, ApJL, 845, L11

    Hosseinzadeh, G., et al. 2017, ApJL, 845, L11

    2017

  24. [32]

    A., Monard, L

    Im, M., Choi, C., Y oon, S.-C., Kim, J.-W., Ehgamberdiev, S. A., Monard, L. A. G., & Sung, H.-I. 2015, ApJS, 221, 22

    2015

  25. [33]

    R., & Thielemann, F.-K

    Iwamoto, K., Brachwitz, F., Nomoto, K., Kishimoto, N., Umed a, H., Hix, W. R., & Thielemann, F.-K. 1999, ApJS, 125, 439

    1999

  26. [34]

    2018, ApJ, 8 65, 149

    Jiang, J.-a., Doi, M., Maeda, K., & Shigeyama, T. 2018, ApJ, 8 65, 149

    2018

  27. [35]

    2017, Nature, 550, 80

    Jiang, J.-A., et al. 2017, Nature, 550, 80

    2017

  28. [36]

    2020, arXiv e-prints, arXiv:2002.1073 7

    Jiang, J.-a., et al. 2020, arXiv e-prints, arXiv:2002.1073 7

    2020

  29. [37]

    2011, ApJL, 730, L34

    Justham, S. 2011, ApJL, 730, L34

    2011

  30. [38]

    2010, ApJ, 708, 1025

    Kasen, D. 2010, ApJ, 708, 1025

    2010

  31. [39]

    S., et al

    Kawabata, K. S., et al. 2008, in Proc. SPIE, V ol. 7014, Ground -based and Airborne Instrumentation for Astronomy II, 70144L

    2008

  32. [40]

    2019, tardis-sn /tardis: TARDIS v3.0 alpha2

    Kerzendorf, W., et al. 2019, tardis-sn /tardis: TARDIS v3.0 alpha2

    2019

  33. [41]

    E., & Sim, S

    Kerzendorf, W. E., & Sim, S. A. 2014, MNRAS, 440, 387

    2014

  34. [42]

    2005, A&A, 436, 1021

    Kotak, R., et al. 2005, A&A, 436, 1021

    2005

  35. [43]

    2005, Nuovo Cimento C Geophysics Space Phy sics C, 28, 755 High-Velocity type Ia Supernov a2019ein 15

    Kotani, T., et al. 2005, Nuovo Cimento C Geophysics Space Phy sics C, 28, 755 High-Velocity type Ia Supernov a2019ein 15

    2005

  36. [44]

    2004, AJ, 128, 3034

    Krisciunas, K., et al. 2004, AJ, 128, 3034

    2004

  37. [45]

    2010, in Society of Photo-Optical Instrum entation Engineers (SPIE) Conference Series, V ol

    Kurita, M., et al. 2010, in Society of Photo-Optical Instrum entation Engineers (SPIE) Conference Series, V ol. 7733, Ground-based and Airborne Telescopes III, 77333E

    2010

  38. [46]

    2015, PASJ, 67, 54

    Kutsuna, M., & Shigeyama, T. 2015, PASJ, 67, 54

    2015

  39. [47]

    2018, ApJ, 8 61, 78

    Maeda, K., Jiang, J.-a., Shigeyama, T., & Doi, M. 2018, ApJ, 8 61, 78

    2018

  40. [48]

    2011, MNRAS, 413, 3075

    Maeda, K., et al. 2011, MNRAS, 413, 3075

    2011

  41. [49]

    H., et al

    Marion, G. H., et al. 2016, ApJ, 820, 92

    2016

  42. [50]

    2019, arXiv e-prints, arXiv:1905

    Matsubayashi, K., et al. 2019, arXiv e-prints, arXiv:1905. 05430

    2019

  43. [51]

    2005, A&A, 443, 649

    Leibundgut, B., & Nomoto, K. 2005, A&A, 443, 649

    2005

  44. [52]

    Mazzali, P . A. 2001, MNRAS, 321, 341

    2001

  45. [53]

    2005, MNRAS, 357, 200

    Nomoto, K., & Hamuy, M. 2005, MNRAS, 357, 200

    2005

  46. [54]

    A., Sauer, D

    Mazzali, P . A., Sauer, D. N., Pastorello, A., Benetti, S., & H illebrandt, W. 2008, MNRAS, 386, 1897

    2008

  47. [55]

    A., et al

    Mazzali, P . A., et al. 2014, MNRAS, 439, 1959

    2014

  48. [56]

    A., et al

    Miller, A. A., et al. 2018, ApJ, 852, 100

    2018

  49. [57]

    K., & Y okoi, K

    Nomoto, K., Thielemann, F. K., & Y okoi, K. 1984, ApJ, 286, 644

    1984

  50. [58]

    1995, ApJ, 455, L147

    Nugent, P ., Phillips, M., Baron, E., Branch, D., & Hauschild t, P . 1995, ApJ, 455, L147

    1995

  51. [59]

    E., et al

    Nugent, P . E., et al. 2011, Nature, 480, 344

    2011

  52. [60]

    P ., et al

    Olling, R. P ., et al. 2015, Nature, 521, 332

    2015

  53. [61]

    2013, A&A, 554, A27

    Pereira, R., et al. 2013, A&A, 554, A27

    2013

  54. [62]

    1998, Nature, 391, 51 —

    Perlmutter, S., et al. 1998, Nature, 391, 51 —. 1999, ApJ, 517, 565

    1998

  55. [63]

    E., Murphy, D

    Persson, S. E., Murphy, D. C., Krzeminski, W., Roth, M., & Rie ke, M. J. 1998, AJ, 116, 2475

    1998

  56. [64]

    Phillips, M. M. 1993, ApJL, 413, L105

    1993

  57. [65]

    2008, MNRAS, 388, 971 —

    Pignata, G., et al. 2008, MNRAS, 388, 971 —. 2004, MNRAS, 355, 178

    2008

  58. [66]

    L., Rest, A., & Suntze ff, N

    Prieto, J. L., Rest, A., & Suntze ff, N. B. 2006, ApJ, 647, 501

    2006

  59. [67]

    A., Sandage, A., & Saha, A

    Reindl, B., Tammann, G. A., Sandage, A., & Saha, A. 2005, ApJ, 624, 532

    2005

  60. [68]

    2001, in American Astronomical Socie ty Meeting Abstracts, V ol

    Baron, E., & Branch, D. 2001, in American Astronomical Socie ty Meeting Abstracts, V ol. 199, 84.08

    2001

  61. [69]

    G., et al

    Riess, A. G., et al. 1998, AJ, 116, 1009 —. 1999, AJ, 118, 2675

    1998

  62. [70]

    2014, MNRAS, 445, 711 Schlafly, E

    Cappellaro, E., & Benetti, S. 2014, MNRAS, 445, 711 Schlafly, E. F., & Finkbeiner, D. P . 2011, ApJ, 737, 103

    2014

  63. [71]

    J., et al

    Shappee, B. J., et al. 2019, ApJ, 870, 13 —. 2016, ApJ, 826, 144

    2019

  64. [72]

    M., & Pogge, R

    Lipunov, V . M., & Pogge, R. W. 2018, ApJ, 855, 6

    2018

  65. [73]

    A., Röpke, F

    Sim, S. A., Röpke, F. K., Hillebrandt, W., Kromer, M., Pakmor , R., Fink, M., Ruiter, A. J., & Seitenzahl, I. R. 2010, ApJL, 714, L52

    2010

  66. [74]

    2007, A&A, 469, 645

    Stanishev, V ., et al. 2007, A&A, 469, 645

    2007

  67. [75]

    2002, AJ, 124, 2100

    Stritzinger, M., et al. 2002, AJ, 124, 2100

    2002

  68. [76]

    D., et al

    Stritzinger, M. D., et al. 2018, ApJL, 864, L35

    2018

  69. [77]

    2008, ApJ, 677, 448

    Tanaka, M., et al. 2008, ApJ, 677, 448

    2008

  70. [78]

    A., Maeda, K., & Nomoto, K

    Tanaka, M., Mazzali, P . A., Maeda, K., & Nomoto, K. 2006, ApJ, 645, 470

    2006

  71. [79]

    2011, MNRAS, 410, 1725

    Nomoto, K. 2011, MNRAS, 410, 1725

    2011

  72. [80]

    2019, Transient Name Server Discovery Repo rt, 2019-678, 1 van Dokkum, P

    Tonry, J., et al. 2019, Transient Name Server Discovery Repo rt, 2019-678, 1 van Dokkum, P . G. 2001, PASP, 113, 1420 van Dokkum, P . G., Bloom, J., & Tewes, M. 2012, L.A.Cosmic: La placian Cosmic Ray Identification, Astrophysics Source Code Librar y

    2019

  73. [81]

    2018, arXiv e-prints, arXiv:1810.11936

    Wang, X., Chen, J., Wang, L., Hu, M., Xi, G., Y ang, Y ., Zhao, X., & Li, W. 2018, arXiv e-prints, arXiv:1810.11936

    2018 arXiv

  74. [82]

    2009, ApJ, 699, L139 —

    Wang, X., et al. 2009, ApJ, 699, L139 —. 2008, ApJ, 675, 626

    2009

  75. [83]

    V ., Zhang, T., & Zhao, X

    Wang, X., Wang, L., Filippenko, A. V ., Zhang, T., & Zhao, X. 2013, Science, 340, 170

    2013

  76. [84]

    2005, ApJL, 6 20, L87

    Wang, X., Wang, L., Zhou, X., Lou, Y .-Q., & Li, Z. 2005, ApJL, 6 20, L87

    2005

  77. [85]

    2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol

    Hamamoto, K., & Ozaki, A. 2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 8446, Proc. SPIE, 84462O Y amanaka, M., et al. 2014, ApJL, 782, L35 —. 2009, PASJ, 61, 713 Y aron, O., & Gal-Y am, A. 2012, PASP, 124, 668 Y oshida, M. 2005, J...

    2012

  78. [86]

    2016, ApJ, 820, 67

    Zhang, K., et al. 2016, ApJ, 820, 67

    2016

  79. [87]

    2010, PASP, 122, 1

    Zhang, T., et al. 2010, PASP, 122, 1

    2010

  80. [88]

    2016, ApJ, 826, 211

    Zhao, X., et al. 2016, ApJ, 826, 211

    2016

  81. [89]

    2014, ApJL, 783, L24 —

    Zheng, W., et al. 2014, ApJL, 783, L24 —. 2013, ApJL, 778, L15

    2014

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.