Pith. sign in

REVIEW 3 major objections 5 minor 298 references

This paper claims that early flux excesses appear in up to about a quarter of Type Ia supernovae, with over-luminous subtypes over-represented, and that the excesses are consistent with but do not decisively favor either companion-interacti

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 →

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

T0 review · deepseek-v4-flash

2026-08-01 05:55 UTC pith:NKE64WDB

load-bearing objection A genuinely useful census of early-excess SNe Ia whose 17 'robust' candidates include seven identified only by two methods that share a known under-prediction bias — the qualitative picture and the ≲25% upper limit survive, but the catalog needs revision. the 3 major comments →

arxiv 2607.22050 v1 pith:NKE64WDB submitted 2026-07-24 astro-ph.CO

ZTF SN Ia DR2 follow-up: early excess in Type Ia supernova light curves

Tom\'as E. M\"uller-Bravo , Kate Maguire , Alaa Alburai , Umut Burgaz , Georgios Dimitriadis , Llu\'is Galbany , Joel Johansson , Young-Lo Kim
show 10 more authors
Chang Liu Adam A. Miller Mathew Smith Jesper Sollerman Eric C. Bellm Joahan Castaneda Jaimes Mansi M. Kasliwal Russ R. Laher Roger Smith Niharika Sravan
This is my paper
classification astro-ph.CO
keywords early flux excessType Ia supernovaeZTF DR2light curvesdouble detonationcompanion interactionSALT2supernova progenitors
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.

Type Ia supernovae are thermonuclear explosions of white dwarfs, but how the explosion starts and what the companion star is remains unsettled. The first days of the light curve carry the answer, because any extra brightness there would betray a surviving companion or a helium shell detonation. This paper searches a large, uniform sample of nearly 1,800 supernovae for such early flux excesses using four comparison methods and two families of physical models. It establishes that early excess is not rare: roughly up to a quarter of all Type Ia supernovae show one, and over-luminous subtypes show it more often. The strongest bumps, about 10–17% of peak brightness, form a robust sample of 17 candidates whose properties hint at younger stellar populations.

Core claim

The paper's central claim is that early flux excess in Type Ia supernovae is a real and fairly common phenomenon, not a rare oddity. Combining four independent methods for detecting deviations from no-excess models, it finds 17 strong candidates, with the brightest excesses reaching roughly 10–17% of the g-band peak flux and lasting up to about four rest-frame days. Within a volume-limited subsample it estimates the fraction of early-excess supernovae at ≲25% of all SNe Ia, with 91T-like and 03fg-like over-luminous subtypes showing higher relative incidence than normal ones. When fitting double-detonation models, the excess candidates favor a white-dwarf core of about one solar mass, a low s

What carries the argument

The 'excess window' – the phase range from the first detection to a few days later, where an early bump would appear – is the central device. Data inside the window are excluded from the fits, and an excess is declared when at least two nights in the window deviate from a no-excess model by more than five times the error. The paper deploys four no-excess models (SALT2, a power law, a modified power law, and TURTLS 56Ni-distribution models) plus two excess-producing model grids (double-detonation and companion-interaction). For the latter, a supernova is flagged as an excess candidate when more than 90% of the acceptable best-fit models within a 3σ chi-squared interval show an excess.

Load-bearing premise

The whole identification rests on trusting the no-excess models – SALT2, the power laws, and the 56Ni-distribution grid – to predict what the light curve should look like in the very first days, and the paper itself notes that SALT2 over-predicts luminosities around −15 days, inside or near the window where an excess is claimed.

What would settle it

Take the 17 best candidates and refit them after removing all SALT2 epochs near −15 days, or replace SALT2 with a model built from early-time spectroscopy that shows no systemic over-prediction; if the five-sigma deviations in the excess window disappear, the excesses are model artifacts. Alternatively, obtain spectra of the candidates during the first nights after first detection and check for the blue continuum of companion interaction or the helium and iron-group lines of double detonation.

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

If this is right

  • If the estimate holds, early-excess supernovae are a substantial population – up to roughly one in four of all Type Ia supernovae – rather than a rare subclass, so any complete theory of SNe Ia must reproduce these bumps.
  • The higher relative incidence in 91T-like and 03fg-like over-luminous subtypes suggests the explosion mechanism itself, not just the environment, influences the presence and prominence of the excess.
  • The preference of the best candidates for higher stretch and lower-mass, bluer host galaxies connects early-excess events to younger stellar populations.
  • Double-detonation model fits pin down physical parameters: core mass near one solar mass, about 20% shell burning, and heavier helium-burning products, giving concrete targets for explosion simulations.
  • Because excesses are identified only after several rise epochs are in hand, real-time triggering of early spectroscopy is difficult; upcoming surveys will need high-cadence follow-up to catch these events while the bump is visible.

Where Pith is reading between the lines

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

  • I infer that the true rate for normal SNe Ia is likely below the 25% upper limit: the lower limit from the conservative candidates is about 2% and the companion-interaction upper limit is 27%, so the paper's headline number binds from above rather than pinning the rate.
  • The SALT2 over-prediction at about −15 days, which the authors flag, could create false 5σ deviations inside the excess window; a re-analysis with a model trained on early-time spectra would be the cleanest test of whether the 17 candidates survive.
  • The near lack of overlap between the double-detonation and companion-interaction candidate lists suggests the two scenarios leave distinguishable traces in the rise shape – so a dedicated sample with early color and spectroscopy could separate them even if this paper cannot.
  • The two-night, >5σ requirement excludes single-epoch excesses such as the one seen in supernova 2019yvq, so the paper's candidate list is conservative for sharp, short bumps; a companion search allowing one strong epoch plus color information could find additional events.

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 paper searches the ZTF DR2 SN Ia sample (1,792 objects after data cuts) for early flux excess (EEx). It uses two complementary approaches: (i) comparing early g-band light curves with four no-excess models (SALT2, simple power law, modified power law, and 56Ni-distribution TURTLS models) and requiring at least two nights with pull ≥ 5 inside a method-dependent 'excess window'; and (ii) fitting double-detonation (DD) and companion-interaction (CI) models and selecting objects with an early-excess probability > 0.9. The two approaches yield very different candidate sets, and the paper defines 17 'robust' candidates as those flagged by at least two of the four no-excess methods. These 17 are then used for rate estimates (≲25% of SNe Ia), for light-curve and host-galaxy comparisons (higher stretch, lower-mass bluer hosts), and for DD/CI model parameter trends. The paper concludes that no strong preference between the DD and CI explosion scenarios can be drawn.

Significance. If the 17-candidate list is secure, the paper provides a valuable systematic census of early-excess SNe Ia in a large, homogeneous sample, with a transparent multi-method comparison, visual/chip-level verification, and a large grid of TURTLS models. The public data and reproducible workflow are clear strengths. However, the central claim rests on a robustness criterion that does not protect against systematic biases shared by the methods used to define the sample; several quantitative conclusions (rate, host-property trends, model-parameter preferences) are sensitive to this issue. The paper's honest caveats mitigate but do not remove the concern.

major comments (3)
  1. [Section 5.3, Table 5] The '≥2 methods' criterion does not filter out bias shared by the modified power-law and 56Ni-distribution methods, both of which the paper itself reports as systematically under-predicting early flux (Sect. 4.1: MPL 'seems to vastly under-predict the underlying early SN flux in a systematic manner'; Sect. 5.1: ND 'does not seem to alleviate the issue of under-predicting early-time flux'). Since the pull statistic (Sect. 3.1) is (data − model)/photometric error, with no model-systematic term, systematic under-prediction directly produces positive ≥5σ pulls. Seven of the 17 robust candidates (ZTF18abtfvsk, ZTF18acxyarg, ZTF18acybdar, ZTF19abqhikf, ZTF19aclofmz, ZTF20aazquhc, ZTF20abeywdn) are flagged only by MPL+ND (Table 5), so their inclusion is not independent confirmation. Please rerun the robust-sample analysis after removing the MPL+ND pairing, or add a model-bias term to the pull a
  2. [Section 4.1] The excess-window durations are chosen post hoc to maximize candidate counts: SALT2 with a 4 d window 'maximises the number of identified EEx SNe Ia'; the power-law 3 d window 'seems to maximise' the count; MPL and ND use 2 d windows selected 'to be conservative'. This is a selection effect. The quoted 5σ pull threshold is not corrected for the number of windows and methods scanned, so the nominal significance of the reported candidate counts (15, 8, 27, 34) is unknown. The paper should provide a null calibration (e.g., no-excess mock light curves with the same model biases, or residual randomization) to show that these yields are not consistent with model bias plus window selection. Without this, the 17-object overlap cannot be interpreted as a controlled false-positive rate.
  3. [Sections 4.2 and 5.5] The DD/CI analysis both selects EEx candidates (probability > 0.9) and then interprets the best-fit parameter distributions of those same fits. The preference for WD core mass ~1 M⊙, 20% burning-shell fraction, and 56Ni as the dominant He-burning product (Fig. 11) is therefore partly a property of the model-selection path rather than an independent constraint on the explosion mechanism. The paper does state that no strong conclusions can be drawn, but the presentation should explicitly frame the parameter distributions as conditional on the DD/CI model selection. In addition, Sect. 4.2 states '27 EEx SN Ia candidates identified with both DD and CI models', while Sect. 5.5 says 'only 21 SNe' in common; this discrepancy needs to be resolved or explained.
minor comments (5)
  1. [Section 6] Typo: 'as the simple power law daos' should read '...does'.
  2. [Section 1] Typo: 'for constrains from early UV observations' should read 'for constraints'.
  3. [Section 2.2] The phrase 'two prior non-detections epochs' should be 'two prior non-detection epochs'.
  4. [Section 5.4] 'by using the two-samples Kolmogorov-Smirnov (KS) test' should be 'two-sample'.
  5. [Section 4.2] The definition of n_EE and n_No−EE could be stated more explicitly with equations; currently the text is a little hard to follow.

Circularity Check

1 steps flagged

DD/CI parameter 'preferences' inherit the model grid's excess definition; the 17-candidate detection claim itself is not circular, though shared model under-prediction is a bias risk.

specific steps
  1. self definitional [Sect. 5.5 (Fig. 11); selection in Sect. 4.2; model-excess definition in Sect. 3.4.2 (Fig. 5)]
    "It can be seen that, considering the available parameter space, EEx SNe Ia have a preference for DD models with WD core mass 1M⊙, a lower fraction of shell burning (20%) and heavier He-burning products (56Ni)."

    The EEx candidates analyzed here are selected in Sect. 4.2 as SNe whose best-fit DD/CI models are dominated by models with early excess (probability > 0.9). In the same DD model grid, the presence of early excess is defined by the same parameters: 'those with lighter intermediate-mass elements... do not show early excess', and excess is seen mainly for WD core masses below 1.2 M⊙ and products at least as heavy as 44Ti (Sect. 3.4.2, Fig. 5). Hence the reported preference for heavier He-burning products, and partly for lower core mass, is a restatement of the grid's excess definition rather than an independent empirical constraint. The paper itself notes that 'the physical parameters that affect the early excess of the models also affect the overall shape of the light curves' (Sect. 5.1), so

full rationale

The central EEx detection claim does not reduce to a fit: the four no-excess methods (SALT2, PL, MPL, ND) fit only data outside the excess window, and the excess is a residual (pull) against those fits; the 17 'robust' candidates are then defined by agreement among these methods. That definition can be criticized — the paper admits MPL and ND systematically under-predict early flux, so the seven MPL+ND-only candidates may share a model bias rather than an astrophysical excess — but this is a model-validity/bias concern, not a circularity, because the excess is not by construction equal to any fitted parameter. The one genuinely self-referential element is the DD/CI parameter analysis: candidates are selected using the DD/CI models, and the reported DD 'preference' for heavier He-burning products and lower core masses mirrors the same grid's built-in definition of which models show early excess, so those parameter distributions do not independently constrain the explosion mechanism. The paper itself hedges this ('we cannot say a priori whether the early excess...'; 'unable to draw strong conclusions'), which limits the circularity's impact. No load-bearing self-citation was found; the SALT2 behavior cited from Rigault et al. (2025b) is used as a caveat, not as proof.

Axiom & Free-Parameter Ledger

4 free parameters · 6 axioms · 0 invented entities

The central claim depends on numerous hand-chosen thresholds (excess window, pull, probability) and on domain assumptions about early-phase model reliability, K-corrections, and the adequacy of the DD/CI grids. No new physical entities are postulated. The free parameters are detection criteria rather than physical constants fitted to data.

free parameters (4)
  • excess_window_duration_per_method
    Chosen per method to maximize the number of EEx candidates (e.g., SALT2: 4 d, power-law: 3 d, modified PL: 2 d, 56Ni-dist: 2 d; Sect. 4.1). This is a hand-tuned detection threshold on the same data.
  • pull_threshold = 5
    Required 5σ deviation in at least two nights to flag an excess (Sect. 3.1). Hand-chosen to reduce false positives.
  • flux_excess_probability_threshold = 0.9
    For DD/CI models, candidates are those with probability >0.9; authors call the choice 'somewhat arbitrary' (Sect. 4.2).
  • tfd_detection_criteria = 3σ + two non-detections
    Definitions of time of first detection (Sect. 2.2) rely on hand-set significance and non-detection counts, influencing the excess window and epochs available.
axioms (6)
  • domain assumption SNe Ia without early excess are well described by SALT2/power-law/TURTLS models at early phases
    The detection of excess is defined as deviation from these models (Sects. 3.2–3.4.1); if models are systematically wrong at φ≲−15 d, detections may be artifacts.
  • domain assumption K-corrections are negligible for z≲0.1
    The authors state K-corrections are not applied because of SED uncertainties, citing Liu et al. (in prep.) for the z≲0.1 claim (Sect. 2.2).
  • domain assumption Early excess appears primarily in the g band
    All no-excess methods use g-band data; r-band is only inspected for a subset (Sect. 3.1).
  • domain assumption DD and CI model grids (Magee et al. 2021; Magee et al. 2022) adequately cover the EEx parameter space and their model light curves are reliable
    Used to classify candidates and to interpret parameter preferences (Sects. 3.4.2, 5.5).
  • standard math Flat ΛCDM cosmology with H0=70 km/s/Mpc, Ωm=0.3 for distances
    Used for distance modulus initial guesses and absolute magnitudes (Sects. 3.4.1, 5.4, footnote 11).
  • domain assumption SALT2 over-prediction around φ∼−15 d is a training-set bias, not an astrophysical signal
    The paper relies on this to justify excluding the window and to interpret 3σ agreement checks (Sect. 3.2).

pith-pipeline@v1.3.0-alltime-deepseek · 29165 in / 12697 out tokens · 119880 ms · 2026-08-01T05:55:19.911928+00:00 · methodology

0 comments
read the original abstract

There is broad consensus that Type Ia supernovae (SNe Ia) are the thermonuclear explosions of C/O white dwarfs (WDs) in binary systems, but their progenitors and explosion mechanisms remain uncertain. Their earliest light curves probe the outermost ejecta and provide important constraints on the explosion. We analyse the ZTF DR2 sample of SNe Ia to search for objects exhibiting early flux excess (EEx SNe Ia). We employ two complementary approaches: (i) identifying deviations from models without early excess using power-law and SALT2 fits, and (ii) comparing observations with double-detonation (DD) and companion-interaction (CI) models. The latter identify 145 and 199 candidates, respectively, although the methods disagree substantially on both the objects selected and the total number of candidates. Combining all methods, we identify 17 robust EEx SN Ia candidates, including six over-luminous events (five 91T-like and one 03fg-like). The strongest excesses reach ${\sim}10$--17\% of the peak flux. The best candidates have, on average, higher stretch and preferentially occur in lower-mass, bluer host galaxies, suggesting younger stellar populations. We estimate that EEx SNe Ia comprise $\lesssim25\%$ of all SNe Ia, consistent with previous work, with over-luminous subtypes showing a higher relative incidence than normal SNe Ia. Among the DD models, the preferred solutions favour intermediate WD core masses ($1 M_{\odot}$), low shell-burning fractions ($20\%$), and heavier He-burning products ($^{56}$Ni), whereas the CI models show no clear parameter trends. Overall, we find no compelling evidence that either scenario is preferred as the origin of the observed early flux excesses.

Figures

Figures reproduced from arXiv: 2607.22050 by Adam A. Miller, Alaa Alburai, Chang Liu, Eric C. Bellm, Georgios Dimitriadis, Jesper Sollerman, Joahan Castaneda Jaimes, Joel Johansson, Kate Maguire, Llu\'is Galbany, Mansi M. Kasliwal, Mathew Smith, Niharika Sravan, Roger Smith, Russ R. Laher, Tom\'as E. M\"uller-Bravo, Umut Burgaz, Young-Lo Kim.

Figure 1
Figure 1. Figure 1: Pseudo-rise time, i.e. rest-frame time from [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: ZTF gri rest-frame light curves of ZTF18abxxssh. Top: opaque circles are epochs included in the SALT2 fit, while semi￾transparent circles are epochs not included (see Sect. 3.2). Solid lines represent the best-fitting SALT2 model. The vertical dot￾ted blue lines mark the bounds of the ‘excess window’(ϕ ∈ [tfd, tfd + 5] d in this case). Bottom: semi-transparent circles in ϕ ∈ [tfd + 5, −10] d (i.e. to the r… view at source ↗
Figure 3
Figure 3. Figure 3: ZTF gr rest-frame light curves of ZTF18abxxssh. Top: opaque circles are epochs included in the power-law fit (see Sect. 3.3), while semi-transparent circles are epochs not included as they fall in the excess window. The vertical lines mark the time of first light (tfl; dashed orange line) and the excess window boundaries (ϕ ∈ [tfd, tfd + 3] d in this case; dotted blue lines). Bottom: opaque circles fall in… view at source ↗
Figure 4
Figure 4. Figure 4: ZTF gri rest-frame light curves of ZTF18abxxssh. Top: best-fit 56Ni-distribution model from Sect. 3.4.1 for this SN. Best fit values are also shown in the plot with the initial values in parentheses. Semi-transparent circles are epochs not included in the fit as they fall in the excess window. Bottom: best-fit light￾curve residual (i.e. pull). Opaque circles are epochs in the excess window used to identify… view at source ↗
Figure 5
Figure 5. Figure 5: Parameter distributions for the double-detonation models from Magee et al. (2021). In blue and red are the models with and without early flux excess, respectively. 1.0 1.5 Kinetic Energy (10 51 erg) 0.0 2.5 5.0 7.5 10.0 12.5 15.0 No excess Excess 1 2 log10(a=10 11cm) 0 2 4 6 8 10 12 0 50 100 150 µ(°) 0 2 4 6 8 10 12 Companion Interaction Number of models [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Parameter distributions for the companion-interaction models from Magee et al. (2022). In blue and red are the models with (s = 9.7) and without (s = 3) early flux excess, respectively. Note that the parameter distributions are the same between those models with and without early excess. models whose parameters are within ∆χ 2 = χ 2 − χ 2 min∼16.257 . An example of the best-fit DD and CI parameters/models … view at source ↗
Figure 7
Figure 7. Figure 7: ZTF gri rest-frame light curves of ZTF18abxxssh. The best-fit models (semi-transparent dashed lines), with the num￾ber of models included (N), and the best-fit model (i.e., low￾est χ 2 ; solid lines) are shown for the double-detonation (left) and companion-interaction (right) models (see Sect. 3.4.2). The residuals are with respect to the best-fit model to help visualise whether the models are a good appro… view at source ↗
Figure 8
Figure 8. Figure 8: Flux excess probability for the SNe Ia in our sample, [PITH_FULL_IMAGE:figures/full_fig_p008_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Number of g-band epochs (unique nights; top) and av￾erage rest-frame cadence (bottom) during the light-curve rise of EEx SN Ia candidates in this work. The light-curve rise is con￾sidered between tfd and t0. The median rest-frame cadence of the EEx SNe Ia is ∼1.5 d. Note that the power-law method actually uses data up to the time of 50% of g-band peak flux (Sect. 3.3), which translate to a lower number of … view at source ↗
Figure 10
Figure 10. Figure 10: Distributions of light-curve parameters and host properties for the non-EEx SNe Ia (assuming the DD model; grey circles) [PITH_FULL_IMAGE:figures/full_fig_p011_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Parameter distributions for the best-fit [PITH_FULL_IMAGE:figures/full_fig_p011_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Parameter distributions for the best-fit [PITH_FULL_IMAGE:figures/full_fig_p012_12.png] view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

298 extracted references · 30 canonical work pages · 1 internal anchor

  1. [1]

    arXiv , author =:1811.02374 , journal =

    doi:10.3847/2041-8213/ab04fa , eid =. arXiv , author =:1811.02374 , journal =

    Pith/arXiv arXiv 2041

  2. [2]

    doi:10.1093/mnras/stx721 , eprint =

    , keywords =. doi:10.1093/mnras/stx721 , eprint =

    doi:10.1093/mnras/stx721

  3. [3]

    doi:10.1093/mnras/stv1505 , eprint =

    , keywords =. doi:10.1093/mnras/stv1505 , eprint =

    doi:10.1093/mnras/stv1505

  4. [4]

    Fast Direct Methods for Gaussian Processes , volume =

    S. Fast Direct Methods for Gaussian Processes , volume =. IEEE Transactions on Pattern Analysis and Machine Intelligence , number =

  5. [5]

    , keywords =

    ZTF SN Ia DR2: Simulations and volume-limited sample. , keywords =. doi:10.1051/0004-6361/202452134 , archivePrefix =. 2409.04650 , primaryClass =

    Pith/arXiv arXiv

  6. [6]

    doi:10.1093/mnras/stz1321 , eprint =

    , keywords =. doi:10.1093/mnras/stz1321 , eprint =

    doi:10.1093/mnras/stz1321

  7. [7]

    doi:10.1086/159681 , journal =

    doi:10.1086/159681

  8. [8]

    , keywords =

    Hubble's constant and exploding carbon-oxygen white dwarf models for Type I supernovae. , keywords =. doi:10.1038/314337a0 , adsurl =

    doi:10.1038/314337a0

  9. [9]

    , keywords =

    A Physical Basis for the H-band Blue-edge Velocity and Light-curve Shape Correlation in Context of Type Ia Supernova Explosion Physics. , keywords =. doi:10.3847/1538-4357/ab204b , archivePrefix =. 1904.01633 , primaryClass =

    Pith/arXiv arXiv 1904

  10. [10]

    , keywords =

    Carnegie Supernova Project-II: Using Near-infrared Spectroscopy to Determine the Location of the Outer ^ 56 Ni in Type Ia Supernovae. , keywords =. doi:10.3847/2041-8213/ab1654 , archivePrefix =. 1902.10088 , primaryClass =

    Pith/arXiv arXiv 2041

  11. [11]

    arXiv , author =:2003.11121 , journal =

    doi:10.3847/2041-8213/ab8e37 , eid =. arXiv , author =:2003.11121 , journal =

    Pith/arXiv arXiv 2041

  12. [12]

    doi:10.1051/0004-6361:20054185 , eprint =

    , keywords =. doi:10.1051/0004-6361:20054185 , eprint =

    doi:10.1051/0004-6361:20054185

  13. [13]

    arXiv , Author =:1307.6212 , Journal =

    doi:10.1051/0004-6361/201322068 , Eid =. arXiv , Author =:1307.6212 , Journal =

    Pith/arXiv arXiv

  14. [14]

    , keywords =

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    Pith/arXiv arXiv

  15. [15]

    , keywords =

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package. , keywords =. doi:10.3847/1538-4357/ac7c74 , archivePrefix =. 2206.14220 , primaryClass =

    Pith/arXiv arXiv

  16. [16]

    arXiv , author =:1902.03261 , journal =

    doi:10.3847/1538-4357/ab2a16 , eid =. arXiv , author =:1902.03261 , journal =

    Pith/arXiv arXiv 1902

  17. [17]

    doi:10.1086/671198 , journal =

    doi:10.1086/671198

  18. [18]

    doi:10.5281/zenodo.804967 , eid =

    doi:10.5281/zenodo.804967

  19. [20]

    doi:10.1088/1538-3873/aaecbe , eprint =

    , keywords =. doi:10.1088/1538-3873/aaecbe , eprint =

    doi:10.1088/1538-3873/aaecbe

  20. [21]

    doi:10.1086/132749 , journal =

    doi:10.1086/132749

  21. [22]

    arXiv , author =:1401.4064 , journal =

    doi:10.1051/0004-6361/201423413 , eid =. arXiv , author =:1401.4064 , journal =

    Pith/arXiv arXiv

  22. [23]

    doi:10.1086/520494 , eprint =

    , keywords =. doi:10.1086/520494 , eprint =

    doi:10.1086/520494

  23. [24]

    doi:10.1093/mnras/sts484 , eprint =

    , keywords =. doi:10.1093/mnras/sts484 , eprint =

    doi:10.1093/mnras/sts484

  24. [25]

    , keywords =

    A Compact Degenerate Primary-star Progenitor of SN 2011fe. , keywords =. doi:10.1088/2041-8205/744/2/L17 , archivePrefix =. 1111.0966 , primaryClass =

    Pith/arXiv arXiv 2041

  25. [26]

    doi:10.1086/425880 , journal =

    work page doi:10.1086/425880

  26. [27]

    arXiv , author =:2105.02204 , journal =

    Pith/arXiv arXiv

  27. [28]

    doi:10.1093/mnras/staa2485 , eprint =

    , keywords =. doi:10.1093/mnras/staa2485 , eprint =

    doi:10.1093/mnras/staa2485

  28. [29]

    arXiv , author =:1811.02378 , journal =

    doi:10.3847/1538-4357/ab06c1 , eid =. arXiv , author =:1811.02378 , journal =

    Pith/arXiv arXiv

  29. [30]

    arXiv , author =:2004.10206 , journal =

    doi:10.3847/1538-4357/abd69b , eid =. arXiv , author =:2004.10206 , journal =

    Pith/arXiv arXiv 2004

  30. [31]

    , keywords =

    Constraints on Type Ia Supernova Progenitor Companions from Early Ultraviolet Observations with Swift. , keywords =. doi:10.1088/0004-637X/749/1/18 , archivePrefix =. 1203.5315 , primaryClass =

    Pith/arXiv arXiv

  31. [32]

    , keywords =

    A Swift Look at SN 2011fe: The Earliest Ultraviolet Observations of a Type Ia Supernova. , keywords =. doi:10.1088/0004-637X/753/1/22 , archivePrefix =. 1110.2538 , primaryClass =

    Pith/arXiv arXiv

  32. [33]

    ZTF Early Observations of Type Ia Supernovae. III. Early-time Colors As a Test for Explosion Models and Multiple Populations. , keywords =. doi:10.3847/1538-4357/abb13c , archivePrefix =. 2001.00587 , primaryClass =

    Pith/arXiv arXiv 2001

  33. [34]

    , keywords =

    ZTF SN Ia DR2: Properties of the low-mass host galaxies of Type Ia supernovae in a volume-limited sample. , keywords =. doi:10.1051/0004-6361/202452571 , archivePrefix =. 2412.14262 , primaryClass =

    Pith/arXiv arXiv

  34. [35]

    , keywords =

    A Bright Ultraviolet Excess in the Transitional 02es-like Type Ia Supernova 2019yvq. , keywords =. doi:10.3847/1538-4357/ac126b , archivePrefix =. 2101.06345 , primaryClass =

    Pith/arXiv arXiv

  35. [36]

    arXiv e-prints , keywords =

    Companion Shocking Fits to the 2018 ZTF Sample of SNe Ia Are Consistent with Single-Degenerate Progenitor Systems. arXiv e-prints , keywords =. doi:10.48550/arXiv.2208.11201 , archivePrefix =. 2208.11201 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2208.11201 2018

  36. [37]

    arXiv , author =:1010.4040 , journal =

    doi:10.1088/0004-6256/141/1/19 , eid =. arXiv , author =:1010.4040 , journal =

    Pith/arXiv arXiv

  37. [38]

    arXiv , author =:1405.3934 , journal =

    doi:10.1088/0004-637X/789/1/32 , eid =. arXiv , author =:1405.3934 , journal =

    Pith/arXiv arXiv

  38. [39]

    arXiv , author =:1809.06381 , journal =

    doi:10.3847/1538-4357/aae51c , eid =. arXiv , author =:1809.06381 , journal =

    Pith/arXiv arXiv

  39. [40]

    The Astronomer's Telegram , year = 2021, month = mar, volume =

    Introducing POISE: Precision Observations of Infant Supernova Explosions. The Astronomer's Telegram , year = 2021, month = mar, volume =

    2021

  40. [41]

    arXiv , author =:2404.04724 , journal =

    doi:10.3847/1538-4357/ad3c45 , eid =. arXiv , author =:2404.04724 , journal =

    Pith/arXiv arXiv

  41. [42]

    Supernovae as Distance Indicators , doi =

  42. [43]

    arXiv , author =:1211.4480 , journal =

    doi:10.1088/0004-637X/763/2/88 , eid =. arXiv , author =:1211.4480 , journal =

    Pith/arXiv arXiv

  43. [44]

    doi:10.1086/167900 , journal =

    doi:10.1086/167900

  44. [45]

    doi:10.1093/mnras/sty2405 , eprint =

    , keywords =. doi:10.1093/mnras/sty2405 , eprint =

    work page doi:10.1093/mnras/sty2405

  45. [46]

    arXiv , author =:1312.3342 , journal =

    doi:10.1088/0004-637X/789/1/89 , eid =. arXiv , author =:1312.3342 , journal =

    Pith/arXiv arXiv

  46. [47]

    doi:10.21105/joss.00045 , eid =

    The Journal of Open Source Software , month =. doi:10.21105/joss.00045 , eid =

    doi:10.21105/joss.00045

  47. [48]

    doi:10.1086/150102 , journal =

    doi:10.1086/150102

  48. [49]

    arXiv , author =:1104.1443 , journal =

    doi:10.1088/0067-0049/192/1/1 , eid =. arXiv , author =:1104.1443 , journal =

    Pith/arXiv arXiv

  49. [50]

    doi:10.1086/588518 , eprint =

    The Astrophysical Journal , keywords =. doi:10.1086/588518 , eprint =

    doi:10.1086/588518

  50. [51]

    Synthetic observables

    Double detonations: variations in Type Ia supernovae due to different core and He shell masses - II. Synthetic observables. , keywords =. doi:10.1093/mnras/stac2665 , archivePrefix =. 2209.04305 , primaryClass =

    Pith/arXiv arXiv

  51. [52]

    doi:10.1088/0004-6256/139/2/519 , eprint =

    The Astronomical Journal , keywords =. doi:10.1088/0004-6256/139/2/519 , eprint =

    doi:10.1088/0004-6256/139/2/519

  52. [54]

    doi:10.21105/joss.00024 , journal =

    doi:10.21105/joss.00024

  53. [55]

    , keywords =

    Constraining Type Ia supernova explosions and early flux excesses with the Zwicky Transient Factory. , keywords =. doi:10.1093/mnras/stac558 , archivePrefix =. 2202.12914 , primaryClass =

    Pith/arXiv arXiv

  54. [56]

    arXiv , author =:2406.05060 , journal =

    doi:10.48550/arXiv.2406.05060 , eid =. arXiv , author =:2406.05060 , journal =

    Pith/arXiv arXiv doi:10.48550/arxiv.2406.05060

  55. [57]

    doi:10.1093/mnras/stx2300 , eprint =

    , keywords =. doi:10.1093/mnras/stx2300 , eprint =

    work page doi:10.1093/mnras/stx2300

  56. [58]

    arXiv , author =:2008.04923 , journal =

    doi:10.1088/1538-3873/ab4ca2 , eid =. arXiv , author =:2008.04923 , journal =

    arXiv 2008

  57. [59]

    , keywords =

    Constraints on the explosion mechanism and progenitors of Type Ia supernovae. , keywords =. doi:10.1093/mnras/stu598 , archivePrefix =. 1310.7747 , primaryClass =

    Pith/arXiv arXiv

  58. [60]

    doi:10.1093/mnras/stu2716 , eprint =

    , keywords =. doi:10.1093/mnras/stu2716 , eprint =

    work page doi:10.1093/mnras/stu2716

  59. [61]

    arXiv , author =:1707.00715 , journal =

    doi:10.1051/0004-6361/201731501 , eid =. arXiv , author =:1707.00715 , journal =

    Pith/arXiv arXiv

  60. [62]

    , keywords =

    K2 Observations of SN 2018oh Reveal a Two-component Rising Light Curve for a Type Ia Supernova. , keywords =. doi:10.3847/2041-8213/aaedb0 , archivePrefix =. 1811.10061 , primaryClass =

    Pith/arXiv arXiv 2041

  61. [63]

    , keywords =

    ZTF SN Ia DR2: The diversity and relative rates of the thermonuclear supernova population. , keywords =. doi:10.1051/0004-6361/202451852 , archivePrefix =. 2406.01434 , primaryClass =

    arXiv

  62. [64]

    arXiv , author =:2103.01183 , journal =

    doi:10.1088/1361-6382/ac086d , eid =. arXiv , author =:2103.01183 , journal =

    Pith/arXiv arXiv

  63. [65]

    doi:10.1093/mnras/stae2501 , eprint =

    , keywords =. doi:10.1093/mnras/stae2501 , eprint =

    doi:10.1093/mnras/stae2501

  64. [66]

    arXiv , author =:2311.06178 , journal =

    doi:10.3847/1538-4357/ad1ff5 , eid =. arXiv , author =:2311.06178 , journal =

    Pith/arXiv arXiv

  65. [67]

    doi:10.1111/j.1365-2966.2006.10430.x , eprint =

    , keywords =. doi:10.1111/j.1365-2966.2006.10430.x , eprint =

    arXiv 2006

  66. [68]

    doi:10.1111/j.1365-2966.2007.12638.x , eprint =

    , keywords =. doi:10.1111/j.1365-2966.2007.12638.x , eprint =

    arXiv 2007

  67. [69]

    doi:10.1086/183683 , journal =

    work page doi:10.1086/183683

  68. [70]

    doi:10.1086/163456 , journal =

    doi:10.1086/163456

  69. [71]

    doi:10.1086/524981 , eprint =

    , keywords =. doi:10.1086/524981 , eprint =

    work page doi:10.1086/524981

  70. [72]

    doi:10.1086/670067 , eprint =

    , keywords =. doi:10.1086/670067 , eprint =

    doi:10.1086/670067

  71. [73]

    doi:10.1086/190440 , journal =

    doi:10.1086/190440

  72. [74]

    , keywords =

    Early-time Light Curves of Type Ia Supernovae Observed with TESS. , keywords =. doi:10.3847/1538-4357/abcd42 , archivePrefix =. 1904.02171 , primaryClass =

    Pith/arXiv arXiv 1904

  73. [75]

    doi:10.1086/186252 , journal =

    doi:10.1086/186252

  74. [76]

    doi:10.1086/116339 , journal =

    doi:10.1086/116339

  75. [77]

    doi:10.1146/annurev.astro.35.1.309 , journal =

    doi:10.1146/annurev.astro.35.1.309

  76. [78]

    , keywords =

    Double-detonation sub-Chandrasekhar supernovae: can minimum helium shell masses detonate the core?. , keywords =. doi:10.1051/0004-6361/200913892 , archivePrefix =. 1002.2173 , primaryClass =

    Pith/arXiv arXiv

  77. [79]

    doi:10.1093/mnras/stu2314 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stu2314 , eprint =

    doi:10.1093/mnras/stu2314

  78. [80]

    doi:10.1086/316293 , eprint =

    , keywords =. doi:10.1086/316293 , eprint =

    doi:10.1086/316293

  79. [81]

    doi:10.1088/0004-6256/139/1/120 , eprint =

    , keywords =. doi:10.1088/0004-6256/139/1/120 , eprint =

    doi:10.1088/0004-6256/139/1/120

  80. [82]

    , keywords =

    SN 2006bt: A Perplexing, Troublesome, and Possibly Misleading Type Ia Supernova. , keywords =. doi:10.1088/0004-637X/708/2/1748 , archivePrefix =. 0912.0263 , primaryClass =

    Pith/arXiv arXiv

Showing first 80 references.