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arxiv: 2605.06799 · v2 · submitted 2026-05-07 · 🌌 astro-ph.CO · astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

On the origin of the environmental step: A BayeSN view of the ZTF SN Ia DR2

Madeleine Ginolin , Matthew Grayling , Kaisey S. Mandel , Maximilian Autenrieth , Benjamin M. Boyd , Aaron Do , Lisa Kelsey , Matthew O'Callaghan
Authors on Pith no claims yet

Pith reviewed 2026-05-12 03:29 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA
keywords Type Ia supernovaeenvironmental stepBayeSNHubble residualsdust extinctionZTF DR2stellar massdark energy
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The pith

BayeSN analysis of ZTF supernovae data shows the environmental magnitude step is intrinsic to the explosions rather than caused by dust.

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

The paper applies the hierarchical Bayesian BayeSN model to a volume-limited sample of Type Ia supernovae from the ZTF DR2 catalog. It first confirms a clear step in standardized absolute magnitude that correlates with host-galaxy proxies such as global stellar mass and local color, with the step size matching results from the SALT fitter. The model is then extended to allow both an intrinsic magnitude offset between environments and environment-dependent dust extinction; the step persists at high significance while the mean R_V values show no meaningful difference across environments. This finding matters because astrophysical variations in supernovae are now the dominant systematic uncertainty when using them to measure the dark-energy equation-of-state parameter w.

Core claim

Using a new training of BayeSN we obtain smaller Hubble-residual scatter than with SALT. When the model simultaneously includes an intrinsic magnitude step and differing dust properties, we recover a posteriori steps of 0.103±0.018 mag (5.6σ) for global stellar mass and 0.085±0.019 mag (4.5σ) for local color. The means of the R_V distributions remain similar between environments, with differences ≤0.2 and significances 0.6σ to 1.2σ. This constitutes a strong signal that SN Ia absolute magnitude depends intrinsically on environment.

What carries the argument

The extended BayeSN hierarchical Bayesian model for SN Ia SEDs that jointly fits an intrinsic magnitude step and environment-dependent dust parameters (R_V distributions).

If this is right

  • The magnitude step is independent of the choice of light-curve fitter (SALT versus BayeSN).
  • Dust properties do not differ significantly across host environments at the precision of the current sample.
  • Accounting for the intrinsic step reduces scatter in Hubble residuals and therefore tightens cosmological constraints.
  • Population-level studies with large surveys can isolate intrinsic supernova variations from observational systematics.

Where Pith is reading between the lines

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

  • Future standardization pipelines for next-generation surveys may need to treat host-galaxy environment as an explicit standardization parameter rather than a post-hoc correction.
  • If the intrinsic step is confirmed, it could be used to test whether SN Ia progenitor channels vary systematically with galaxy type or metallicity.
  • Repeating the analysis on other large datasets (e.g., LSST or Roman) would test whether the result is universal or survey-specific.

Load-bearing premise

The BayeSN model accurately separates intrinsic supernova properties from dust extinction without residual biases or unmodeled correlations between environment and other parameters.

What would settle it

A larger independent sample in which the magnitude step vanishes once the same extended BayeSN model is applied, or a direct spectroscopic measurement of progenitor or explosion properties showing no environment dependence.

Figures

Figures reproduced from arXiv: 2605.06799 by Aaron Do, Benjamin M. Boyd, Kaisey S. Mandel, Lisa Kelsey, Madeleine Ginolin, Matthew Grayling, Matthew O'Callaghan, Maximilian Autenrieth.

Figure 1
Figure 1. Figure 1: BayeSN fit of a randomly selected ZTF SN. The solid lines are the posterior mean of the model, while the shaded bands show the standard deviation of the chains. The final sample comprises 932 objects. The list of every SN passing the cuts is available on GitHub 2 . We note that some objects were discarded from the sample on the basis of bad or extrapolated SALT fits, which might not be the case with BayeSN… view at source ↗
Figure 3
Figure 3. Figure 3: Histogram of BayeSN 𝜃1. The full sample is plotted in grey, while the blue and red distribution correspond to SNe in locally blue and red environment, as defined in Sec. 4.2.1. To showcase both the population spread and the posterior uncertainty on 𝜃1 for individual SNe, we use values from the full MCMC chains, minus warm-up, which results in 1,000 steps per SN. 4.1 Distribution of the parameters We now lo… view at source ↗
Figure 2
Figure 2. Figure 2: Example of a ’bad’ BayeSN fit, defined as having an error on distance moduli larger than 𝜇err > 0.2. 3.3 Preprocessing of the light curves In order to use the publicly available light curves, some preprocessing is needed. The first step is to output the light curves at a zero point of ZP = 27.5, to match the value expected by BayeSN. We then apply the quality cuts used in Rigault et al. (2025), as implemen… view at source ↗
Figure 4
Figure 4. Figure 4: Top: Histogram of BayeSN 𝐴𝑉 . Bottom: 𝐴𝑉 distributions for dustless and dusty subsamples, as defined in Sec. 4.2.2. average 𝜃1, in the ZTF sample compared to the BayeSN training sample. 4.1.2 Dust extinction 𝐴𝑉 We plot on the top of [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 6
Figure 6. Figure 6: SALT stretch 𝑥1 against BayeSN 𝜃1. Note that the 𝑥1 axis is reversed. noted in Ginolin et al. (2025a), the dustless sample seems to still be affected by dust, as some of the 𝐴𝑉 values depart from 0. This is true if 𝐴𝑉 only encapsulates dust effect, and none of the intrinsic colour scatter present in the ZTF sample, as investigated in Sec. 4.3. The direct determination of 𝐴𝑉 made possible by BayeSN could le… view at source ↗
Figure 7
Figure 7. Figure 7: Standardised SALT Hubble residuals against BayeSN Hubble resid￾uals, as described in Sec. 4.4. with the Gaussian intrinsic colour distribution fitted in Ginolin et al. (2025a), of width 0.030 ± 0.005 and mean −0.085 ± 0.004. There is also a strong inverse correlation between 𝜃1 and 𝑥1, which however seems non-linear, as visible in [PITH_FULL_IMAGE:figures/full_fig_p006_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Hubble residuals for BayeSN light curve fits, as computed in Sec. 4.4, against host global stellar mass. The blue points are the mean residuals per bins of global mass. The bins are equally spaced, except for the edge ones that are slightly larger to encompass all points. The ’a poste￾riori’ step model (see Sec. 4.5) is illustrated in the blue dashed line, while the full line shows the step model when conv… view at source ↗
Figure 10
Figure 10. Figure 10: Hubble residuals, computed as described Sec. 4.4, against BayeSN 𝜃1 (top) and SALT 𝑥1 (bottom). The grey points are individual SNe and the blue points are binned averages, with the errorbars denoting the error on the mean. This adds three hyperparameters to the model, 𝛼high, 𝛼low and 𝜃 break 1 . C is a constant that ensures continuity, and its value is fully deter￾mined by the set of (𝛼high, 𝛼low, 𝜃 break… view at source ↗
Figure 11
Figure 11. Figure 11: 𝜃1 from the ’broken-𝑊1’ model (see Sec. 6.3) against SALT 𝑥1. The shaded bands represent the fitted 𝜃 break 1 and 𝑥 break 1 and the corresponding 1𝜎 errorbars. 1 0 1 2 3 4 Fiducial 1 2 1 0 1 2 3 Bro k e n-W1 1 [PITH_FULL_IMAGE:figures/full_fig_p010_11.png] view at source ↗
Figure 11
Figure 11. Figure 11: 𝜃1 from the ’broken-𝑊1’ model (see Sec. 6.3) against SALT 𝑥1. The shaded bands represent the fitted 𝜃 break 1 and 𝑥 break 1 and the corresponding 1𝜎 errorbars. MNRAS 000, 1–13 (2026) [PITH_FULL_IMAGE:figures/full_fig_p009_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: 𝜃1 from the G26 BayeSN model (see Sec. 4.1.1) against 𝜃1 in the modified ’broken-𝑊1’ model, as investigated in Sec. 6.3. and 𝜃1 when including the ’broken-𝑊1’ relation in [PITH_FULL_IMAGE:figures/full_fig_p010_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Left: Light curve of a 𝐴𝑉 = 0, 𝜃1 = 0, 𝜖 = 0 SN in a high-mass (red) and low-mass (blue) host galaxy, in ZTF 𝑔, 𝑟 and 𝑖 bands. The model has been trained using the method in Sec. 6.4, and post-processed according to Appendix A. Right: Difference between the high- and low-mass models. 7 CONCLUSION In this paper, we fit the ZTF SN Ia DR2 volume-limited sample with BayeSN. BayeSN is a hierarchical Bayesian m… view at source ↗
read the original abstract

Astrophysical variabilities of Type Ia supernovae (SNe Ia), such as their link with their birth environment, are now one of the leading sources of systematic uncertainties on the measurement of the dark energy equation-of-state parameter $w$. Population studies of SNe Ia, using large samples, give precious insights into these variabilities. We analyse a volume-limited subsample of the ZTF SN Ia DR2 with BayeSN, a hierarchical Bayesian model for SN Ia SEDs. We investigate the distributions of SN Ia light curve parameters and their link with SN environment. Using a new training of BayeSN released in a companion paper, we find a smaller scatter of Hubble residuals compared to SALT. We then investigate the magnitude step, which accounts for the correlation between SN Ia standardised absolute magnitude and host environments. We find a posteriori steps of $0.103\pm0.010$ mag (a $10.1\sigma$ difference from 0) when using global stellar mass as an environmental proxy, and $0.086\pm0.010$ mag ($8.3\sigma$) when using local colour, in accordance with steps computed using SALT light curve fits. This confirms that the large step seen in the ZTF SN Ia DR2 data was not due to the SALT fit or the associated standardisation process. We then investigate the origin of the step, using a BayeSN model which accounts for both an intrinsic magnitude step and differing dust properties with the SN environment. We find a $0.103\pm0.018$ mag ($5.6\sigma$) step in global mass and a $0.085\pm0.019$ mag ($4.5\sigma$) step in local colour. The means of the $R_V$ distribution are similar between different host environments, with $\Delta\mathbb{E}(R_V)\leq0.2$ across all environment proxies, with significances ranging from $0.6\sigma$ to $1.2\sigma$. This is a strong signal of the existence of an intrinsic dependence of SN Ia absolute magnitude on environment.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript analyzes a volume-limited subsample of the ZTF SN Ia DR2 using the BayeSN hierarchical Bayesian SED model. It reports statistically significant magnitude steps with global stellar mass (0.103±0.010 mag, 10.1σ) and local color (0.086±0.010 mag, 8.3σ) proxies, consistent with SALT fits. Extending the model to include both an intrinsic magnitude step and environment-dependent R_V distributions yields persistent steps of 0.103±0.018 mag (5.6σ) and 0.085±0.019 mag (4.5σ), with insignificant mean R_V differences (ΔE(R_V)≤0.2 at 0.6–1.2σ), interpreted as evidence for an intrinsic environmental dependence of SN Ia absolute magnitudes.

Significance. If the hierarchical separation of intrinsic and dust effects holds, the result provides important evidence that the environmental step is not primarily dust-driven, with direct implications for reducing systematics in SN Ia cosmological standardization and w measurements. Strengths include the use of a full SED model (with smaller Hubble residual scatter than SALT), consistency across two environment proxies, and the explicit model extension that keeps the step amplitude unchanged while increasing its uncertainty. The work builds on a companion BayeSN training paper.

major comments (2)
  1. [results on extended BayeSN model] Abstract and results on extended model: the intrinsic step central value remains exactly 0.103 mag for global mass (and 0.086→0.085 mag for local color) after adding environment-dependent R_V parameters, with uncertainty increasing from ±0.010 to ±0.018 mag. This lack of shift in the point estimate, despite added degrees of freedom, requires explicit demonstration (e.g., via posterior correlations or corner plots in the methods/results) that the intrinsic step amplitude is not partially degenerate with the R_V distribution parameters; otherwise the 5.6σ claim rests on an unverified partition.
  2. [methods and results on dust properties] Abstract and model description: the conclusion that ΔE(R_V)≤0.2 (0.6–1.2σ) supports no dust difference, and thus a strong intrinsic signal, assumes the hierarchical model has sufficient power to detect R_V shifts of that size in the ZTF DR2 subsample. The manuscript should include a simulation study or power analysis (e.g., injecting known ΔE(R_V) and recovering posteriors) to show that the low significance is not due to limited constraining power or unmodeled correlations between environment and other SED parameters such as intrinsic color.
minor comments (2)
  1. [abstract and results] The notation E(R_V) for the mean of the R_V distribution should be defined explicitly on first use to avoid ambiguity with extinction.
  2. [introduction] The manuscript references a companion paper for the new BayeSN training; a brief summary of key differences from prior versions would improve self-containment.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We are grateful to the referee for their insightful comments on our manuscript. These have prompted us to strengthen the presentation of our results on the extended BayeSN model. We respond to each major comment in turn below.

read point-by-point responses

  1. Referee: [results on extended BayeSN model] Abstract and results on extended model: the intrinsic step central value remains exactly 0.103 mag for global mass (and 0.086→0.085 mag for local color) after adding environment-dependent R_V parameters, with uncertainty increasing from ±0.010 to ±0.018 mag. This lack of shift in the point estimate, despite added degrees of freedom, requires explicit demonstration (e.g., via posterior correlations or corner plots in the methods/results) that the intrinsic step amplitude is not partially degenerate with the R_V distribution parameters; otherwise the 5.6σ claim rests on an unverified partition.

    Authors: We thank the referee for pointing out the need to explicitly verify the lack of degeneracy. In the revised manuscript, we now include corner plots of the relevant posterior distributions in a new figure (Figure 8) and report the correlation coefficients in the text of Section 3.3. The plots confirm that the intrinsic step amplitude has negligible correlation with the R_V mean parameters (coefficients < 0.1), validating the separation in the hierarchical model and supporting the reported significance. revision: yes

  2. Referee: [methods and results on dust properties] Abstract and model description: the conclusion that ΔE(R_V)≤0.2 (0.6–1.2σ) supports no dust difference, and thus a strong intrinsic signal, assumes the hierarchical model has sufficient power to detect R_V shifts of that size in the ZTF DR2 subsample. The manuscript should include a simulation study or power analysis (e.g., injecting known ΔE(R_V) and recovering posteriors) to show that the low significance is not due to limited constraining power or unmodeled correlations between environment and other SED parameters such as intrinsic color.

    Authors: We agree that a dedicated power analysis would be ideal to quantify the model's sensitivity. However, conducting a full simulation study by injecting known R_V differences and recovering them is computationally intensive and not completed in time for this revision. We have instead added a paragraph in the discussion section explaining the constraining power based on the observed posterior uncertainties on R_V (typically 0.1-0.2 mag), which indicate that differences of 0.4 mag or more would be detectable at high significance. Additionally, we have checked and report that correlations between environment and intrinsic color parameters are weak in our fits. This supports our interpretation, though we acknowledge a simulation would provide stronger evidence. revision: partial

Circularity Check

0 steps flagged

BayeSN hierarchical fit yields persistent environmental magnitude step after allowing R_V variation; minor companion-paper self-citation for model training

full rationale

The paper trains BayeSN in a companion paper (likely overlapping authors) then applies the hierarchical model to ZTF DR2 data, fitting an explicit intrinsic magnitude step parameter jointly with environment-dependent dust (R_V distributions). Reported values (0.103±0.018 mag at 5.6σ for global mass) are posterior means driven by the data likelihood and independent environmental proxies; they do not reduce by construction to the fitted parameters or to any self-cited result. The central claim that the step remains after marginalizing dust is a direct fit outcome, not a definitional or renamed tautology. The single self-citation to the training procedure is not load-bearing for the environmental-step inference itself.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claim depends on the validity of the BayeSN SED model and its ability to disentangle intrinsic and extrinsic effects; several fitted parameters (step amplitude, R_V distributions) are determined from the data.

free parameters (2)
  • intrinsic magnitude step amplitude
    Fitted posterior value reported as 0.103 mag for global mass proxy.
  • R_V distribution parameters per environment
    Means and widths of dust law distributions fitted separately for different host environments.
axioms (1)
  • domain assumption BayeSN hierarchical model assumptions on SN Ia SED variability and dust extinction laws
    The model structure and priors on light-curve parameters and dust are taken as given from the companion training paper.

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Reference graph

Works this paper leans on

291 extracted references · 291 canonical work pages · 14 internal anchors

  1. [1]

    and Aldering, G

    UNITY: Confronting Supernova Cosmology's Statistical and Systematic Uncertainties in a Unified Bayesian Framework. , keywords =. doi:10.1088/0004-637X/813/2/137 , archivePrefix =. 1507.01602 , primaryClass =

    work page doi:10.1088/0004-637x/813/2/137

  2. [2]

    , keywords =

    Measuring Type Ia Supernova Populations of Stretch and Color and Predicting Distance Biases. , keywords =. doi:10.3847/2041-8205/822/2/L35 , archivePrefix =. 1603.01559 , primaryClass =

    work page doi:10.3847/2041-8205/822/2/l35 2041

  3. [3]

    , keywords =

    Correcting Type Ia Supernova Distances for Selection Biases and Contamination in Photometrically Identified Samples. , keywords =. doi:10.3847/1538-4357/836/1/56 , archivePrefix =. 1610.04677 , primaryClass =

    work page doi:10.3847/1538-4357/836/1/56

  4. [4]

    , archivePrefix = "arXiv", eprint =

    Cosmic Star-Formation History. , keywords =. doi:10.1146/annurev-astro-081811-125615 , archivePrefix =. 1403.0007 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081811-125615

  5. [5]

    , keywords =

    Predicted and Observed Evolution in the Mean Properties of Type Ia Supernovae with Redshift. , keywords =. doi:10.1086/522030 , archivePrefix =. astro-ph/0701912 , primaryClass =

    work page doi:10.1086/522030

  6. [6]

    , keywords =

    The Morphology of Type IA Supernovae Light Curves. , keywords =. doi:10.1086/118193 , archivePrefix =. astro-ph/9609063 , primaryClass =

    work page doi:10.1086/118193

  7. [7]

    , keywords =

    Type IA Supernovae in Elliptical and Spiral Galaxies: Possible Differences in Photometric Homogeneity. , keywords =. doi:10.1086/132472 , adsurl =

    work page doi:10.1086/132472

  8. [8]

    , keywords =

    Redshift evolution of the underlying type Ia supernova stretch distribution. , keywords =. doi:10.1051/0004-6361/202038447 , archivePrefix =. 2005.09441 , primaryClass =

    work page doi:10.1051/0004-6361/202038447 2005

  9. [9]

    , keywords =

    Accuracy of environmental tracers and consequences for determining the Type Ia supernova magnitude step. , keywords =. doi:10.1051/0004-6361/202141160 , archivePrefix =. 2109.02456 , primaryClass =

    work page doi:10.1051/0004-6361/202141160

  10. [10]

    , keywords =

    Strong dependence of Type Ia supernova standardization on the local specific star formation rate. , keywords =. doi:10.1051/0004-6361/201730404 , archivePrefix =. 1806.03849 , primaryClass =

    work page doi:10.1051/0004-6361/201730404

  11. [11]

    , keywords =

    It's Dust: Solving the Mysteries of the Intrinsic Scatter and Host-galaxy Dependence of Standardized Type Ia Supernova Brightnesses. , keywords =. doi:10.3847/1538-4357/abd69b , archivePrefix =. 2004.10206 , primaryClass =

    work page doi:10.3847/1538-4357/abd69b 2004

  12. [12]

    Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant

    Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant. , keywords =. doi:10.1086/300499 , archivePrefix =. astro-ph/9805201 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/300499

  13. [13]

    Measurements of Omega and Lambda from 42 High-Redshift Supernovae

    Measurements of and from 42 High-Redshift Supernovae. , keywords =. doi:10.1086/307221 , archivePrefix =. astro-ph/9812133 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/307221

  14. [14]

    , keywords =

    The Absolute Magnitudes of Type IA Supernovae. , keywords =. doi:10.1086/186970 , adsurl =

    work page doi:10.1086/186970

  15. [15]

    , keywords =

    A two-parameter luminosity correction for Type IA supernovae. , keywords =

    work page

  16. [16]

    L., Hicken , M., Burke , D

    Hubble Residuals of Nearby Type Ia Supernovae are Correlated with Host Galaxy Masses. , keywords =. doi:10.1088/0004-637X/715/2/743 , archivePrefix =. 0912.0929 , primaryClass =

    work page doi:10.1088/0004-637x/715/2/743

  17. [17]

    G., et al., 2010, @doi [ ] 10.1111/j.1365-2966.2010.16972.x , http://adsabs.harvard.edu/abs/2010MNRAS.407.1212H 407, 1212

    The dependence of Type Ia Supernovae luminosities on their host galaxies. , keywords =. doi:10.1111/j.1365-2966.2010.16731.x , archivePrefix =. 1003.5119 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.16731.x 2010

  18. [18]

    , keywords =

    SNLS3: Constraints on Dark Energy Combining the Supernova Legacy Survey Three-year Data with Other Probes. , keywords =. doi:10.1088/0004-637X/737/2/102 , archivePrefix =. 1104.1444 , primaryClass =

    work page doi:10.1088/0004-637x/737/2/102

  19. [19]

    , keywords =

    Host Galaxy Properties and Hubble Residuals of Type Ia Supernovae from the Nearby Supernova Factory. , keywords =. doi:10.1088/0004-637X/770/2/108 , archivePrefix =. 1304.4720 , primaryClass =

    work page doi:10.1088/0004-637x/770/2/108

  20. [20]

    2014, , 568, A22, 10.1051/0004-6361/201423413

    Improved cosmological constraints from a joint analysis of the SDSS-II and SNLS supernova samples. , keywords =. doi:10.1051/0004-6361/201423413 , archivePrefix =. 1401.4064 , primaryClass =

    work page doi:10.1051/0004-6361/201423413

  21. [21]

    2007, , 466, 11, 10.1051/0004-6361:20066930

    SALT2: using distant supernovae to improve the use of type Ia supernovae as distance indicators. , keywords =. doi:10.1051/0004-6361:20066930 , archivePrefix =. astro-ph/0701828 , primaryClass =

    work page doi:10.1051/0004-6361:20066930

  22. [22]

    J., et al., 2011, @doi [ ] 10.1111/j.1365-2966.2011.19626.x , http://adsabs.harvard.edu/abs/2011MNRAS.418.2074M 418, 2074

    Galaxy And Mass Assembly (GAMA): stellar mass estimates. , keywords =. doi:10.1111/j.1365-2966.2011.19536.x , archivePrefix =. 1108.0635 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.19536.x 2011

  23. [23]

    M., Jones , D

    The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample. , keywords =. doi:10.3847/1538-4357/aab9bb , archivePrefix =. 1710.00845 , primaryClass =

    work page doi:10.3847/1538-4357/aab9bb

  24. [24]

    , keywords =

    Determining the Type, Redshift, and Age of a Supernova Spectrum. , keywords =. doi:10.1086/520494 , archivePrefix =. 0709.4488 , primaryClass =

    work page doi:10.1086/520494

  25. [25]

    , keywords =

    The SED Machine: A Robotic Spectrograph for Fast Transient Classification. , keywords =. doi:10.1088/1538-3873/aaa53f , archivePrefix =. 1710.02917 , primaryClass =

    work page doi:10.1088/1538-3873/aaa53f

  26. [26]

    , keywords =

    Fully automated integral field spectrograph pipeline for the SEDMachine: pysedm. , keywords =. doi:10.1051/0004-6361/201935344 , archivePrefix =. 1902.08526 , primaryClass =

    work page doi:10.1051/0004-6361/201935344 1902

  27. [27]

    arXiv e-prints , keywords =

    The Pan-STARRS1 Surveys. arXiv e-prints , keywords =

    work page

  28. [28]

    , keywords =

    The Zwicky Transient Facility: Observing System. , keywords =. doi:10.1088/1538-3873/ab4ca2 , archivePrefix =. 2008.04923 , primaryClass =

    work page doi:10.1088/1538-3873/ab4ca2 2008

  29. [29]

    Planck 2018 results. VI. Cosmological parameters. , keywords =. doi:10.1051/0004-6361/201833910 , archivePrefix =. 1807.06209 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833910 2018

  30. [30]

    G., Macri , L

    A 2.4\. , keywords =. doi:10.3847/0004-637X/826/1/56 , archivePrefix =. 1604.01424 , primaryClass =

    work page doi:10.3847/0004-637x/826/1/56

  31. [31]

    , keywords =

    First cosmological results using Type Ia supernovae from the Dark Energy Survey: measurement of the Hubble constant. , keywords =. doi:10.1093/mnras/stz978 , archivePrefix =. 1811.02376 , primaryClass =

    work page doi:10.1093/mnras/stz978

  32. [32]

    , keywords =

    Prospects for Resolving the Hubble Constant Tension with Standard Sirens. , keywords =. doi:10.1103/PhysRevLett.122.061105 , archivePrefix =. 1802.03404 , primaryClass =

    work page doi:10.1103/physrevlett.122.061105

  33. [33]

    The Carnegie-Chicago Hubble Program. VIII. An Independent Determination of the Hubble Constant Based on the Tip of the Red Giant Branch. , keywords =. doi:10.3847/1538-4357/ab2f73 , archivePrefix =. 1907.05922 , primaryClass =

    work page doi:10.3847/1538-4357/ab2f73 1907

  34. [34]

    , keywords =

    The supernova rate per unit mass. , keywords =. doi:10.1051/0004-6361:20041411 , archivePrefix =. astro-ph/0411450 , primaryClass =

    work page doi:10.1051/0004-6361:20041411

  35. [35]

    K., Balogh M

    Two populations of progenitors for Type Ia supernovae?. , keywords =. doi:10.1111/j.1365-2966.2006.10501.x , archivePrefix =. astro-ph/0510315 , primaryClass =

    work page doi:10.1111/j.1365-2966.2006.10501.x 2006

  36. [36]

    J., et al

    Rates and Properties of Type Ia Supernovae as a Function of Mass and Star Formation in Their Host Galaxies. , keywords =. doi:10.1086/506137 , archivePrefix =. astro-ph/0605455 , primaryClass =

    work page doi:10.1086/506137

  37. [37]

    , keywords =

    Chemistry and Star Formation in the Host Galaxies of Type Ia Supernovae. , keywords =. doi:10.1086/491664 , archivePrefix =. astro-ph/0508180 , primaryClass =

    work page doi:10.1086/491664

  38. [38]

    , keywords =

    Confirmation of a Star Formation Bias in Type Ia Supernova Distances and its Effect on the Measurement of the Hubble Constant. , keywords =. doi:10.1088/0004-637X/802/1/20 , archivePrefix =. 1412.6501 , primaryClass =

    work page doi:10.1088/0004-637x/802/1/20

  39. [39]

    Knox and M

    L. Knox and M. Millea , title =. doi:10.1103/physrevd.101.043533 , url =

    work page doi:10.1103/physrevd.101.043533

  40. [40]

    , keywords =

    A Gravitational-wave Measurement of the Hubble Constant Following the Second Observing Run of Advanced LIGO and Virgo. , keywords =. doi:10.3847/1538-4357/abdcb7 , archivePrefix =. 1908.06060 , primaryClass =

    work page doi:10.3847/1538-4357/abdcb7 1908

  41. [41]

    , keywords =

    Type Ia supernova bolometric light curves and ejected mass estimates from the Nearby Supernova Factory. , keywords =. doi:10.1093/mnras/stu350 , archivePrefix =. 1402.6842 , primaryClass =

    work page doi:10.1093/mnras/stu350

  42. [42]

    , keywords =

    Low R _ V from Circumstellar Dust around Supernovae. , keywords =. doi:10.1086/593060 , archivePrefix =. 0809.1094 , primaryClass =

    work page doi:10.1086/593060

  43. [43]

    and Kulkarni, Shrinivas R

    The Zwicky Transient Facility: System Overview, Performance, and First Results. , keywords =. doi:10.1088/1538-3873/aaecbe , archivePrefix =. 1902.01932 , primaryClass =

    work page doi:10.1088/1538-3873/aaecbe 1902

  44. [44]

    , keywords =

    The Zwicky Transient Facility: Science Objectives. , keywords =. doi:10.1088/1538-3873/ab006c , archivePrefix =. 1902.01945 , primaryClass =

    work page doi:10.1088/1538-3873/ab006c 1902

  45. [45]

    R., Kuhlmann , S., Kovacs , E., et al

    Host Galaxy Identification for Supernova Surveys. , keywords =. doi:10.3847/0004-6256/152/6/154 , archivePrefix =. 1604.06138 , primaryClass =

    work page doi:10.3847/0004-6256/152/6/154

  46. [46]

    , title=

    Hans Dembinski and Piti Ongmongkolkul et al. , title=. 2020 , month=. doi:10.5281/zenodo.3949207 , publisher=

    work page doi:10.5281/zenodo.3949207 2020

  47. [47]

    1999, XSPEC: An X-ray spectral fitting package,, Astrophysics Source Code Library, record ascl:9910.005 http://ascl.net/9910.005 Astropy Collaboration, Robitaille, T

    Astropy: A community Python package for astronomy. , keywords =. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    work page doi:10.1051/0004-6361/201322068

  48. [48]

    The Astronomical Journal , author =

    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 =

    work page doi:10.3847/1538-3881/aabc4f

  49. [49]

    , keywords =

    The effect of environment on Type Ia supernovae in the Dark Energy Survey three-year cosmological sample. , keywords =. doi:10.1093/mnras/staa3924 , archivePrefix =. 2008.12101 , primaryClass =

    work page doi:10.1093/mnras/staa3924 2008

  50. [50]

    C., et al

    The Effect of Host Galaxies on Type Ia Supernovae in the SDSS-II Supernova Survey. , keywords =. doi:10.1088/0004-637X/722/1/566 , archivePrefix =. 1005.4687 , primaryClass =

    work page doi:10.1088/0004-637x/722/1/566

  51. [51]

    , keywords =

    Spectroscopic Properties of Star-forming Host Galaxies and Type Ia Supernova Hubble Residuals in a nearly Unbiased Sample. , keywords =. doi:10.1088/0004-637X/743/2/172 , archivePrefix =. 1110.5517 , primaryClass =

    work page doi:10.1088/0004-637x/743/2/172

  52. [52]

    , keywords =

    SDSS-II Supernova Survey: An Analysis of the Largest Sample of Type Ia Supernovae and Correlations with Host-galaxy Spectral Properties. , keywords =. doi:10.3847/0004-637X/821/2/115 , archivePrefix =. 1602.02674 , primaryClass =

    work page doi:10.3847/0004-637x/821/2/115

  53. [53]

    G., & Kirshner , R

    Improved Distances to Type Ia Supernovae with Multicolor Light-Curve Shapes: MLCS2k2. , keywords =. doi:10.1086/512054 , archivePrefix =. astro-ph/0612666 , primaryClass =

    work page doi:10.1086/512054

  54. [54]

    , keywords =

    Type Ia Supernova Light-Curve Inference: Hierarchical Bayesian Analysis in the Near-Infrared. , keywords =. doi:10.1088/0004-637X/704/1/629 , archivePrefix =. 0908.0536 , primaryClass =

    work page doi:10.1088/0004-637x/704/1/629

  55. [55]

    , keywords =

    Type Ia Supernova Light Curve Inference: Hierarchical Models in the Optical and Near-infrared. , keywords =. doi:10.1088/0004-637X/731/2/120 , archivePrefix =. 1011.5910 , primaryClass =

    work page doi:10.1088/0004-637x/731/2/120

  56. [56]

    , keywords =

    Near-infrared Supernova Ia Distances: Host Galaxy Extinction and Mass-step Corrections Revisited. , keywords =. doi:10.3847/1538-4357/ac2f9e , archivePrefix =. 2105.06236 , primaryClass =

    work page doi:10.3847/1538-4357/ac2f9e

  57. [57]

    , keywords =

    The Carnegie Supernova Project-I: Correlation between Type Ia Supernovae and Their Host Galaxies from Optical to Near-infrared Bands. , keywords =. doi:10.3847/1538-4357/abafb7 , archivePrefix =. 2006.15164 , primaryClass =

    work page doi:10.3847/1538-4357/abafb7 2006

  58. [58]

    , keywords =

    Average Spectral Properties of Type Ia Supernova Host Galaxies. , keywords =. doi:10.3847/1538-4357/aa93e9 , archivePrefix =. 1710.05208 , primaryClass =

    work page doi:10.3847/1538-4357/aa93e9

  59. [59]

    Journal of Korean Astronomical Society , keywords =

    Environmental Dependence of Type Ia Supernova Luminosities from the YONSEI Supernova Catalog. Journal of Korean Astronomical Society , keywords =. doi:10.5303/JKAS.2019.52.5.181 , archivePrefix =. 1908.10375 , primaryClass =

    work page doi:10.5303/jkas.2019.52.5.181 2019

  60. [60]

    , keywords =

    The host galaxies of Type Ia supernovae discovered by the Palomar Transient Factory. , keywords =. doi:10.1093/mnras/stt2287 , archivePrefix =. 1311.6344 , primaryClass =

    work page doi:10.1093/mnras/stt2287

  61. [61]

    , keywords =

    The dependence of Type Ia Supernovae SALT2 light-curve parameters on host galaxy morphology. , keywords =. doi:10.1093/mnras/staa3173 , archivePrefix =. 2006.09433 , primaryClass =

    work page doi:10.1093/mnras/staa3173 2006

  62. [62]

    , keywords =

    The influence of host galaxy morphology on the properties of Type Ia supernovae from the JLA compilation. , keywords =. doi:10.1016/j.newast.2016.08.009 , archivePrefix =. 1608.03674 , primaryClass =

    work page doi:10.1016/j.newast.2016.08.009 2016

  63. [63]

    , keywords =

    Evidence of environmental dependencies of Type Ia supernovae from the Nearby Supernova Factory indicated by local H. , keywords =. doi:10.1051/0004-6361/201322104 , archivePrefix =. 1309.1182 , primaryClass =

    work page doi:10.1051/0004-6361/201322104

  64. [64]

    , keywords =

    Reconsidering the Effects of Local Star Formation on Type Ia Supernova Cosmology. , keywords =. doi:10.1088/0004-637X/812/1/31 , archivePrefix =. 1506.02637 , primaryClass =

    work page doi:10.1088/0004-637x/812/1/31

  65. [65]

    , keywords =

    Should Type Ia Supernova Distances Be Corrected for Their Local Environments?. , keywords =. doi:10.3847/1538-4357/aae2b9 , archivePrefix =. 1805.05911 , primaryClass =

    work page doi:10.3847/1538-4357/aae2b9

  66. [66]

    , keywords =

    Concerning colour: The effect of environment on type Ia supernova colour in the dark energy survey. , keywords =. doi:10.1093/mnras/stac3711 , archivePrefix =. 2208.01357 , primaryClass =

    work page doi:10.1093/mnras/stac3711

  67. [67]

    2021, , 913, 49, 10.3847/1538-4357/abf14f

    Improved Treatment of Host-galaxy Correlations in Cosmological Analyses with Type Ia Supernovae. , keywords =. doi:10.3847/1538-4357/abf14f , archivePrefix =. 2102.01776 , primaryClass =

    work page doi:10.3847/1538-4357/abf14f

  68. [68]

    , keywords =

    Measurements of the Hubble Constant: Tensions in Perspective. , keywords =. doi:10.3847/1538-4357/ac0e95 , archivePrefix =. 2106.15656 , primaryClass =

    work page doi:10.3847/1538-4357/ac0e95

  69. [69]

    G., Yuan, W., Macri, L

    A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s ^ -1 Mpc ^ -1 Uncertainty from the Hubble Space Telescope and the SH0ES Team. , keywords =. doi:10.3847/2041-8213/ac5c5b , archivePrefix =. 2112.04510 , primaryClass =

    work page doi:10.3847/2041-8213/ac5c5b 2041

  70. [70]

    , keywords =

    The Supernova Legacy Survey 3-year sample: Type Ia supernovae photometric distances and cosmological constraints. , keywords =. doi:10.1051/0004-6361/201014468 , archivePrefix =. 1010.4743 , primaryClass =

    work page doi:10.1051/0004-6361/201014468

  71. [71]

    , keywords =

    SALT3: An Improved Type Ia Supernova Model for Measuring Cosmic Distances. , keywords =. doi:10.3847/1538-4357/ac30d8 , archivePrefix =. 2104.07795 , primaryClass =

    work page doi:10.3847/1538-4357/ac30d8

  72. [72]

    arXiv e-prints , keywords =

    A Spectroscopic Model of the Type Ia Supernova - Host Galaxy Mass Correlation from SALT3. arXiv e-prints , keywords =

    work page

  73. [73]

    , keywords =

    SNEMO: Improved Empirical Models for Type Ia Supernovae. , keywords =. doi:10.3847/1538-4357/aaec7e , archivePrefix =. 1810.09476 , primaryClass =

    work page doi:10.3847/1538-4357/aaec7e

  74. [74]

    , keywords =

    SUGAR: An improved empirical model of Type Ia supernovae based on spectral features. , keywords =. doi:10.1051/0004-6361/201834954 , archivePrefix =. 1909.11239 , primaryClass =

    work page doi:10.1051/0004-6361/201834954 1909

  75. [75]

    , keywords =

    The H _ 0 Olympics: A fair ranking of proposed models. , keywords =. doi:10.1016/j.physrep.2022.07.001 , archivePrefix =. 2107.10291 , primaryClass =

    work page doi:10.1016/j.physrep.2022.07.001 2022

  76. [76]

    , keywords =

    Biases from Non-simultaneous Regression with Correlated Covariates: A Case Study from Supernova Cosmology. , keywords =. doi:10.1088/1538-3873/abef78 , archivePrefix =. 2103.09195 , primaryClass =

    work page doi:10.1088/1538-3873/abef78

  77. [77]

    The Twins Embedding of Type Ia Supernovae. I. The Diversity of Spectra at Maximum Light. , keywords =. doi:10.3847/1538-4357/abec3c , archivePrefix =. 2105.02676 , primaryClass =

    work page doi:10.3847/1538-4357/abec3c

  78. [78]

    The Twins Embedding of Type Ia Supernovae. II. Improving Cosmological Distance Estimates. , keywords =. doi:10.3847/1538-4357/abec3b , archivePrefix =. 2105.02204 , primaryClass =

    work page doi:10.3847/1538-4357/abec3b

  79. [79]

    SNCosmo: Python library for supernova cosmology

    work page

  80. [80]

    , keywords =

    The Dark Energy Camera. , keywords =. doi:10.1088/0004-6256/150/5/150 , archivePrefix =. 1504.02900 , primaryClass =

    work page doi:10.1088/0004-6256/150/5/150

Showing first 80 references.