pith. machine review for the scientific record. sign in

arxiv: 2604.18859 · v1 · submitted 2026-04-20 · 🌌 astro-ph.CO

Recognition: unknown

Testing ΛCDM versus dynamical dark energy in one year: A DESI spectroscopic follow-up program for Rubin supernovae

Jannik Truong , Greg Aldering , Saul Perlmutter , David Rubin , David Schlegel
Authors on Pith no claims yet

Pith reviewed 2026-05-10 03:04 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords dynamical dark energyType Ia supernovaeDESIRubin ObservatoryLambda CDM tensionw0-wa parametrizationspectroscopic follow-upcosmological probes
0
0 comments X

The pith

Re-prioritizing DESI observations around Rubin supernova alerts can deliver a volume-limited sample that raises tension with Lambda CDM above 5 sigma in one year if current w0-wa fits hold.

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

The paper outlines a one-year supernova survey that uses real-time alerts from the Vera C. Rubin Observatory to re-prioritize tile visits already scheduled for the Dark Energy Spectroscopic Instrument. This yields 7500 near-peak spectra without delaying DESI's primary program, with emphasis on a spectroscopically confirmed volume-limited subset of 2300 Type Ia supernovae at redshifts below 0.3. Those low-redshift objects sit near dark energy-matter equality and add the strongest leverage against a cosmological constant when combined with existing supernova, baryon acoustic oscillation, and cosmic microwave background measurements. If the present best-fit values of the w0 and wa parameters continue, the combined dataset would exceed 5 sigma tension with Lambda CDM across a broad range of assumed uncertainties.

Core claim

By triggering DESI observations from Rubin supernova alerts, the program secures 7500 near-peak transient spectra in one year, including a volume-limited sample of 2300 SNe Ia at z less than 0.3. When this subset is added to current SN, BAO, and CMB data, any persistence of the existing best-fit w0 and wa values pushes the deviation from Lambda CDM beyond 5 sigma. The forecast remains robust under varied uncertainty assumptions, and the same spectra open a route to machine-learning-based spectroscopic standardization that bypasses light-curve methods.

What carries the argument

Alert-driven re-prioritization of DESI tile visits to assemble a spectroscopically confirmed volume-limited supernova sample at z less than 0.3.

If this is right

  • The new low-redshift SNe Ia raise tension with Lambda CDM above 5 sigma if current w0-wa best fits persist, across wide uncertainty assumptions.
  • The full program reaches greater than 5 sigma sensitivity to dynamical dark energy using only one year of data starting in 2027.
  • DESI spectra enable machine-learning standardization that could produce cosmology results independent of light-curve methods.
  • Early results from the survey can directly inform the design of future dark energy experiments.

Where Pith is reading between the lines

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

  • Coordinated alert-driven scheduling between optical surveys and spectroscopic facilities could be applied to other transient populations to accelerate parameter constraints.
  • Emphasis on volume-limited samples at z less than 0.3 may become a standard strategy for testing dark energy evolution in upcoming facilities.
  • If the program succeeds, it would illustrate how modest operational flexibility between existing telescopes can deliver high-impact cosmological tests without new hardware.

Load-bearing premise

That today's best-fit w0 and wa values will remain the same after the new data arrive and that the re-prioritized DESI observations will achieve the forecasted sample size with systematics held at the assumed levels.

What would settle it

A combined analysis in which the tension with Lambda CDM stays below 5 sigma after including the 2300 new low-redshift SNe Ia, or an operational failure to obtain the projected 7500 spectra because of scheduling conflicts.

Figures

Figures reproduced from arXiv: 2604.18859 by David Rubin, David Schlegel, Greg Aldering, Jannik Truong, Saul Perlmutter.

Figure 1
Figure 1. Figure 1: Reconstructed 1σ and 2σ Gaussian contours for w0 and wa from different datasets: Union3 (D. Rubin et al. 2025a) SNe Ia only (blue), DESI DR2 BAO+Planck CMB without SNe (green, M. Abdul Karim et al. (2025)), and all three combined (orange). When combining all three datasets, ΛCDM (w0 = −1 and wa = 0, top left black point) is 3.8σ from the best-fit values. many of which were conceptualized without considerin… view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of uncertainties of binned distance moduli between ∼ 3000 simulated volume-limited z < 0.3 LSST supernovae with (green) and without (orange) DESI follow-up, and Union3 (blue). We plot the square roots of the diagonal elements of the distance modulus covariance matrix, and σcorr correspond to the first off-diagonal. Without spec￾troscopic follow-up, the new statistical power of LSST SNe can hardl… view at source ↗
Figure 3
Figure 3. Figure 3: We sample different cosmologies according to the current (DESI DR2+Planck+Union3) best-fitting probability distributions for w0, wa, Ωm, compute the theoretical distance moduli and compare them against the best-fit cosmology (black dashed line). On the left panel, we can see how measuring additional SNe Ia at redshifts z ≈ 0.55 would currently be the most helpful for constraining dynamical dark energy. On … view at source ↗
Figure 4
Figure 4. Figure 4: Distance from ΛCDM given by the number of standard deviations, and Figure of Merit when adding supernovae at one redshift bin z with different total uncertainties to DESI DR2+Planck+Union3 and low-z SNe. Total uncertainties include statistical and systematic errors, although statistical errors typically become subdominant for 103 to 104 SNe Ia. We find that measuring around z ≈ 0.6 increases the distance f… view at source ↗
Figure 5
Figure 5. Figure 5: Distance from ΛCDM and Figure of Merit when adding supernovae at two redshift bins (z1 and z2) with 10mmag total uncertainty each to DESI DR2+Planck+Union3 and low-z SNe. Two measurements at medium redshifts z ≈ 0.6 and the combination of low-z and medium-z are considered optimal. baseline uncertainty of 10 mmag. This allows for a con￾servative accounting of statistical and systematic uncer￾tainties. For e… view at source ↗
Figure 6
Figure 6. Figure 6: Simulated light curve for a median Type Ia su￾pernova at z = 0.225, reflecting the (high-activity) WFD strategy to observe in pairs of filters every three days. These results are similar to other simulations, e.g. fig. 16 of (R. Kessler et al. 2019). Missing points reflect bright moon phases (affecting g, r, i predominantly), the possibility of a supernova being missed due to chip gaps, and u and Y bands b… view at source ↗
Figure 7
Figure 7. Figure 7: Histogram of forecasted SNe Ia discovered in our simulations of Rubin’s high-activity Wide Fast Deep in the overlap region with DESI in one year. Practically all SNe are well-measured up to z = 0.35. The SNR values given here are defined to be the quadrature sum of all measurements of a single supernova. • 7 mmag/µm tilt in flux calibration vs. wavelength (R. C. Bohlin et al. 2014), correlated across all S… view at source ↗
Figure 8
Figure 8. Figure 8: DESI, DESI-II and approximated LSST Wide Fast Deep footprints. The numbers in the legend refer to the areas inside DESI(-II) and LSST-WFD that are observable by both sites in a single night. The total footprint overlaps with LSST-WFD are 9000 deg2 for DESI and 5000 deg2 for DESI-II. Jan Feb Mar Apr May Jun Jul Aug Sep Oct Nov Dec Date (2027) 3000 4000 5000 6000 Observable area [deg 2 ] DESI footprints with… view at source ↗
Figure 9
Figure 9. Figure 9: The nightly observable area of DESI and DESI-II footprints within LSST-WFD in 2027, requiring object altitude > 30◦ and Sun altitude < −15◦ at both sites [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: A faint Type Ia supernova spectrum at maximum light (bold colored lines), with added noise (thin colored lines) as simulated by DESI’s SpecSim for a single dark exposure. Binned in 15 ˚A. SNR15˚A = 3.0, total SNR = 52. 7200 7400 7600 7800 8000 8200 8400 8600 Wavelength [˚A] 0.0 0.1 0.2 0.3 0.4 Flux [10−17 erg/s/cm2 /˚A] SN Ia, ∆M = 1.0, z = 0.3, teff =1000.0 s Si II feature [PITH_FULL_IMAGE:figures/full_… view at source ↗
Figure 11
Figure 11. Figure 11: The same simulated SN Ia spectrum as in Fig￾ure 10. Even without the visual cue from the template, the SiII absorption line is still readily visible. SiII 6150˚Afeature, simply employ a gray (wavelength￾independent) offset of the aforementioned ∆M = 1.0 mag, which dampens the flux by 60%. The gray offset leaves open the question whether such a faint su￾pernova is intrinsically faint, or appears faint due … view at source ↗
Figure 12
Figure 12. Figure 12: Stacked histogram showing the one-year fore￾cast of spectroscopically followed near-peak (±5 days) vol￾ume-limited SNe Ia per redshift. The current DESI Tran￾sients Survey program, where spare fibers are assigned to live transients if they happen to fall into a planned point￾ing (blue), would obtain around 880 SNe Ia. When allowing a transient to actively trigger any remaining tile pointing, 2300 SNe Ia c… view at source ↗
Figure 13
Figure 13. Figure 13: Number of pointings with at least one near-peak (±5 days) SN Ia per 10-day bin for bright (left) and dark (right) tiles, compared to the available observing time (red). For bright tiles, the small volume at z < 0.15 means that available tile pointings initially exceed the supernova rate, but efficiency still decreases continuously as tiles are depleted. For dark tiles, the larger volume produces more SNe,… view at source ↗
Figure 14
Figure 14. Figure 14: Efficiency: Fibers per pointing used on volume-limited SNe Ia (left) and all candidates passing the magnitude cut (right) within ±5 days of maximum light, for bright and dark tiles combined. Even with active triggers, some pointings will not contain a volume-limited SN Ia because tiles can only be scored and scheduled based on the number of all candidates, out of which only around 30% belong to the volume… view at source ↗
Figure 15
Figure 15. Figure 15: Projected 1, 2 and 5σ contours for the w0 and wa parameters of dynamical dark energy, and an inset zoomed in around ΛCDM (w0 = −1, wa = 0). We combine the current data baseline (gray, DESI BAO+CMB+Union3+low-z SNe as described in §2) with one year of DESI’s current transient program (blue), and our proposed survey with SNe actively triggering tile visits (orange). Without increasing total effective observ… view at source ↗
Figure 16
Figure 16. Figure 16: Stacked histogram of DESI spectroscopic follow-up yields of Rubin WFD targets. Our proposed survey observes around 7500 total objects within ±5 days of their peak bright￾ness with 3100 actively-triggered pointings. The current spare fiber program would obtain 2800 objects with 3500 passive pointings. −1.5 −1.0 −0.5 0.0 0.5 w0 −5 −4 −3 −2 −1 0 1 2 wa Baseline + DESI active triggers BAO+CMB only DESI SNe on… view at source ↗
Figure 18
Figure 18. Figure 18: Zero-point calibration priors versus posteriors for each Rubin filter. The unified fitting framework allows for self-calibration, reducing posterior uncertainties by up to 40% relative to the assumed priors. However, we find no floor beyond which the posterior uncertainty is always lower than the prior uncertainty for any realistic prior. This in￾dicates a potential prior-dependence of cosmology results i… view at source ↗
Figure 19
Figure 19. Figure 19: Distance from ΛCDM in σ (left) and Dark Energy Task Force Figure of Merit (right) as a function of the assumed zero-point calibration prior and gray dispersion — the two dominant systematics most likely to improve in the near future. Values in parentheses correspond to forecasts without a separate sample of new low-z supernova. The 5σ threshold is reached or exceeded across a wide range of assumed priors.… view at source ↗
Figure 20
Figure 20. Figure 20: Distance from ΛCDM and Figure of Merit when adding supernovae at two redshift bins (z1 and z2) with 10mmag total uncertainty each to baseline data (§2) plus DESI “active trigger” SNe. Compared to [PITH_FULL_IMAGE:figures/full_fig_p021_20.png] view at source ↗
read the original abstract

Combined cosmological probes currently indicate that best-fit values in the $w_0-w_a$ parametrization of dynamical dark energy deviate from $\Lambda$CDM by $\sim3\sigma$. In this work, we present a supernova survey capable of measuring dynamical dark energy at the $>5\sigma$ level with just one year of data, starting in 2027. We first show that with the present values of $w_0$ and $w_a$, new SNe Ia at redshifts $z\lesssim0.6$ near dark energy-matter equality would add the most constraining power. This is well within reach of the Vera C. Rubin Observatory and the Dark Energy Spectroscopic Instrument (DESI). Because cosmology measurements with SNe Ia quickly become systematics-limited, we focus on eliminating key systematics by using only a spectroscopically confirmed and volume-limited sample. In our proposed survey, SN alerts from Rubin would actively re-prioritize the scheduling of already-planned DESI tile visits. This would yield 7 500 near-peak transient spectra in one year without delaying DESI's primary survey. We forecast that if current best-fit $w_0-w_a$ values persist, combining just our volume-limited subset of 2 300 new SNe Ia at $z<0.3$ with current SN, BAO, and CMB data would push the tension with $\Lambda$CDM beyond $5\sigma$. This applies across a wide range of assumed uncertainties. To further circumvent systematics, we explore how DESI enables spectroscopic standardization via machine learning, offering a path toward a cosmology measurement independent of light-curve-based standardization. Finally, we discuss how early results from this program could inform future dark energy experiments.

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 proposes an alert-driven DESI spectroscopic follow-up program for Rubin-discovered supernovae, yielding 7500 near-peak spectra in one year without delaying the primary survey. It identifies that new SNe Ia at z ≲ 0.6 add the most constraining power for w0-wa and forecasts that a volume-limited, spectroscopically confirmed subset of 2300 SNe Ia at z < 0.3, when combined with existing SN, BAO, and CMB data, would drive tension with ΛCDM above 5σ if current best-fit w0-wa values persist. The work also explores an ML-based spectroscopic standardization path to reduce reliance on light-curve methods.

Significance. If the forecasts hold, the proposed program offers an efficient, low-systematics route to a decisive test of dynamical dark energy using only one year of data and existing facilities. The emphasis on volume-limited, spectroscopically confirmed low-z objects trades redshift leverage for control of key systematics, and the alert-triggered re-prioritization strategy demonstrates practical integration of Rubin and DESI. The ML standardization discussion provides a forward-looking alternative that could influence future survey design.

major comments (2)
  1. [Forecasting section] Forecasting section: the detailed error budgets, covariance assumptions, and simulation framework underlying the >5σ projection (and its claimed robustness across a wide range of uncertainties) are not presented with sufficient quantitative detail to allow independent verification of the result.
  2. [Survey yield section] Survey yield section: the mapping from 7500 spectra to the specific volume-limited sample of 2300 SNe Ia at z < 0.3 requires explicit justification of selection efficiency, completeness, and redshift distribution assumptions, as these directly determine the forecasted constraining power.
minor comments (2)
  1. [Abstract] The abstract and introduction could more precisely state the redshift range corresponding to 'near dark energy-matter equality' to aid readers unfamiliar with the w0-wa sensitivity peak.
  2. [Throughout] Notation for the w0-wa parametrization and the definition of tension with ΛCDM should be standardized between the text and any forecast figures.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their positive evaluation of the manuscript's significance and for the constructive major comments. We address each point below and will revise the manuscript to incorporate additional quantitative details and justifications as requested.

read point-by-point responses

  1. Referee: [Forecasting section] Forecasting section: the detailed error budgets, covariance assumptions, and simulation framework underlying the >5σ projection (and its claimed robustness across a wide range of uncertainties) are not presented with sufficient quantitative detail to allow independent verification of the result.

    Authors: We agree that the forecasting section would benefit from expanded quantitative detail to facilitate independent verification. The >5σ projection is derived from a Fisher matrix forecast combining the proposed low-z SN sample with existing SN, BAO, and CMB constraints, using standard covariance assumptions for each probe and testing robustness by varying key systematics (e.g., SN intrinsic scatter, calibration uncertainties) over ranges informed by current data. In the revised manuscript, we will add an expanded methods subsection and appendix that explicitly tabulates the error budgets, full covariance matrices (including cross-probe terms), the simulation framework for generating mock samples, and the specific uncertainty ranges explored. This will include the impact of each variation on the final significance to demonstrate the claimed robustness. revision: yes

  2. Referee: [Survey yield section] Survey yield section: the mapping from 7500 spectra to the specific volume-limited sample of 2300 SNe Ia at z < 0.3 requires explicit justification of selection efficiency, completeness, and redshift distribution assumptions, as these directly determine the forecasted constraining power.

    Authors: We acknowledge that the transition from the total 7500 near-peak spectra to the volume-limited subset of 2300 SNe Ia at z < 0.3 requires more explicit justification. This subset is obtained by applying a strict volume-limited cut (z < 0.3) to the expected alert-triggered DESI follow-up yield, with selection efficiencies derived from DESI's fiber allocation efficiency for bright transients, alert prioritization logic, and estimated spectroscopic completeness (>90% for z < 0.3 events based on prior DESI SN programs). In the revised version, we will add a dedicated subsection in the survey yield section (with supporting figures) that details the selection criteria, completeness fractions as a function of redshift and magnitude, the resulting redshift distribution, and the assumptions used (including references to DESI observing simulations and similar low-z SN surveys). This will directly link the numbers to the forecasted constraining power. revision: yes

Circularity Check

0 steps flagged

No significant circularity in conditional forecast

full rationale

The paper's central claim is a conditional forecast: assuming the current external best-fit w0-wa values from existing SN+BAO+CMB data persist, the addition of a new volume-limited sample of 2300 spectroscopically confirmed SNe Ia at z<0.3 is projected to increase tension with ΛCDM above 5σ. This projection relies on standard cosmological forecasting methods (e.g., Fisher matrices or similar) applied to the proposed sample's expected constraining power, combined with existing constraints. No step reduces by construction to self-definition, renames a fit as a prediction, or depends on load-bearing self-citations whose content is unverified. The argument is explicitly forward-looking and trades on external benchmarks for current tensions plus stated assumptions about future systematics, rendering the derivation self-contained.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The proposal depends on forecasts that take current cosmological parameter fits as given and assume specific levels of survey performance and systematic control.

free parameters (1)
  • assumed systematic and statistical uncertainties for new SNe Ia
    The >5 sigma projection is stated to hold across a wide range of these assumed values, making them load-bearing for the claim.
axioms (2)
  • domain assumption Current best-fit w0 and wa values from existing SN+BAO+CMB data represent the true underlying cosmology
    The tension forecast is conditioned on these values persisting.
  • domain assumption Re-prioritizing DESI tile visits can yield 7500 spectra without delaying the primary survey
    This operational assumption underpins the feasibility of the 2300-SN sample.

pith-pipeline@v0.9.0 · 5640 in / 1466 out tokens · 59011 ms · 2026-05-10T03:04:53.712336+00:00 · methodology

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

94 extracted references · 90 canonical work pages · 6 internal anchors

  1. [1]

    Survey and Other Telescope Technologies and Discoveries , year = 2002, editor =

    Overview of the Nearby Supernova Factory. Survey and Other Telescope Technologies and Discoveries , year = 2002, editor =. doi:10.1117/12.458107 , adsurl =

    work page doi:10.1117/12.458107 2002

  2. [2]

    , keywords =

    The La Silla Schmidt Southern Survey. , keywords =. doi:10.1088/1538-3873/ae02c5 , archivePrefix =. 2503.14579 , primaryClass =

    work page doi:10.1088/1538-3873/ae02c5

  3. [3]

    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

  4. [4]

    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

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

    work page doi:10.1051/0004-6361/201322068

  5. [5]

    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

  6. [6]

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac7c74

  7. [7]

    arXiv e-prints , keywords =

    Using Supernovae to Determine the Equation of State of the Dark Energy: Is Shallow Better than Deep?. arXiv e-prints , keywords =. doi:10.48550/arXiv.astro-ph/0204089 , archivePrefix =. astro-ph/0204089 , primaryClass =

    work page internal anchor Pith review doi:10.48550/arxiv.astro-ph/0204089

  8. [8]

    Perlmutter, et al., Measurements of the cosmological parameters Omega and Lambda from the first 7 super- novae at z>=0.35, Astrophys

    Measurements of the Cosmological Parameters and from the First Seven Supernovae at z >= 0.35. , keywords =. doi:10.1086/304265 , archivePrefix =. astro-ph/9608192 , primaryClass =

    work page doi:10.1086/304265

  9. [9]

    Philo- sophical Transactions of the Royal Society of London

    On the Mathematical Foundations of Theoretical Statistics. Philosophical Transactions of the Royal Society of London Series A , year = 1922, month = jan, volume =. doi:10.1098/rsta.1922.0009 , adsurl =

    work page doi:10.1098/rsta.1922.0009 1922

  10. [10]

    2023, AJ, 165, 144, doi: 10.3847/1538-3881/acb212 18

    The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument. , keywords =. doi:10.3847/1538-3881/acb212 , archivePrefix =. 2209.14482 , primaryClass =

    work page doi:10.3847/1538-3881/acb212

  11. [11]

    arXiv e-prints , keywords =

    Uniform Rolling: An LSST Observing Cadence Offering Sufficient Survey Uniformity for Comprehensive Cosmological Analysis. arXiv e-prints , keywords =. doi:10.48550/arXiv.2512.16478 , archivePrefix =. 2512.16478 , primaryClass =

    work page doi:10.48550/arxiv.2512.16478

  12. [12]

    Marshall, T

    Science-Driven Optimization of the LSST Observing Strategy. arXiv e-prints , keywords =. doi:10.48550/arXiv.1708.04058 , archivePrefix =. 1708.04058 , primaryClass =

    work page doi:10.48550/arxiv.1708.04058

  13. [13]

    arXiv e-prints , keywords =

    Optimizing the LSST Observing Strategy for Dark Energy Science: DESC Recommendations for the Wide-Fast-Deep Survey. arXiv e-prints , keywords =. doi:10.48550/arXiv.1812.00515 , archivePrefix =. 1812.00515 , primaryClass =

    work page doi:10.48550/arxiv.1812.00515

  14. [14]

    2022, ApJS, 259, 58, doi: 10.3847/1538-4365/ac5033

    The Impact of Observing Strategy on Cosmological Constraints with LSST. , keywords =. doi:10.3847/1538-4365/ac5033 , archivePrefix =. 2104.05676 , primaryClass =

    work page doi:10.3847/1538-4365/ac5033

  15. [15]

    , keywords =

    Evaluation of probabilistic photometric redshift estimation approaches for The Rubin Observatory Legacy Survey of Space and Time (LSST). , keywords =. doi:10.1093/mnras/staa2799 , archivePrefix =. 2001.03621 , primaryClass =

    work page doi:10.1093/mnras/staa2799 2001

  16. [16]

    , keywords =

    The Dark Energy Survey Supernova Program: Cosmological Biases from Host Galaxy Mismatch of Type Ia Supernovae. , keywords =. doi:10.3847/1538-4357/ad251d , archivePrefix =. 2307.13696 , primaryClass =

    work page doi:10.3847/1538-4357/ad251d

  17. [17]

    I., Dai, M., Ponder, K

    Are light curve classification metrics good proxies for SN Ia cosmological constraining power?. , keywords =. doi:10.1051/0004-6361/202346891 , archivePrefix =. 2305.14421 , primaryClass =

    work page doi:10.1051/0004-6361/202346891

  18. [18]

    , keywords =

    ZTF SN Ia DR2: Overview. , keywords =. doi:10.1051/0004-6361/202450388 , archivePrefix =. 2409.04346 , primaryClass =

    work page doi:10.1051/0004-6361/202450388

  19. [19]

    R., Millman, K

    Charles R. Harris and K. Jarrod Millman and St. Array programming with. 2020 , month = sep, journal =. doi:10.1038/s41586-020-2649-2 , publisher =

    work page doi:10.1038/s41586-020-2649-2 2020

  20. [20]

    Hunter, J. D. , Title =. Computing in Science & Engineering , Volume =

  21. [21]

    doi:10.5281/zenodo.168220 , version =

    sncosmo/sncosmo: v1.4.0. doi:10.5281/zenodo.168220 , version =

    work page doi:10.5281/zenodo.168220

  22. [22]

    , keywords =

    Absolute-magnitude Distributions of Supernovae. , keywords =. doi:10.1088/0004-6256/147/5/118 , archivePrefix =. 1403.5755 , primaryClass =

    work page doi:10.1088/0004-6256/147/5/118

  23. [23]

    , keywords =

    The Rate of Core Collapse Supernovae to Redshift 2.5 from the CANDELS and CLASH Supernova Surveys. , keywords =. doi:10.1088/0004-637X/813/2/93 , archivePrefix =. 1509.06574 , primaryClass =

    work page doi:10.1088/0004-637x/813/2/93

  24. [24]

    2010, Monthly Notices of the Royal Astronomical Society, 408, 1181, doi: 10.1111/j.1365-2966.2010.17197.x

    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

  25. [25]

    arXiv e-prints , keywords =

    Probabilistic Autoencoder. arXiv e-prints , keywords =. doi:10.48550/arXiv.2006.05479 , archivePrefix =. 2006.05479 , primaryClass =

    work page doi:10.48550/arxiv.2006.05479 2006

  26. [26]

    The Messenger , keywords =

    4MOST: Project overview and information for the First Call for Proposals. The Messenger , keywords =. doi:10.18727/0722-6691/5117 , archivePrefix =. 1903.02464 , primaryClass =

    work page doi:10.18727/0722-6691/5117 1903

  27. [27]

    Report of the Dark Energy Task Force

    Report of the Dark Energy Task Force. arXiv e-prints , keywords =. doi:10.48550/arXiv.astro-ph/0609591 , archivePrefix =. astro-ph/0609591 , primaryClass =

    work page Pith review doi:10.48550/arxiv.astro-ph/0609591

  28. [28]

    C., Kulkarni, S

    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

  29. [29]

    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

  30. [30]

    , archivePrefix = "arXiv", eprint =

    Techniques and Review of Absolute Flux Calibration from the Ultraviolet to the Mid-Infrared. , keywords =. doi:10.1086/677655 , archivePrefix =. 1406.1707 , primaryClass =

    work page doi:10.1086/677655

  31. [31]

    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

  32. [32]

    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

  33. [33]

    Comparative Direct Analysis of Type Ia Supernova Spectra. II. Maximum Light. , keywords =. doi:10.1086/502778 , archivePrefix =. astro-ph/0601048 , primaryClass =

    work page doi:10.1086/502778

  34. [34]

    and Carr, Anthony and Zuntz, Joe and Kessler, Rick and Davis, Tamara M

    The Pantheon+ Analysis: Cosmological Constraints. , keywords =. doi:10.3847/1538-4357/ac8e04 , archivePrefix =. 2202.04077 , primaryClass =

    work page doi:10.3847/1538-4357/ac8e04

  35. [35]

    and Clayton, Geoffrey C

    The Relationship between Infrared, Optical, and Ultraviolet Extinction. , keywords =. doi:10.1086/167900 , adsurl =

    work page doi:10.1086/167900

  36. [36]

    arXiv e-prints , keywords =

    Characterizing the Roman Grism Redshift Efficiency of Type Ia Supernova Host Galaxies for the High-Latitude Time-Domain Survey. arXiv e-prints , keywords =. doi:10.48550/arXiv.2512.09993 , archivePrefix =. 2512.09993 , primaryClass =

    work page doi:10.48550/arxiv.2512.09993

  37. [37]

    Chevallier and D

    Accelerating Universes with Scaling Dark Matter. International Journal of Modern Physics D , keywords =. doi:10.1142/S0218271801000822 , archivePrefix =. gr-qc/0009008 , primaryClass =

    work page doi:10.1142/s0218271801000822

  38. [38]

    , keywords =

    The Dark Energy Survey: Cosmology Results with 1500 New High-redshift Type Ia Supernovae Using the Full 5 yr Data Set. , keywords =. doi:10.3847/2041-8213/ad6f9f , archivePrefix =. 2401.02929 , primaryClass =

    work page doi:10.3847/2041-8213/ad6f9f 2041

  39. [39]

    The DESI Experiment Part I: Science,Targeting, and Survey Design

    The DESI Experiment Part I: Science,Targeting, and Survey Design. arXiv e-prints , keywords =. doi:10.48550/arXiv.1611.00036 , archivePrefix =. 1611.00036 , primaryClass =

    work page internal anchor Pith review doi:10.48550/arxiv.1611.00036

  40. [40]

    DESI DR2 results. II. Measurements of baryon acoustic oscillations and cosmological constraints. , keywords =. doi:10.1103/tr6y-kpc6 , archivePrefix =. 2503.14738 , primaryClass =

    work page doi:10.1103/tr6y-kpc6

  41. [41]

    Efstathiou, Evolving dark energy or supernovae systematics?, Mon

    Evolving dark energy or supernovae systematics?. , keywords =. doi:10.1093/mnras/staf301 , archivePrefix =. 2408.07175 , primaryClass =

    work page doi:10.1093/mnras/staf301

  42. [42]

    , keywords =

    Improving Cosmological Distance Measurements Using Twin Type Ia Supernovae. , keywords =. doi:10.1088/0004-637X/815/1/58 , archivePrefix =. 1511.01102 , primaryClass =

    work page doi:10.1088/0004-637x/815/1/58

  43. [43]

    , year = 1997, month = jan, volume =

    Optical Spectra of Supernovae. , year = 1997, month = jan, volume =. doi:10.1146/annurev.astro.35.1.309 , adsurl =

    work page doi:10.1146/annurev.astro.35.1.309 1997

  44. [44]

    1999, Publications of the Astronomical Society of the Pacific, 111, 63, doi: 10.1086/316293 33

    Correcting for the Effects of Interstellar Extinction. , keywords =. doi:10.1086/316293 , archivePrefix =. astro-ph/9809387 , primaryClass =

    work page doi:10.1086/316293

  45. [45]

    , keywords =

    The volumetric rate of normal type Ia supernovae in the local Universe discovered by the Palomar Transient Factory. , keywords =. doi:10.1093/mnras/stz807 , archivePrefix =. 1903.08580 , primaryClass =

    work page doi:10.1093/mnras/stz807 1903

  46. [46]

    , keywords =

    TiDES: The 4MOST Time Domain Extragalactic Survey. , keywords =. doi:10.3847/1538-4357/adff4e , archivePrefix =. 2501.16311 , primaryClass =

    work page doi:10.3847/1538-4357/adff4e

  47. [47]

    arXiv e-prints , keywords =

    ZTF-SEDm Type Ia supernova sample for Twins Embedding spectrophotometric standardisation. arXiv e-prints , keywords =. doi:10.48550/arXiv.2512.07696 , archivePrefix =. 2512.07696 , primaryClass =

    work page doi:10.48550/arxiv.2512.07696

  48. [48]

    , keywords =

    ZTF SN Ia DR2: Colour standardisation of type Ia supernovae and its dependence on the environment. , keywords =. doi:10.1051/0004-6361/202450943 , archivePrefix =. 2406.02072 , primaryClass =

    work page doi:10.1051/0004-6361/202450943

  49. [49]

    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

  50. [50]

    arXiv e-prints , keywords =

    The DESI Transients Survey: Legacy Classifications and Methodology. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.12611 , archivePrefix =. 2601.12611 , primaryClass =

    work page doi:10.48550/arxiv.2601.12611

  51. [51]

    Ivezi ´c, S

    LSST: From Science Drivers to Reference Design and Anticipated Data Products. , keywords =. doi:10.3847/1538-4357/ab042c , archivePrefix =. 0805.2366 , primaryClass =

    work page doi:10.3847/1538-4357/ab042c

  52. [52]

    , 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

  53. [53]

    , keywords =

    Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee. , keywords =. doi:10.3847/1538-4357/ae07c9 , archivePrefix =. 2506.04402 , primaryClass =

    work page doi:10.3847/1538-4357/ae07c9

  54. [54]

    , 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

  55. [55]

    , keywords =

    Models and Simulations for the Photometric LSST Astronomical Time Series Classification Challenge (PLAsTiCC). , keywords =. doi:10.1088/1538-3873/ab26f1 , archivePrefix =. 1903.11756 , primaryClass =

    work page doi:10.1088/1538-3873/ab26f1 1903

  56. [56]

    Astroparticle Physics , keywords =

    Optimal extraction of cosmological information from supernova data in the presence of calibration uncertainties. Astroparticle Physics , keywords =. doi:10.1016/j.astropartphys.2005.09.005 , archivePrefix =. astro-ph/0508252 , primaryClass =

    work page doi:10.1016/j.astropartphys.2005.09.005 2005

  57. [57]

    Nature Astronomy , keywords =

    Looking beyond lambda. Nature Astronomy , keywords =. doi:10.1038/s41550-025-02627-2 , archivePrefix =. 2509.00359 , primaryClass =

    work page doi:10.1038/s41550-025-02627-2

  58. [58]

    Exploring the expansion history of the universe

    Exploring the Expansion History of the Universe. , keywords =. doi:10.1103/PhysRevLett.90.091301 , archivePrefix =. astro-ph/0208512 , primaryClass =

    work page doi:10.1103/physrevlett.90.091301

  59. [59]

    Lodhaet al.[DESI], Extended dark energy analysis using DESI DR2 BAO measure- ments, Phys

    Extended dark energy analysis using DESI DR2 BAO measurements. , keywords =. doi:10.1103/w4c6-1r5j , archivePrefix =. 2503.14743 , primaryClass =

    work page doi:10.1103/w4c6-1r5j

  60. [60]

    2018, arXiv e-prints, arXiv:1809.01669

    The LSST Dark Energy Science Collaboration (DESC) Science Requirements Document. arXiv e-prints , keywords =. doi:10.48550/arXiv.1809.01669 , archivePrefix =. 1809.01669 , primaryClass =

    work page doi:10.48550/arxiv.1809.01669

  61. [61]

    LSST Science Book, Version 2.0

    LSST Science Book, Version 2.0. arXiv e-prints , keywords =. doi:10.48550/arXiv.0912.0201 , archivePrefix =. 0912.0201 , primaryClass =

    work page Pith review doi:10.48550/arxiv.0912.0201

  62. [62]

    Meddelanden fran Lunds Astronomiska Observatorium Serie I , year = 1925, month = feb, volume =

    A contribution to the problem of determining the distribution in space of the stars. Meddelanden fran Lunds Astronomiska Observatorium Serie I , year = 1925, month = feb, volume =

    1925

  63. [63]

    , keywords =

    Using Host Galaxy Photometric Redshifts to Improve Cosmological Constraints with Type Ia Supernovae in the LSST Era. , keywords =. doi:10.3847/1538-4357/acb057 , archivePrefix =. 2210.07560 , primaryClass =

    work page doi:10.3847/1538-4357/acb057

  64. [64]

    arXiv e-prints , keywords =

    A Fully Photometric Approach to Type Ia Supernova Cosmology in the LSST Era: Host Galaxy Redshifts and Supernova Classification. arXiv e-prints , keywords =

  65. [65]

    , keywords =

    Understanding type Ia supernovae through their U-band spectra. , keywords =. doi:10.1051/0004-6361/201732137 , archivePrefix =. 1801.01834 , primaryClass =

    work page doi:10.1051/0004-6361/201732137

  66. [66]

    1999, apj, 517, 565, doi: 10.1086/307221

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

    work page internal anchor Pith review doi:10.1086/307221

  67. [67]

    , keywords =

    SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements. , keywords =. doi:10.3847/1538-4357/ac93f9 , archivePrefix =. 2209.05594 , primaryClass =

    work page doi:10.3847/1538-4357/ac93f9

  68. [68]

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

    work page doi:10.1051/0004-6361/201833910 2018

  69. [69]

    Popovic et al.,A Reassessment of the Pantheon+ and DES 5YR Calibration Uncertainties: Dovekie,2506.05471

    A Reassessment of the Pantheon+ and DES 5YR Calibration Uncertainties: Dovekie. arXiv e-prints , keywords =. doi:10.48550/arXiv.2506.05471 , archivePrefix =. 2506.05471 , primaryClass =

    work page doi:10.48550/arxiv.2506.05471

  70. [70]

    The Dark Energy Survey Supernova Program: A Reanalysis Of Cosmology Results And Evidence For Evolving Dark Energy With An Updated Type Ia Supernova Calibration

    The Dark Energy Survey Supernova Program: A Reanalysis Of Cosmology Results And Evidence For Evolving Dark Energy With An Updated Type Ia Supernova Calibration. arXiv e-prints , keywords =. doi:10.48550/arXiv.2511.07517 , archivePrefix =. 2511.07517 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2511.07517

  71. [71]

    G., Filippenko, A

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

    work page Pith review doi:10.1086/300499

  72. [72]

    , keywords =

    Type Ia Supernova Rate Measurements to Redshift 2.5 from CANDELS: Searching for Prompt Explosions in the Early Universe. , keywords =. doi:10.1088/0004-6256/148/1/13 , archivePrefix =. 1401.7978 , primaryClass =

    work page doi:10.1088/0004-6256/148/1/13

  73. [73]

    Rubin Observatory, Nancy Grace Roman Space Telescope, and Euclid Mission: Constraining Dark Energy with Type Ia Supernovae

    Synergies between Vera C. Rubin Observatory, Nancy Grace Roman Space Telescope, and Euclid Mission: Constraining Dark Energy with Type Ia Supernovae. arXiv e-prints , keywords =. doi:10.48550/arXiv.2104.01199 , archivePrefix =. 2104.01199 , primaryClass =

    work page doi:10.48550/arxiv.2104.01199

  74. [74]

    M., Baltay, C., Hounsell, R., et al

    A Reference Survey for Supernova Cosmology with the Nancy Grace Roman Space Telescope. arXiv e-prints , keywords =. doi:10.48550/arXiv.2111.03081 , archivePrefix =. 2111.03081 , primaryClass =

    work page doi:10.48550/arxiv.2111.03081

  75. [75]

    arXiv e-prints , keywords =

    Fishing for the Optimal Roman High Latitude Time Domain Survey: Cosmological Constraints for 1,000 Possible Surveys. arXiv e-prints , keywords =. doi:10.48550/arXiv.2506.04327 , archivePrefix =. 2506.04327 , primaryClass =

    work page doi:10.48550/arxiv.2506.04327

  76. [76]

    Rubinet al., Union Through UNITY: Cosmology with 2,000 SNe Using a Unified Bayesian Framework, Astrophys

    Union through UNITY: Cosmology with 2000 SNe Using a Unified Bayesian Framework. , keywords =. doi:10.3847/1538-4357/adc0a5 , archivePrefix =. 2311.12098 , primaryClass =

    work page doi:10.3847/1538-4357/adc0a5 2000

  77. [77]

    Rubin, T

    Banana Split: Improved Cosmological Constraints with Two Light-Curve-Shape and Color Populations Using Union3.1+UNITY1.8. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.19854 , archivePrefix =. 2601.19854 , primaryClass =

    work page doi:10.48550/arxiv.2601.19854

  78. [78]

    F., Kirkby, D., Schlegel, D

    Survey Operations for the Dark Energy Spectroscopic Instrument. , keywords =. doi:10.3847/1538-3881/ad0832 , archivePrefix =. 2306.06309 , primaryClass =

    work page doi:10.3847/1538-3881/ad0832

  79. [79]

    , keywords =

    A Probabilistic Autoencoder for Type Ia Supernova Spectral Time Series. , keywords =. doi:10.3847/1538-4357/ac7c08 , archivePrefix =. 2207.07645 , primaryClass =

    work page doi:10.3847/1538-4357/ac7c08

  80. [80]

    , keywords =

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

Showing first 80 references.