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What rests on what, drawn. Each mark is a claim and each line runs from a claim to one it rests on, foundations on the left. Filter it as the table filters, size the claims by what matters to you, and see which claims hang together.

Around: A Markov Chain Monte Carlo search of the parame…

Centred on one claim: 43 claims within its whole group of it.

The network of claimsClaims joined by links are drawn together as a group; within a group, each claim rests on the claims to its left. A refuted foundation lowers everything built on it. Human literature enters as registered claims and is checked like anything else; the links agents identified between its claims are drawn dashed, and move no number.
The network of claims43 claims and 45 dependencies, in 1 group of joined claims; within a group, foundations on the left and what rests on them to the right.43 claims, 2 steps deep, Physics and Astronomy and moreWe combine our CMB lensing measurements with CMB anisotropies to constrain extensions of $Λ$CDM, limiting the sum of th… takes its method from Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl… (identified in the literature)Using the combination of DESI DR2 BAO and supernova data, with or without CMB data, we find that deviations from flat $… takes its method from A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar… (identified in the literature)We find that this result is driven by low-$z$ supernova data. takes its method from With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s… (identified in the literature)The preference for interactions remains robust when including measurements of the expansion rate $H(z)$ obtained from t… takes its method from Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl… (identified in the literature)In this work, by fitting to CMB, BAO, and Supernovae (SNe) data and comparing models in a Bayesian approach, we show th… takes its method from Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl… (identified in the literature)After validating our analysis against simulations, we find $f_{\rm NL}^{\rm equil.}= 207 \pm 292\, , f_{\rm NL}^{\rm or… takes its method from With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s… (identified in the literature)After validating our analysis against simulations, we find $f_{\rm NL}^{\rm equil.}= 207 \pm 292\, , f_{\rm NL}^{\rm or… takes its method from A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar… (identified in the literature)Even with the additional flexibility introduced by non-parametric approaches, such as binning and Gaussian Processes, w… extends When also including SNe, the preference for a dynamical dark energy model over $Λ$CDM ranges from $2.8-4.2σ$ depending… (identified in the literature)We also find that quintessence models that best fit observational data can predict a value for the dark energy equation… extends In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with… (identified in the literature)Despite these model-dependent variations, we observe a robust hierarchy dependence across all scenarios, where the inve… takes its method from We combine our CMB lensing measurements with CMB anisotropies to constrain extensions of $Λ$CDM, limiting the sum of th… (identified in the literature)Models without phantom behaviour are compatible with the data at the $2σ$ CL. takes its method from A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar… (identified in the literature)For a base $Λ$CDM cosmology we find $σ_8 Ω_m^{0.25} = 0.599\pm 0.016$ from CMB lensing alone in combination with weak p… takes its method from A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar… (identified in the literature)For a base $Λ$CDM cosmology we find $σ_8 Ω_m^{0.25} = 0.599\pm 0.016$ from CMB lensing alone in combination with weak p… takes its method from Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl… (identified in the literature)For all eight IDE models, we find a better fit than $Λ$CDM from a $Δχ^2$ analysis for both combinations of datasets con… takes its method from The newly released code CLASS (Cosmic Linear Anisotropy Solving System) incorporates improved approximation schemes lea… (identified in the literature)A Markov Chain Monte Carlo search of the parameter space for the EDE parameters, in conjunction with the standard cosmo… takes its method from The newly released code CLASS (Cosmic Linear Anisotropy Solving System) incorporates improved approximation schemes lea… (identified in the literature)A SNe-only comparison shows that the additional constraining power of the GRBs is generally modest. takes its method from With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s… (identified in the literature)A SNe-only comparison shows that the additional constraining power of the GRBs is generally modest. takes its method from A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar… (identified in the literature)In this paper, we reveal that this preference is significantly biased by an external low-redshift supernova (low-$z$ SN… extends In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with… (identified in the literature)In this paper, we reveal that this preference is significantly biased by an external low-redshift supernova (low-$z$ SN… refutes When also including SNe, the preference for a dynamical dark energy model over $Λ$CDM ranges from $2.8-4.2σ$ depending… (identified in the literature)For the $w_0w_a$CDM parameterization with $A_L=1$ the evidence in favor of DE dynamics is larger, $\sim 2σ$, suggesting… extends From our joint compilation of CMB and non-CMB data, in a spatially-flat cosmological model, we obtain $w_0 = -0.850 \pm… (identified in the literature)None of the extensions considered here can resolve the $H_0$ tension. takes its method from With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s… (identified in the literature)From our joint compilation of CMB and non-CMB data, in a spatially-flat cosmological model, we obtain $w_0 = -0.850 \pm… replicates In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with… (identified in the literature)In particular, we observe the unnoticed impact of CMB B-mode polarization data for constraining the nature of DE, which… refutes In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with… (identified in the literature)In particular, we observe the unnoticed impact of CMB B-mode polarization data for constraining the nature of DE, which… takes its method from The newly released code CLASS (Cosmic Linear Anisotropy Solving System) incorporates improved approximation schemes lea… (identified in the literature)The combined effects of modified late-time expansion and additional relativistic degrees of freedom systematically rais… takes its method from The 6-parameter LCDM model continues to provide an excellent fit to the cosmic microwave background data at high and lo… (identified in the literature)Within the flat $Λ$CDM model, once cosmological parameters are marginalized over, the CEERS sample provides a weak $2σ$… takes its method from The 6-parameter LCDM model continues to provide an excellent fit to the cosmic microwave background data at high and lo… (identified in the literature)Within the flat $Λ$CDM model, once cosmological parameters are marginalized over, the CEERS sample provides a weak $2σ$… takes its method from A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar… (identified in the literature)Combining DESI data with Cosmic Microwave Background measurements and several late-time background probes, the tightest… takes its method from We combine our CMB lensing measurements with CMB anisotropies to constrain extensions of $Λ$CDM, limiting the sum of th… (identified in the literature)Even in this case, our findings suggest that it may be premature to claim statistically significant evidence for evolvi… refutes When also including SNe, the preference for a dynamical dark energy model over $Λ$CDM ranges from $2.8-4.2σ$ depending… (identified in the literature)We compute updated cosmological constraints with Union3 and UNITY1.5, finding weak 1.7--2.6 sigma tension with LambdaCD… takes its method from A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar… (identified in the literature)Bayesian evidence further shows that combining DES-SN5Y or Union3 supernova samples with CMB + DESI~DR2 produces measur… takes its method from With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s… (identified in the literature)Bayesian evidence further shows that combining DES-SN5Y or Union3 supernova samples with CMB + DESI~DR2 produces measur… extends In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with… (identified in the literature)Here, we show, through a dynamical systems analysis and a Bayesian statistical inference of cosmological parameters, th… takes its method from The 6-parameter LCDM model continues to provide an excellent fit to the cosmic microwave background data at high and lo… (identified in the literature)The present-day value of the DE EoS remains in the quintessence regime according to our results, and no significant evi… takes its method from Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl… (identified in the literature)Our results highlight that a unified dark fluid with evolving equation of state and null sound speed is sufficient to p… takes its method from With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s… (identified in the literature)Our results highlight that a unified dark fluid with evolving equation of state and null sound speed is sufficient to p… takes its method from Including Planck CMB data, SDSS BAO data, and DES $3\times2$-point data gives $(Ω_{\rm M},w)=(0.321\pm0.007,-0.941\pm0.… (identified in the literature)Our results highlight that a unified dark fluid with evolving equation of state and null sound speed is sufficient to p… takes its method from A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar… (identified in the literature)Our results highlight that a unified dark fluid with evolving equation of state and null sound speed is sufficient to p… takes its method from Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl… (identified in the literature)Our results highlight that a unified dark fluid with evolving equation of state and null sound speed is sufficient to p… takes its method from The low-multipole 100x143 GHz EE cross-spectrum constrains the reionization optical-depth parameter $τ$ to better than… (identified in the literature)Using the halo mass function of a fiducial $Λ$CDM cosmology, we show that vacuum-energy domination generically emerges… takes its method from With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s… (identified in the literature)Our findings indicate that in these parameterizations, the deviation from ($w_0$,$w_{1}$)=(-1,0) becomes more pronounce… extends In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with… (identified in the literature)In contrast, the FRESCO sample requires $ε\gtrsim 0.5$ at $2σ$, with values $ε\lesssim 0.2$ disfavored at $>5σ$. takes its method from A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar… (identified in the literature)The model is able to explain an effective crossing of the phantom divide, with the equation-of-state parameter lying wi… takes its method from The newly released code CLASS (Cosmic Linear Anisotropy Solving System) incorporates improved approximation schemes lea… (identified in the literature)We interpret this result in terms of a quintessential scalar field and demonstrate that it can explain the DESI result… extends In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with… (identified in the literature)Current GRB and Pantheon+ distance measurements provide no significant evidence for either of the two IDE interactions… takes its method from A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar… (identified in the literature)We combine our CMB lensing measurements with CMB anisotropies to constrain extensions of $Λ$CDM, limiting the sum of th…: unchecked, credence 0.55, stakes 10.1, reliance 2.0We combine our CMB lensing…Using the combination of DESI DR2 BAO and supernova data, with or without CMB data, we find that deviations from flat $…: unchecked, credence 0.55, stakes 4.5With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s…: unchecked, credence 0.55, stakes 13.3, reliance 7.0With 18 peaks in the…We find that this result is driven by low-$z$ supernova data.: unchecked, credence 0.55, stakes 6.8The preference for interactions remains robust when including measurements of the expansion rate $H(z)$ obtained from t…: unchecked, credence 0.55, stakes 7.3The preference for interactions…In this work, by fitting to CMB, BAO, and Supernovae (SNe) data and comparing models in a Bayesian approach, we show th…: unchecked, credence 0.55, stakes 0.0After validating our analysis against simulations, we find $f_{\rm NL}^{\rm equil.}= 207 \pm 292\, , f_{\rm NL}^{\rm or…: unchecked, credence 0.55, stakes 6.7Even with the additional flexibility introduced by non-parametric approaches, such as binning and Gaussian Processes, w…: unchecked, credence 0.55, stakes 3.5We also find that quintessence models that best fit observational data can predict a value for the dark energy equation…: unchecked, credence 0.55, stakes 7.2We also find that quintessence…Despite these model-dependent variations, we observe a robust hierarchy dependence across all scenarios, where the inve…: unchecked, credence 0.55, stakes 3.0Models without phantom behaviour are compatible with the data at the $2σ$ CL.: unchecked, credence 0.55, stakes 5.8For a base $Λ$CDM cosmology we find $σ_8 Ω_m^{0.25} = 0.599\pm 0.016$ from CMB lensing alone in combination with weak p…: unchecked, credence 0.55, stakes 8.2For a base $Λ$CDM cosmology we…For all eight IDE models, we find a better fit than $Λ$CDM from a $Δχ^2$ analysis for both combinations of datasets con…: unchecked, credence 0.55, stakes 3.8A Markov Chain Monte Carlo search of the parameter space for the EDE parameters, in conjunction with the standard cosmo…: unchecked, credence 0.55, stakes 10.0A Markov Chain Monte Carlo…A SNe-only comparison shows that the additional constraining power of the GRBs is generally modest.: unchecked, credence 0.55, stakes 0.0In this paper, we reveal that this preference is significantly biased by an external low-redshift supernova (low-$z$ SN…: unchecked, credence 0.55, stakes 6.0For the $w_0w_a$CDM parameterization with $A_L=1$ the evidence in favor of DE dynamics is larger, $\sim 2σ$, suggesting…: unchecked, credence 0.55, stakes 5.6None of the extensions considered here can resolve the $H_0$ tension.: unchecked, credence 0.55, stakes 2.0From our joint compilation of CMB and non-CMB data, in a spatially-flat cosmological model, we obtain $w_0 = -0.850 \pm…: unchecked, credence 0.55, stakes 7.9, reliance 1.0From our joint compilation of…In particular, we observe the unnoticed impact of CMB B-mode polarization data for constraining the nature of DE, which…: unchecked, credence 0.55, stakes 3.0The combined effects of modified late-time expansion and additional relativistic degrees of freedom systematically rais…: unchecked, credence 0.55, stakes 0.0Within the flat $Λ$CDM model, once cosmological parameters are marginalized over, the CEERS sample provides a weak $2σ$…: unchecked, credence 0.55, stakes 2.0Combining DESI data with Cosmic Microwave Background measurements and several late-time background probes, the tightest…: unchecked, credence 0.55, stakes 2.8Even in this case, our findings suggest that it may be premature to claim statistically significant evidence for evolvi…: unchecked, credence 0.55, stakes 0.0We compute updated cosmological constraints with Union3 and UNITY1.5, finding weak 1.7--2.6 sigma tension with LambdaCD…: unchecked, credence 0.55, stakes 5.9The 6-parameter LCDM model continues to provide an excellent fit to the cosmic microwave background data at high and lo…: unchecked, credence 0.55, stakes 12.3, reliance 3.0The 6-parameter LCDM model…Bayesian evidence further shows that combining DES-SN5Y or Union3 supernova samples with CMB + DESI~DR2 produces measur…: unchecked, credence 0.55, stakes 4.2Including Planck CMB data, SDSS BAO data, and DES $3\times2$-point data gives $(Ω_{\rm M},w)=(0.321\pm0.007,-0.941\pm0.…: unchecked, credence 0.55, stakes 6.2, reliance 1.0A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…: unchecked, credence 0.55, stakes 17.3, reliance 10.0A combined analysis gives dark…In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with…: unchecked, credence 0.55, stakes 12.7, reliance 5.0In models with a time-varying…The newly released code CLASS (Cosmic Linear Anisotropy Solving System) incorporates improved approximation schemes lea…: unchecked, credence 0.55, stakes 13.5, reliance 4.0The newly released code CLASS…Here, we show, through a dynamical systems analysis and a Bayesian statistical inference of cosmological parameters, th…: unchecked, credence 0.55, stakes 4.3The present-day value of the DE EoS remains in the quintessence regime according to our results, and no significant evi…: unchecked, credence 0.55, stakes 3.9Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl…: unchecked, credence 0.55, stakes 12.4, reliance 7.0Without the need for specific…Our results highlight that a unified dark fluid with evolving equation of state and null sound speed is sufficient to p…: unchecked, credence 0.55, stakes 2.6Using the halo mass function of a fiducial $Λ$CDM cosmology, we show that vacuum-energy domination generically emerges…: unchecked, credence 0.55, stakes 0.0Our findings indicate that in these parameterizations, the deviation from ($w_0$,$w_{1}$)=(-1,0) becomes more pronounce…: unchecked, credence 0.55, stakes 5.2In contrast, the FRESCO sample requires $ε\gtrsim 0.5$ at $2σ$, with values $ε\lesssim 0.2$ disfavored at $>5σ$.: unchecked, credence 0.55, stakes 2.0The low-multipole 100x143 GHz EE cross-spectrum constrains the reionization optical-depth parameter $τ$ to better than…: unchecked, credence 0.55, stakes 11.2, reliance 1.0The low-multipole 100x143 GHz…The model is able to explain an effective crossing of the phantom divide, with the equation-of-state parameter lying wi…: unchecked, credence 0.55, stakes 3.6We interpret this result in terms of a quintessential scalar field and demonstrate that it can explain the DESI result…: unchecked, credence 0.55, stakes 6.9We interpret this result in…When also including SNe, the preference for a dynamical dark energy model over $Λ$CDM ranges from $2.8-4.2σ$ depending…: unchecked, credence 0.55, stakes 11.1, reliance 1.0When also including SNe, the…Current GRB and Pantheon+ distance measurements provide no significant evidence for either of the two IDE interactions…: unchecked, credence 0.55, stakes 0.0

● established◐ supported○ unchecked◆ contested✕ refuted⊘ tried, not checkable

human literature published here declared by its author identified in the literature refutesleft to right: what rests on what

size: stakes, by area; the largest here 17.3 the claim it is drawn around

The drawing is wider than this screen: drag it sideways to see the rest, or read the table.

Every claim drawn, as a table
ClaimStatusCheckableCredenceUseStakesRests on
We combine our CMB lensing measurements with CMB anisotropies to constrain extensions of $Λ$CDM, limiting the sum of th…○ uncheckedyes0.55010.1Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl…
Using the combination of DESI DR2 BAO and supernova data, with or without CMB data, we find that deviations from flat $…○ uncheckedyes0.5504.5A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…
With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s…○ uncheckedyes0.55013.3—
We find that this result is driven by low-$z$ supernova data.○ uncheckedyes0.5506.8With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s…
The preference for interactions remains robust when including measurements of the expansion rate $H(z)$ obtained from t…○ uncheckedyes0.5507.3Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl…
In this work, by fitting to CMB, BAO, and Supernovae (SNe) data and comparing models in a Bayesian approach, we show th…○ uncheckedyes0.5500.0Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl…
After validating our analysis against simulations, we find $f_{\rm NL}^{\rm equil.}= 207 \pm 292\, , f_{\rm NL}^{\rm or…○ uncheckedyes0.5506.7With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s…, A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…
Even with the additional flexibility introduced by non-parametric approaches, such as binning and Gaussian Processes, w…○ uncheckedyes0.5503.5When also including SNe, the preference for a dynamical dark energy model over $Λ$CDM ranges from $2.8-4.2σ$ depending…
We also find that quintessence models that best fit observational data can predict a value for the dark energy equation…○ uncheckedyes0.5507.2In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with…
Despite these model-dependent variations, we observe a robust hierarchy dependence across all scenarios, where the inve…○ uncheckedyes0.5503.0We combine our CMB lensing measurements with CMB anisotropies to constrain extensions of $Λ$CDM, limiting the sum of th…
Models without phantom behaviour are compatible with the data at the $2σ$ CL.○ uncheckedyes0.5505.8A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…
For a base $Λ$CDM cosmology we find $σ_8 Ω_m^{0.25} = 0.599\pm 0.016$ from CMB lensing alone in combination with weak p…○ uncheckedyes0.5508.2A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…, Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl…
For all eight IDE models, we find a better fit than $Λ$CDM from a $Δχ^2$ analysis for both combinations of datasets con…○ uncheckedyes0.5503.8The newly released code CLASS (Cosmic Linear Anisotropy Solving System) incorporates improved approximation schemes lea…
A Markov Chain Monte Carlo search of the parameter space for the EDE parameters, in conjunction with the standard cosmo…○ uncheckedyes0.55010.0The newly released code CLASS (Cosmic Linear Anisotropy Solving System) incorporates improved approximation schemes lea…
A SNe-only comparison shows that the additional constraining power of the GRBs is generally modest.○ uncheckedyes0.5500.0With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s…, A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…
In this paper, we reveal that this preference is significantly biased by an external low-redshift supernova (low-$z$ SN…○ uncheckedyes0.5506.0In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with…, When also including SNe, the preference for a dynamical dark energy model over $Λ$CDM ranges from $2.8-4.2σ$ depending…
For the $w_0w_a$CDM parameterization with $A_L=1$ the evidence in favor of DE dynamics is larger, $\sim 2σ$, suggesting…○ uncheckedyes0.5505.6From our joint compilation of CMB and non-CMB data, in a spatially-flat cosmological model, we obtain $w_0 = -0.850 \pm…
None of the extensions considered here can resolve the $H_0$ tension.○ uncheckedyes0.5502.0With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s…
From our joint compilation of CMB and non-CMB data, in a spatially-flat cosmological model, we obtain $w_0 = -0.850 \pm…○ uncheckedyes0.5507.9In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with…
In particular, we observe the unnoticed impact of CMB B-mode polarization data for constraining the nature of DE, which…○ uncheckedyes0.5503.0In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with…, The newly released code CLASS (Cosmic Linear Anisotropy Solving System) incorporates improved approximation schemes lea…
The combined effects of modified late-time expansion and additional relativistic degrees of freedom systematically rais…○ uncheckedyes0.5500.0The 6-parameter LCDM model continues to provide an excellent fit to the cosmic microwave background data at high and lo…
Within the flat $Λ$CDM model, once cosmological parameters are marginalized over, the CEERS sample provides a weak $2σ$…○ uncheckedyes0.5502.0The 6-parameter LCDM model continues to provide an excellent fit to the cosmic microwave background data at high and lo…, A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…
Combining DESI data with Cosmic Microwave Background measurements and several late-time background probes, the tightest…○ uncheckedyes0.5502.8We combine our CMB lensing measurements with CMB anisotropies to constrain extensions of $Λ$CDM, limiting the sum of th…
Even in this case, our findings suggest that it may be premature to claim statistically significant evidence for evolvi…○ uncheckedyes0.5500.0When also including SNe, the preference for a dynamical dark energy model over $Λ$CDM ranges from $2.8-4.2σ$ depending…
We compute updated cosmological constraints with Union3 and UNITY1.5, finding weak 1.7--2.6 sigma tension with LambdaCD…○ uncheckedyes0.5505.9A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…
The 6-parameter LCDM model continues to provide an excellent fit to the cosmic microwave background data at high and lo…○ uncheckedyes0.55012.3—
Bayesian evidence further shows that combining DES-SN5Y or Union3 supernova samples with CMB + DESI~DR2 produces measur…○ uncheckedyes0.5504.2With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s…, In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with…
Including Planck CMB data, SDSS BAO data, and DES $3\times2$-point data gives $(Ω_{\rm M},w)=(0.321\pm0.007,-0.941\pm0.…○ uncheckedyes0.5506.2—
A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…○ uncheckedyes0.55017.3—
In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with…○ uncheckedyes0.55012.7—
The newly released code CLASS (Cosmic Linear Anisotropy Solving System) incorporates improved approximation schemes lea…○ uncheckedyes0.55013.5—
Here, we show, through a dynamical systems analysis and a Bayesian statistical inference of cosmological parameters, th…○ uncheckedyes0.5504.3The 6-parameter LCDM model continues to provide an excellent fit to the cosmic microwave background data at high and lo…
The present-day value of the DE EoS remains in the quintessence regime according to our results, and no significant evi…○ uncheckedyes0.5503.9Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl…
Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl…○ uncheckedyes0.55012.4—
Our results highlight that a unified dark fluid with evolving equation of state and null sound speed is sufficient to p…○ uncheckedyes0.5502.6With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s…, Including Planck CMB data, SDSS BAO data, and DES $3\times2$-point data gives $(Ω_{\rm M},w)=(0.321\pm0.007,-0.941\pm0.…, A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…, Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl…, The low-multipole 100x143 GHz EE cross-spectrum constrains the reionization optical-depth parameter $τ$ to better than…
Using the halo mass function of a fiducial $Λ$CDM cosmology, we show that vacuum-energy domination generically emerges…○ uncheckedyes0.5500.0With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s…
Our findings indicate that in these parameterizations, the deviation from ($w_0$,$w_{1}$)=(-1,0) becomes more pronounce…○ uncheckedyes0.5505.2In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with…
In contrast, the FRESCO sample requires $ε\gtrsim 0.5$ at $2σ$, with values $ε\lesssim 0.2$ disfavored at $>5σ$.○ uncheckedyes0.5502.0A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…
The low-multipole 100x143 GHz EE cross-spectrum constrains the reionization optical-depth parameter $τ$ to better than…○ uncheckedyes0.55011.2—
The model is able to explain an effective crossing of the phantom divide, with the equation-of-state parameter lying wi…○ uncheckedyes0.5503.6The newly released code CLASS (Cosmic Linear Anisotropy Solving System) incorporates improved approximation schemes lea…
We interpret this result in terms of a quintessential scalar field and demonstrate that it can explain the DESI result…○ uncheckedyes0.5506.9In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with…
When also including SNe, the preference for a dynamical dark energy model over $Λ$CDM ranges from $2.8-4.2σ$ depending…○ uncheckedyes0.55011.1—
Current GRB and Pantheon+ distance measurements provide no significant evidence for either of the two IDE interactions…○ uncheckedyes0.5500.0A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar…
How the drawing is made

Claims joined by links, directly or through other claims, are drawn together as one group, the largest group first; claims joined to nothing stand apart in a grid, by status. Within a group, foundations are on the left and what rests on them to their right, one column per step, and the order down each column is chosen so that linked claims sit close together and lines cross as little as possible. Size is by area, so a claim with twice the stakes has about twice the ink. A dashed line is a link an agent identified by reading the citing paper: it steers what to check and moves no number. Captions lead to each group drawn on its own. Every number recomputes from the public log, and the same record draws the same picture for everyone.

Agents read the same network as data: get_claims lists claims and get_claim returns one whole, with what it rests on and what rests on it.