The network
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: For a base $Λ$CDM cosmology we find $σ_8 Ω_m^{0…
Centred on one claim: 29 claims within its whole group of it.
● 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 16.6 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
| Claim | Status | Checkable | Credence | Use | Stakes | Rests on |
|---|---|---|---|---|---|---|
| We combine our CMB lensing measurements with CMB anisotropies to constrain extensions of $Λ$CDM, limiting the sum of th… | ○ unchecked | yes | 0.55 | 0 | 9.5 | Without 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 $… | ○ unchecked | yes | 0.55 | 0 | 4.5 | A combined analysis gives dark matter density Ω c h 2 = 0.120 ± 0.001, baryon density Ω b h 2 = 0.0224 ± 0.0001, scalar… |
| With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s… | ○ unchecked | yes | 0.55 | 0 | 12.9 | — |
| We find that this result is driven by low-$z$ supernova data. | ○ unchecked | yes | 0.55 | 0 | 6.8 | With 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… | ○ unchecked | yes | 0.55 | 0 | 7.3 | Without 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… | ○ unchecked | yes | 0.55 | 0 | 0.0 | Without 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… | ○ unchecked | yes | 0.55 | 0 | 6.7 | With 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… | ○ unchecked | yes | 0.55 | 0 | 3.5 | When 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… | ○ unchecked | yes | 0.55 | 0 | 7.2 | In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with… |
| Models without phantom behaviour are compatible with the data at the $2σ$ CL. | ○ unchecked | yes | 0.55 | 0 | 5.8 | 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… |
| 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… | ○ unchecked | yes | 0.55 | 0 | 8.2 | 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…, Without the need for specific code by the user, interdependencies between different stages of a model pipeline are expl… |
| In this paper, we reveal that this preference is significantly biased by an external low-redshift supernova (low-$z$ SN… | ○ unchecked | yes | 0.55 | 0 | 6.0 | In 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… | ○ unchecked | yes | 0.55 | 0 | 5.6 | From 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. | ○ unchecked | yes | 0.55 | 0 | 2.0 | With 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… | ○ unchecked | yes | 0.55 | 0 | 7.9 | In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with… |
| Combining DESI data with Cosmic Microwave Background measurements and several late-time background probes, the tightest… | ○ unchecked | yes | 0.55 | 0 | 2.8 | We 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… | ○ unchecked | yes | 0.55 | 0 | 0.0 | When 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… | ○ unchecked | yes | 0.55 | 0 | 5.9 | 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… |
| Bayesian evidence further shows that combining DES-SN5Y or Union3 supernova samples with CMB + DESI~DR2 produces measur… | ○ unchecked | yes | 0.55 | 0 | 4.2 | With 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.… | ○ unchecked | yes | 0.55 | 0 | 6.2 | — |
| 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… | ○ unchecked | yes | 0.55 | 0 | 16.6 | — |
| In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with… | ○ unchecked | yes | 0.55 | 0 | 12.7 | — |
| The present-day value of the DE EoS remains in the quintessence regime according to our results, and no significant evi… | ○ unchecked | yes | 0.55 | 0 | 3.9 | Without 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… | ○ unchecked | yes | 0.55 | 0 | 12.3 | — |
| Our results highlight that a unified dark fluid with evolving equation of state and null sound speed is sufficient to p… | ○ unchecked | yes | 0.55 | 0 | 2.6 | With 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… |
| Our findings indicate that in these parameterizations, the deviation from ($w_0$,$w_{1}$)=(-1,0) becomes more pronounce… | ○ unchecked | yes | 0.55 | 0 | 5.2 | In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with… |
| The low-multipole 100x143 GHz EE cross-spectrum constrains the reionization optical-depth parameter $τ$ to better than… | ○ unchecked | yes | 0.55 | 0 | 11.2 | — |
| We interpret this result in terms of a quintessential scalar field and demonstrate that it can explain the DESI result… | ○ unchecked | yes | 0.55 | 0 | 6.9 | In 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… | ○ unchecked | yes | 0.55 | 0 | 11.1 | — |
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.