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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: We also find that quintessence models that best…

Centred on one claim: 14 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 claims14 claims and 13 dependencies, in 1 group of joined claims; within a group, foundations on the left and what rests on them to the right.14 claims, 1 step deep, Physics and AstronomyWe 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)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)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)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)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)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)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)With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s…: unchecked, credence 0.55, stakes 12.6, reliance 4.0With 18 peaks in the…We find that this result is driven by low-$z$ supernova data.: unchecked, credence 0.55, stakes 6.8After validating our analysis against simulations, we find $f_{\rm NL}^{\rm equil.}= 207 \pm 292\, , f_{\rm NL}^{\rm or…: unchecked, credence 0.55, stakes 6.7Even with the additional flexibility introduced by non-parametric approaches, such as binning and Gaussian Processes, w…: unchecked, credence 0.55, stakes 3.5We also find that quintessence models that best fit observational data can predict a value for the dark energy equation…: unchecked, credence 0.55, stakes 7.2We also find that quintessence…In this paper, we reveal that this preference is significantly biased by an external low-redshift supernova (low-$z$ SN…: unchecked, credence 0.55, stakes 6.0None 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 6.9Bayesian evidence further shows that combining DES-SN5Y or Union3 supernova samples with CMB + DESI~DR2 produces measur…: unchecked, credence 0.55, stakes 4.2A 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…: unchecked, credence 0.55, stakes 14.8, reliance 1.0A 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…Our findings indicate that in these parameterizations, the deviation from ($w_0$,$w_{1}$)=(-1,0) becomes more pronounce…: unchecked, credence 0.55, stakes 5.2We 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…

● 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 14.8 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
With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the s…○ uncheckedyes0.55012.6—
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…
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…
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…
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…○ uncheckedyes0.5506.9In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with…
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…
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…○ uncheckedyes0.55014.8—
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—
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…
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—
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.