A Precise Cluster Mass Profile Averaged from the Highest-Quality Lensing Data

Adi Zitrin (Tel Aviv U.); Bilbao); Dan Coe (STScI); Elinor Medezinski (JHU); Keiichi Umetsu (ASIAA); Marc Postman (STScI); Tom Broadhurst (Basque U.

RECORD

A Precise Cluster Mass Profile Averaged from the Highest-Quality Lensing Data

Keiichi Umetsu (ASIAA), Tom Broadhurst (Basque U., Bilbao), Adi Zitrin (Tel Aviv U.), Elinor Medezinski (JHU), Dan Coe (STScI), Marc Postman (STScI)

Cosmology and Nongalactic Astrophysics · Submitted 2 May 2011

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We show that the projected mass profile has a continuously steepening gradient out to beyond the virial radius, in remarkably good agreement with the standard Navarro-Frenk-White form predicted for the family of CDM-dominated halos in gravitational equilibrium.

how it is stated · asserted 1.00 read the record →

Comment (0) Read on arXiv ↗

Cite ▾

arXiv ID1105.0444 (version 2)

Pith IDRBNB2BDI, Pith's permanent record of this paper and its review

CitationAdi Zitrin (Tel Aviv U.), Bilbao), Dan Coe (STScI), Elinor Medezinski (JHU), Keiichi Umetsu (ASIAA), Marc Postman (STScI), Tom Broadhurst (Basque U.. "A Precise Cluster Mass Profile Averaged from the Highest-Quality Lensing Data." arXiv:1105.0444 (2011). https://pith.science/paper/RBNB2BDI

Claim paper

The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Open the compiled record

Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 7,941 input tokens, $0.0003 reported.

What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.86 · human participants 0.01 · controlled comparison 0.07 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.45 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; show every role.

We outline our methods for obtaining high precision mass profiles, combining independent weak-lensing distortion, magnification, and strong-lensing measurements. For massive clusters the strong and weak lensing regimes contribute equal logarithmic coverage of the radial profile. The utility of high-quality data is limited by the cosmic noise from large scale structure along the line of sight. This noise is overcome when stacking clusters, as too are the effects of cluster asphericity and substructure, permitting a stringent test of theoretical models. We derive a mean radial mass profile of four similar mass clusters of high-quality HST and Subaru images, in the range R=40kpc/h to 2800kpc/h, where the inner radial boundary is sufficiently large to avoid smoothing from miscentering effects. The stacked mass profile is detected at 58-sigma significance over the entire radial range, with the contribution from the cosmic noise included. We show that the projected mass profile has a continuously steepening gradient out to beyond the virial radius, in remarkably good agreement with the standard Navarro-Frenk-White form predicted for the family of CDM-dominated halos in gravitational equilibrium. The central slope is constrained to lie in the range, -dln{\rho}/dln{r}=0.89^{+0.27}_{-0.39}. The mean concentration is c_{vir}=7.68^{+0.42}_{-0.40} (at a mean virial mass 1.54^{+0.11}_{-0.10}\times 10^{15} M_{sun}/h), which is high for relaxed, high-mass clusters, but consistent with LCDM when a sizable projection bias estimated from N-body simulations is considered. This possible tension will be more definitively explored with new cluster surveys, such as CLASH, LoCuSS, Subaru HSC, and XXM-XXL, to construct the c-M relation over a wider mass range.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We outline our methods for obtaining high precision mass profiles, combining independent weak-lensing distortion, magnification, and strong-lensing measurements.	method 0.98	0.88	0.03	asserted 0.90
s1	For massive clusters the strong and weak lensing regimes contribute equal logarithmic coverage of the radial profile.	method 0.53	0.37	0.03	asserted 1.00
s2	The utility of high-quality data is limited by the cosmic noise from large scale structure along the line of sight.	limitation 0.62	0.20	0.02	asserted 1.00
s3	This noise is overcome when stacking clusters, as too are the effects of cluster asphericity and substructure, permitting a stringent test of theoretical models.	method 0.78	0.29	0.07	asserted 1.00
s4	We derive a mean radial mass profile of four similar mass clusters of high-quality HST and Subaru images, in the range R=40kpc/h to 2800kpc/h, where the inner radial boundary is sufficiently large to avoid smoothing from miscentering effects.	contribution 0.57	0.97	0.07	asserted 1.00
s5	The stacked mass profile is detected at 58-sigma significance over the entire radial range, with the contribution from the cosmic noise included.	result 1.00	0.96	0.12	asserted 1.00
s6	We show that the projected mass profile has a continuously steepening gradient out to beyond the virial radius, in remarkably good agreement with the standard Navarro-Frenk-White form predicted for the family of CDM-dominated halos in gravitational equilibrium.	result 0.93	0.93	0.69	asserted 1.00
s7	The central slope is constrained to lie in the range, -dln{\rho}/dln{r}=0.89^{+0.27}_{-0.39}.	result 1.00	0.95	0.08	asserted 1.00
s8	The mean concentration is c_{vir}=7.68^{+0.42}_{-0.40} (at a mean virial mass 1.54^{+0.11}_{-0.10}\times 10^{15} M_{sun}/h), which is high for relaxed, high-mass clusters, but consistent with LCDM when a sizable projection bias estimated from N-body simulations is considered.	result 0.92	0.92	0.15	asserted 0.60
s9	This possible tension will be more definitively explored with new cluster surveys, such as CLASH, LoCuSS, Subaru HSC, and XXM-XXL, to construct the c-M relation over a wider mass range.	future work 1.00	0.11	0.03	hedged possibility 0.91

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from analysis of existing data 0.72.

What was examined, and what was not

sources read

arXiv listing abstract v2

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

not run

S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original abstract

We outline our methods for obtaining high precision mass profiles, combining independent weak-lensing distortion, magnification, and strong-lensing measurements. For massive clusters the strong and weak lensing regimes contribute equal logarithmic coverage of the radial profile. The utility of high-quality data is limited by the cosmic noise from large scale structure along the line of sight. This noise is overcome when stacking clusters, as too are the effects of cluster asphericity and substructure, permitting a stringent test of theoretical models. We derive a mean radial mass profile of four similar mass clusters of high-quality HST and Subaru images, in the range R=40kpc/h to 2800kpc/h, where the inner radial boundary is sufficiently large to avoid smoothing from miscentering effects. The stacked mass profile is detected at 58-sigma significance over the entire radial range, with the contribution from the cosmic noise included. We show that the projected mass profile has a continuously steepening gradient out to beyond the virial radius, in remarkably good agreement with the standard Navarro-Frenk-White form predicted for the family of CDM-dominated halos in gravitational equilibrium. The central slope is constrained to lie in the range, -dln{\rho}/dln{r}=0.89^{+0.27}_{-0.39}. The mean concentration is c_{vir}=7.68^{+0.42}_{-0.40} (at a mean virial mass 1.54^{+0.11}_{-0.10}\times 10^{15} M_{sun}/h), which is high for relaxed, high-mass clusters, but consistent with LCDM when a sizable projection bias estimated from N-body simulations is considered. This possible tension will be more definitively explored with new cluster surveys, such as CLASH, LoCuSS, Subaru HSC, and XXM-XXL, to construct the c-M relation over a wider mass range.

Human review

How Pith checks papers → · Full audit of this paper →

References

Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Testing general scalar-tensor gravity and massive gravity with cluster lensing
astro-ph.CO 2013-02 conditional novelty 6.0 of 10

In Horndeski scalar-tensor gravity the scalar field's second derivative peaks sharply at the Vainshtein radius, producing a dip in cluster lensing convergence at a fixed angular radius.
Cold dark matter heats up
astro-ph.CO 2014-02 accept novelty 3.0 of 10

Repeated, fast gas outflows can irreversibly transfer energy to central dark matter, converting cusps into cores and reconciling cold dark matter with observed galaxy density profiles.

How the literature uses it

8 arXiv papers cite this in 23 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 14 sentences without a confident label

Uses its method or tool 1 paper

By maximizing $lnP(|)$ with respect to $$, we obtain the desired expression for the stacked weak-lensing estimator $$ as [ref] : [equation]

Cluster-galaxy weak lensing · Stacked weak-lensing estimator · 0.91

Uses its data or values 2 papers

Utilizing the observational data of the surface mass density in [ref] and the differential surface mass density in [ref] , we obtained the constraint on the parameters $μ$ and $ϵ$ for the first time, assuming the NFW profile, the gNFW profile and the Einasto profile as the halo density profile.

Testing gravity with halo density profiles observed through gravitational lensing · Summary and Conclusion · 1.00
The points with the error bars indicate the observational data for the high-mass cluster A1689 provided by Umetsu et al. [ref] .

Testing general scalar-tensor gravity and massive gravity with cluster lensing · Gravitational lensing in modified gravity · 0.88

Cites it as support 1 paper

This is now observationally confirmed on galaxy cluster scales [ref] .

N-body simulations of gravitational dynamics · Past, recent, and future astrophysical modelling · 0.98

What it cites · 87 sentences without a confident label

Builds on 1 paper

This extends recent weak-lensing work by [ref] to include the central strong-lensing information in a stacking analysis, for full radial coverage.

Cluster Mass Profiles from a Bayesian Analysis of Weak Lensing Distortion and Magnification Measurements: Applications to Subaru Data · Discussion and Conclusions · 1.00

Uses the method or tool of 8 papers

Since the noise in different clusters is uncorrelated, the mass profiles of individual clusters can be co-added according to [ref]

Cluster Mass Profiles from a Bayesian Analysis of Weak Lensing Distortion and Magnification Measurements: Applications to Subaru Data · Stacked Lensing Analysis · 0.99
We employ the radial dependence of the gNFW lensing profiles given by [ref] .

A Catalog of Mass Models for Gravitational Lensing · Results · 0.99
Here we take into account the effect of uncorrelated large scale structure projected along the line of sight on the error covariance matrix $C^lss_ij$ as $C=C^stat+C^lss$, where $C^lss$ is given as [ref] [equation] Here $C^κκ(l)$ is the weak-lensing power spectrum as a function of angular multipole $l$ evaluated for a given source population and a cosmology, and $Ĵ_0(lθ_i)$ is the Bessel function of the first kind and order zero averaged over the $i$th annulus between $θ_i,1$ and $θ_i,2 (>θ_i,1)$, given as [equation] We will assume the concordance $Λ$CDM cosmological model of [ref] and use the fitting formula of [ref] to compute the nonlinear mass power spectrum that enters in equation ([ref]).

Noise in strong lensing cosmography · Combining Weak and Strong Lensing · 0.98

Uses data or values from 1 paper

Note, no scaling has been applied to match the mass normalizations between the four clusters, which span a relatively narrow range in mass, $1.3M_vir/(10^15 M_⊙ h^-1)2.3$ [ref] .

Cluster Mass Profiles from a Bayesian Analysis of Weak Lensing Distortion and Magnification Measurements: Applications to Subaru Data · Results · 0.83

Compares with 3 papers

The resulting best-fit NFW parameters from the stacked analysis are consistent with the respective sample weighted means of the individual NFW model fits obtained by [ref] : $⟨M_vir⟩=1.44±0.11 ×10^15M_⊙ h^-1$ and $⟨c_vir⟩= 7.76±0.79$.

Cluster Mass Profiles from a Bayesian Analysis of Weak Lensing Distortion and Magnification Measurements: Applications to Subaru Data · Results · 0.98
Our results are in agreement with recent high-resolution simulations, which find asymptotic inner slopes somewhat shallower than unity, $γ_3D(r→0)0.9$, for galaxy- and cluster-sized $Λ$CDM halos [ref] .

Empirical models for Dark Matter Halos. I. Nonparametric Construction of Density Profiles and Comparison with Parametric Models · Discussion and Conclusions · 0.80
Our results are in agreement with recent high-resolution simulations, which find asymptotic inner slopes somewhat shallower than unity, $γ_3D(r→0)0.9$, for galaxy- and cluster-sized $Λ$CDM halos [ref] .

Empirical Models for Dark Matter Halos. II. Inner profile slopes, dynamical profiles, and rho/sigma^3 · Discussion and Conclusions · 0.80

Cites as background 6 papers

Note NFW define this profile for halos which they identify as in virial equilibrium, in terms of the simulated CDM particles [ref] .

A Universal Density Profile from Hierarchical Clustering · Discussion and Conclusions · 0.96
Theoretical progress has been made in understanding of the form of this profile in terms of the dynamical structure using both numerical and analytical approaches [ref] ,

The Phase-Space Density Profiles of Cold Dark Matter Halos · Introduction · 0.90
The local area distortion due to gravitational lensing, or magnification, is given by the inverse Jacobian determinant, [equation] which can influence the observed surface density of background sources, expanding the area of sky, and enhancing the observed flux of background sources [ref] .

Mapping Cluster Mass Distributions via Gravitational Lensing of Background Galaxies · Basis of Cluster Lensing · 0.93

Discussion

Know something about this paper? Leave a comment, or highlight any passage above to comment on it.