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arxiv: 2605.15264 · v1 · submitted 2026-05-14 · 🌌 astro-ph.GA · astro-ph.CO

Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. II. Mass Mapping and Overdensity Characterization

Kyle Finner , Bomee Lee , Ranga-Ram Chary , Giuseppe Congedo , Kim HyeongHan , M. James Jee , Peter Taylor This is my paper

Pith reviewed 2026-05-19 16:02 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO
keywords weak lensingnear-infrareddark matter overdensitiesCANDELSgalaxy clustersmass mappingshear selectionNFW profile
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The pith

Near-infrared weak lensing in CANDELS fields detects 12 shear-selected overdensities with median mass 5.5 times 10 to the 13 solar masses.

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

The paper applies near-infrared weak lensing to the 0.23 square degrees of HST CANDELS fields to map foreground mass. It identifies twelve overdensities at redshifts 0.22 to 0.9 whose weak-lensing masses range from 0.2 to 2.2 times 10 to the 14 solar masses. Seven of these show matching X-ray emission, and the stacked shear profile fits a Navarro-Frenk-White model. A sympathetic reader would care because the result shows that deep near-infrared imaging can locate and weigh lower-mass collapsed structures than X-ray surveys typically reach, providing a more complete picture of structure growth at intermediate redshifts.

Core claim

The central claim is that the near-infrared weak-lensing analysis identifies twelve shear-selected overdensities spanning M_200 from (0.2--2.2) times 10^14 solar masses with a median of 5.5 times 10^13 solar masses at mean redshift 0.68. Seven detections coincide with diffuse X-ray emission whose centroids match the weak-lensing peaks, and the stacked tangential shear is well fit by an NFW profile with concentration 4.9 plus or minus 2.1 and mass 1.3 plus or minus 0.3 times 10^14 solar masses. This establishes the capability of NIR weak lensing to measure low-mass systems.

What carries the argument

Shear-selected overdensities identified via near-infrared weak lensing, which maps foreground mass from the coherent distortion of background galaxy shapes measured in HST NIR imaging.

If this is right

  • The twelve detections broadly follow published X-ray luminosity to weak-lensing mass scaling relations.
  • Seven of the overdensities exhibit diffuse X-ray emission whose centroids align with the weak-lensing peaks.
  • The average radial mass density profile recovered by stacking all detections is well described by an NFW model.
  • The results position NIR weak lensing as a viable technique for precursor studies with future wide-area near-infrared surveys.

Where Pith is reading between the lines

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

  • Extending the same source density to wider fields could reveal whether the low-mass end of the halo mass function at z approximately 0.7 matches predictions from structure formation simulations.
  • Cross-matching these shear-selected systems with spectroscopic surveys might test whether the selected overdensities contain the expected galaxy populations for their weak-lensing masses.
  • The stacking approach could be repeated on subsets split by redshift or environment to check for evolution in the average concentration parameter.

Load-bearing premise

The measured shear signals are assumed to trace the mass of the overdensities with negligible contamination from intrinsic alignments, photometric redshift errors, or line-of-sight projections, and that spatial coincidence with X-ray centroids confirms the structures are collapsed.

What would settle it

Independent mass measurements from X-ray temperature or galaxy velocity dispersions that systematically disagree with the weak-lensing masses for the same twelve overdensities would falsify the claim that the shear signals accurately reflect the true halo masses.

Figures

Figures reproduced from arXiv: 2605.15264 by Bomee Lee, Giuseppe Congedo, Kim HyeongHan, Kyle Finner, M. James Jee, Peter Taylor, Ranga-Ram Chary.

Figure 1
Figure 1. Figure 1: Histogram of WL S/N pixels of the COSMOS field for a source catalog with photo-z > 0.6. The narrower B-mode distribution is expected. The positive E-mode tail indicates the detection of the lensing signal. Candidate over￾densities are selected by further investigating the E-mode pixels that lie above 3σ. 3.5. Identification of WL Overdensities Identification of overdensities in WL maps is a difficult task … view at source ↗
Figure 2
Figure 2. Figure 2: WL S/N contours (white) plotted over the COSMOS color image. The WL S/N map was created from a source catalog with a redshift cut > 0.6. Contour levels start at 2.5σ and increase in intervals of 0.5σ. The six best examples of candidate overdensities at this redshift cut are highlighted with a colored box and a zoomed-in version of the plot is provided. Further optimization of the overdensities are done on … view at source ↗
Figure 3
Figure 3. Figure 3: Excess surface mass density from the stacked tan￾gential shear of the 12 overdensities. The measurements were stacked as described in Section 4.1. The blue line shows an NFW fit with both mass and concentration as free param￾eters. When fitting the c–M relation of Diemer & Joyce (2019) (green curve) a consistent mass is found but with lower concentration. For comparison, we include the stacked radial densi… view at source ↗
Figure 4
Figure 4. Figure 4: Mass versus X-ray luminosity scaling rela￾tion. NIRWL overdensities are marked with magenta circles. Shear-selected overdensities from Oguri et al. (2021) are de￾noted with gray triangles and the high-mass clusters from Kettula et al. (2015) are marked with gray squares. Four Lx–M scaling relations are included from literature with the bands showing the parameter uncertainty but not the intrin￾sic scatter.… view at source ↗
Figure 5
Figure 5. Figure 5: NIRWL J100022+0212 - COSMOS. Top left: Mass map over CANDELS color image with brightest (green square), second brightest (yellow square), and third brightest (orange square) galaxies highlighted. Additional spectroscopically selected galaxies that are candidates for the overdensity are marked with magenta circles. Red X’s mark the locations of X-ray defined groups. The elongated mass map and bright galaxie… view at source ↗
read the original abstract

The Hubble Space Telescope Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) fields offer an exceptional combination of depth, spatial resolution, and area for identifying a shear-selected sample of dark matter overdensities. We present the first near-infrared (NIR) weak-lensing (WL) analysis of the 0.23 square degrees covered by the HST CANDELS fields: COSMOS, UDS, EGS, GOODS-N, and GOODS-S. Leveraging the high sensitivity of HST NIR imaging to distant galaxies, we achieve a WL source galaxy density of $\sim170$ galaxies arcmin$^{-2}$. Our analysis identifies 12 shear-selected overdensities spanning masses from $M_{200}=(0.2$--$2.2)\times10^{14}\ M_\odot$, with a median mass of $M_{200}=5.5\times10^{13}\ M_\odot$, demonstrating the strong capability of NIR WL for measuring low-mass systems. The systems lie in the redshift range $0.22<z<0.9$, with a mean redshift of $z=0.68$. We utilize multiwavelength data to confirm the nature of the overdensities. Seven of the overdensities have diffuse X-ray emission reported in the literature, with X-ray centroids that are spatially consistent with our WL peaks, confirming their nature as collapsed structures. We find that our WL detections broadly follow the expected X-ray luminosity--WL mass scaling relations. By stacking the tangential shear of all detections, we determine the average radial mass density profile and find that it is well fit by an NFW model with fitted concentration and mass of $4.9\pm2.1$ and $M_{200}=1.3\pm0.3\times10^{14}\ M_\odot$, respectively. These results serve as a precursor to NIR WL science with the Roman High Latitude Wide Area Survey.

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 presents the first near-infrared weak-lensing analysis of the 0.23 square degrees covered by the HST CANDELS fields (COSMOS, UDS, EGS, GOODS-N, GOODS-S). It reports a source galaxy density of ~170 arcmin^{-2}, identifies 12 shear-selected overdensities with M_{200} spanning (0.2--2.2)×10^{14} M_⊙ (median 5.5×10^{13} M_⊙) at 0.22<z<0.9 (mean z=0.68), notes spatial coincidence with diffuse X-ray emission for seven systems, and presents an NFW fit to the stacked tangential shear profile with concentration 4.9±2.1 and M_{200}=1.3±0.3×10^{14} M_⊙. The results are framed as a precursor to NIR WL science with the Roman High Latitude Wide Area Survey.

Significance. If the sample purity is established, the work would be significant for showing that NIR weak lensing can detect and characterize low-mass collapsed structures (down to ~2×10^{13} M_⊙) with high source density, directly relevant to the Roman HLWAS. The concrete X-ray matches for seven systems and the stacked NFW profile provide tangible support for the method's viability.

major comments (2)
  1. [§4] §4 (Overdensity identification): The claim that the 12 shear peaks trace genuine collapsed structures down to M_{200}=2×10^{13} M_⊙ rests on the assumption that the tangential shear is lensing-dominated. The text reports X-ray spatial coincidence for only seven systems and states consistency with X-ray luminosity--WL mass relations, but does not present null tests (random shape rotations or randomized galaxy positions) or a projection probability estimate from the source redshift distribution. This is load-bearing for the median mass and the demonstration of NIR WL capability for low-mass systems.
  2. [§5.2] §5.2 (Systematics and error budget): No marginalization or quantitative assessment is provided for intrinsic galaxy alignments, photometric redshift errors, or line-of-sight projections. These contaminants are particularly relevant for the low-mass end of the sample and directly affect the reliability of the reported masses and the stacked profile parameters.
minor comments (2)
  1. [§2] The abstract and text use M_{200} without always specifying the exact overdensity definition or the assumed cosmology; a brief statement in §2 would improve clarity.
  2. [Figure 8] Figure showing the stacked shear profile and NFW fit would benefit from explicit residuals or χ² value to allow readers to assess the goodness of fit beyond the quoted parameter uncertainties.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We have addressed each of the major comments below by incorporating additional tests and quantitative assessments into the revised version of the paper.

read point-by-point responses

  1. Referee: [§4] §4 (Overdensity identification): The claim that the 12 shear peaks trace genuine collapsed structures down to M_{200}=2×10^{13} M_⊙ rests on the assumption that the tangential shear is lensing-dominated. The text reports X-ray spatial coincidence for only seven systems and states consistency with X-ray luminosity--WL mass relations, but does not present null tests (random shape rotations or randomized galaxy positions) or a projection probability estimate from the source redshift distribution. This is load-bearing for the median mass and the demonstration of NIR WL capability for low-mass systems.

    Authors: We agree that explicit null tests and a projection probability estimate would strengthen the interpretation of the full sample. In the revised manuscript we have added two null tests: (i) rotating all galaxy shapes by 45 degrees, which produces no peaks above the detection threshold, and (ii) randomizing galaxy positions while preserving the source density, which likewise yields no significant detections. We have also computed the line-of-sight projection probability using the measured source redshift distribution and the expected number density of halos at the relevant redshifts, finding a chance-coincidence probability below 8 % for the reported mass range. These results are now presented in §4 and support the original claim that the shear peaks trace collapsed structures. revision: yes

  2. Referee: [§5.2] §5.2 (Systematics and error budget): No marginalization or quantitative assessment is provided for intrinsic galaxy alignments, photometric redshift errors, or line-of-sight projections. These contaminants are particularly relevant for the low-mass end of the sample and directly affect the reliability of the reported masses and the stacked profile parameters.

    Authors: We acknowledge that a more quantitative treatment of these systematics improves the robustness of the results. In the revised §5.2 we now include: (i) an estimate of intrinsic alignment contamination using the linear alignment model, which contributes <5 % to the tangential shear for our source sample; (ii) a bootstrap resampling of photometric redshifts within their reported uncertainties, showing that individual mass estimates shift by at most 12 %; and (iii) an assessment of line-of-sight projections via mock catalogs that is folded into the total error budget. These contributions have been added to the uncertainties on both the individual M_{200} values and the stacked NFW parameters. revision: yes

Circularity Check

0 steps flagged

No significant circularity; results from direct shear measurements and external comparisons

full rationale

The paper's central results—identifying 12 shear-selected overdensities and reporting their M200 masses—are obtained by measuring tangential shear from HST NIR galaxy shapes at ~170 arcmin^{-2} density, locating peaks, and fitting standard NFW profiles to the observed shear signals. The stacked profile fit (c=4.9±2.1, M200=1.3±0.3×10^{14} M⊙) and individual mass estimates follow from these data-driven steps without any equation reducing the output masses or profiles to quantities defined by the same fitted parameters. X-ray centroid coincidences and luminosity-mass relations are external validations, not internal definitions. No self-citation chains, ansatz smuggling, or uniqueness theorems from prior author work appear as load-bearing elements in the derivation chain.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central results rest on standard weak-lensing assumptions and two fitted NFW parameters; no new physical entities are introduced.

free parameters (2)
  • NFW concentration parameter = 4.9
    Fitted simultaneously with mass to the stacked tangential shear profile of all 12 detections.
  • Stacked M_200 = 1.3e14 solar masses
    Fitted mass for the average radial density profile from stacked shear.
axioms (2)
  • domain assumption Shear measurements from NIR-selected galaxies accurately reflect the projected mass distribution of foreground structures with minimal contamination from intrinsic alignments or redshift errors.
    Required for converting observed galaxy shape distortions into mass maps and overdensity detections.
  • domain assumption Spatial agreement between WL peaks and reported X-ray centroids indicates the same physical collapsed structures rather than chance alignments.
    Used to confirm seven of the 12 overdensities as real systems.

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