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REVIEW 3 major objections 6 minor 1 cited by

On the relationship between the cosmic web and the alignment of galaxies and AGN jets

T0 review · 3 major / 6 minor · reviewed 2026-08-09 · deepseek-v4-flash

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Pith's one-line read The cosmic web imprints on galaxies: near filaments, massive galaxies align with the filament while their radio jets point more randomly.

desk verdict New and worth reading, but the jet-randomization half of the abstract rests on a post-hoc subsample and a p=0.036; the galaxy-filament alignment is the solid half. read the letter →

arxiv 2502.03730 v1 pith:NZF22TQE submitted 2025-02-06 astro-ph.GA

Seoyoung Lyla Jung , I. H. Whittam , M. J. Jarvis , C. L. Hale , M. N. Tudorache , T. Yasin This is my paper · ORCID
classification astro-ph.GA
keywords galaxies:evolutionjetslarge-scalestructureofUniversemethods:observationalcosmicfilamentsradiogalaxiesintrinsicalignmentAGNfeedback
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper aims to establish that the cosmic web leaves a direct, measurable imprint on both the shapes of massive galaxies and the directions of their radio jets. Combining the LoTSS DR2 radio survey, DESI Legacy optical imaging, and an SDSS-derived filament catalogue, it reports that galaxies with stellar mass above $10^{11}\,\mathrm{M_\odot}$ within about $11\,\mathrm{Mpc}$ of the nearest filament tend to have their optical major axes aligned with the filament, with the strongest signal within about $6\,\mathrm{Mpc}$. It also reports that radio jets, which are generally perpendicular to the host galaxy's major axis, become more randomly oriented relative to the host within about $8\,\mathrm{Mpc}$ of a filament. The authors interpret this pair of results as evidence that filament-directed mergers build up massive galaxies while feeding the central black hole chaotically, which would explain why coherent large-scale radio jet alignments are weak and why AGN feedback in filaments should act preferentially along dark-matter-halo minor axes.

What carries the argument

The analysis compares three orientation vectors: the optical major axis from DESI Legacy ellipticity components, the radio jet position angle from LoTSS DR2 (deconvolved Gaussian position angle or composite-source convex-hull angle), and the local orientation of the nearest segment of an SDSS DR12 filament catalogue. Distances to filaments are computed in 3D Cartesian coordinates, and because a galaxy and its closest filament sampling point can be separated on the sky, position angles are parallel-transported along the great circle connecting the two locations before the dot product is taken. The statistical workhorse is the skewness of the resulting angle distributions, with one- and two-sample Kolmogorov-Smirnov tests used to compare each distribution against uniformity and against other distance bins.

What would settle it

Use a spectroscopic sample whose completeness does not vary with filament proximity, for example a magnitude-limited survey covering the same volume, and recompute the skewness of the galaxy-filament angle distribution in the $D_{\rm fil} \le 6\,\mathrm{Mpc}$ bin and the misaligned-jet fraction in the $D_{\rm fil} \le 8\,\mathrm{Mpc}$ bin. If the positive skewness and the excess of misaligned jets disappear, the claimed environmental imprint is a selection artifact rather than a physical alignment.

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Extended reading notes

Core claim

The paper's central claim is that distance to the nearest cosmic filament is a controlling variable for galaxy and jet orientations. For the GMRG sample of 84,409 massive radio galaxies with spectroscopic redshifts, the angle between the optical major axis and the nearest filament is not uniform within $D_{\rm fil} \le 6.36\,\mathrm{Mpc}$: it is positively skewed toward $0^\circ$ (one-sample KS $p = 0.00073$), and a two-sample KS test separates the inner bin from the rest of the sample at $p = 0.002$. The alignment persists in the $6.36\!-\!10.96\,\mathrm{Mpc}$ bin ($p = 0.0145$) and disappears beyond $\sim 11\,\mathrm{Mpc}$, and it is stronger for higher-ellipticity galaxies and for filaments with lower line-of-sight inclination. For the extended jet subsample with $|\epsilon_{\rm opt}| > 0.1$, the usual preference for jets to lie perpendicular to the galaxy major axis is diluted at $D_{\rm fil} \le 7.98\,\mathrm{Mpc}$: the misaligned-jet fraction is about $60\%$ there versus about $56\%$ at larger distances, and a two-sample KS test gives $p = 0.036$. The paper takes these results as evidence that massive galaxies in filaments grow by mergers channeled along the filament, while chaotic gas accretion onto the black hole randomizes jet directions, so AGN feedback is preferentially deposited along halo minor axes inside filaments.

Load-bearing premise

The load-bearing premise is that the chance a galaxy has a spectroscopic redshift does not depend on how close it is to a cosmic filament or on how its galaxy and jet are oriented.

Editorial extensions

If this is right

  • If the central claim is right, cosmic shear surveys must treat galaxies within about $11\,\mathrm{Mpc}$ of filaments as intrinsically aligned with the filament, rather than randomly oriented, which biases weak-lensing measurements in filament regions.
  • Searches for coherent large-scale radio jet orientations over tens of Mpc should expect weak or absent signals, because the filament environment acts to randomize jet directions rather than to align them.
  • AGN feedback in massive filament galaxies is preferentially deposited along the minor axes of their dark matter halos, making the circumgalactic medium around such galaxies anisotropic in an environment-dependent way.
  • The observed azimuthal segregation of blue and quenched satellite galaxies around cluster members can partly arise from filament-directed assembly and jet orientation established before infall, rather than only from in-cluster processes.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Going beyond the paper, a natural next test is to split filament galaxies by merger stage: the merger-alignment picture predicts stronger galaxy-filament alignment and stronger jet randomization in galaxies with tidal features or close companions.
  • Because the extended jet sample is restricted to luminous, large radio sources, the chaotic-accretion interpretation could be probed with fainter or younger jets, which should show an even stronger distance-from-filament dependence if reorientation is frequent.
  • The quoted scales of about $11\,\mathrm{Mpc}$ and $8\,\mathrm{Mpc}$ are tied to one filament finder's definition; comparing with filament catalogues built from velocity-shear or tidal-field criteria would show how much of the signal is definition-dependent.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 6 minor

Summary. The paper uses LoTSS DR2 radio sources with spectroscopic redshifts, DESI Legacy imaging shapes, and the Malavasi et al. (2020) SDSS filament catalogue to study alignments between optical major axes, radio jet position angles, and the nearest cosmic filaments. It reports two main findings: (i) for massive galaxies (log M*/M_sun > 11), the optical major axis tends to align with the nearest filament for D_fil < ~11 Mpc, with a one-sample KS p-value of 0.00073 in the innermost bin; and (ii) radio jets are generally perpendicular to the host galaxy major axis, but this preference weakens within D_fil < ~8 Mpc, based on an |epsilon_opt| > 0.1 subset of the extended-jet sample. The results are interpreted as evidence for filament-directed merger-driven growth and chaotic accretion onto supermassive black holes near filaments.

Significance. If both claims hold, the paper provides a direct observational link between cosmic-web environment, galaxy shapes, and AGN jet orientations, with implications for intrinsic alignments, large-scale jet alignment searches, and anisotropic CGM/feedback models. The galaxy-filament alignment is the more secure result: it is supported by strong p-values, bootstrap skewness errors, and explicit projection-effect checks, and it builds on prior observational and simulation work. The jet-randomization claim is more novel but is the least secure pillar of the paper. The analysis uses appropriate statistical machinery (parallel transport, KS tests, bootstrap resampling), real survey data, and includes explicit checks of contributing systematics; however, no analysis code is provided, and the Section 2.4 assertion about selection independence is untested.

major comments (3)
  1. [Section 2.4] The assertion that requiring a spectroscopic redshift "does not affect the results that will follow" is presented without a supporting test. If the completeness of spectroscopic redshifts in the LoTSS cross-match catalogue varies with distance to the nearest SDSS filament (e.g., because dense regions have more SDSS spectroscopy) or with galaxy/radio orientation, the D_fil distributions of the GMRG and EJ samples would be biased, and both the galaxy-filament and jet-galaxy-filament signals could be generated or suppressed. Please add a quantitative comparison of the photometric/spec-z samples or an explicit robustness test, and weaken the claim if no test is possible.
  2. [Section 3.2, Fig. 9] The central new claim that jets become more randomly oriented relative to their host galaxies within ~8 Mpc of filaments rests on a post-hoc analysis chain. After Fig. 8 shows a strong dependence of the jet-galaxy angle on |epsilon_opt|, the sample is cut at |epsilon_opt| > 0.1 and split at D_fil = 7.98 Mpc, with a two-sample KS p = 0.036 and a misaligned-fraction difference (60.2% vs 56.2%) whose 1-sigma errors overlap. No correction is made for the multiple D_fil bins or for the data-driven threshold selection. In addition, the paper does not display the |epsilon_opt| distribution as a function of D_fil; since Fig. 8 establishes that the jet-galaxy angle depends strongly on |epsilon_opt|, a D_fil-dependent ellipticity within the >0.1 subsample could by itself produce the apparent randomization. Please provide (i) the |epsilon_opt| versus D_fil distribution, (ii) a continuous analysis using the full EJ sample without post-hoc cuts, or a pre-specified split at a physically motivated scale, and (iii) a multiple-comparison adjustment or an explicit statement of the number of splits examined.
  3. [Abstract / Summary] The abstract's phrasing "radio jets ... show more randomised orientations with respect to host galaxies within ≲ 8 Mpc of filaments" is stronger than the evidence in Fig. 9 supports. The one-sample KS tests in all D_fil bins reject uniformity, the two-sample KS p is 0.036, and the effect is only present in an ellipticity-selected subset. The conclusion should be tempered or the statistics strengthened before publication.
minor comments (6)
  1. [Abstract] There is a typo in the abstract: "activegalactic nuclei" should be "active galactic nuclei".
  2. [Section 2.3, Eq. (7)] The definition of PA_fil uses a two-argument arctangent without specifying the quadrant convention; please clarify how the angle is wrapped to [0,180) degrees.
  3. [Section 2.4] The EJ sample criteria mention the 'E_PA' column for S_Code='M' sources, but this column is not defined in the text; a brief definition would help reproducibility.
  4. [References] The reference for Springel et al. (2005) lists the journal as "Nature Astrophysics" rather than "Nature"; please correct.
  5. [Section 3.1.1, Fig. 5] The statement that parallel transport alters position angles by ~3 degrees on average is useful, but Fig. 5 shows individual corrections exceeding 10 degrees; please clarify whether the mean is the relevant quantity for the reported alignment signal.
  6. [Data Availability] No analysis code is provided; for reproducibility, please link the scripts used for the KS tests, bootstrap skewness, and sample construction.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the alignment measurements are observational statistics over external catalogs, with no fitted parameter or self-citation chain forcing the reported results.

full rationale

This paper measures angular distributions between optical galaxy major axes, radio jet position angles, and cosmic filament orientations using external data products (LoTSS DR2 cross-match, DESI Legacy, and the Malavasi et al. 2020 SDSS filament catalogue). There is no parameter fitted to the data that is later renamed as a prediction, and no equation in the paper defines the reported alignment in terms of itself. The filament catalogue is constructed from SDSS galaxies, some of which may overlap with the radio-host sample, but that is standard practice; the measured angle between a galaxy major axis and the nearest filament orientation is not fixed by construction, because the filament orientation is a large-scale property of the galaxy density field, not a function of the individual galaxy's position angle. The jet-randomization result relies on a post-hoc ellipticity cut and a modest KS p-value, but statistical fragility or possible selection effects are concerns about validity, not circularity. The paper does not invoke any load-bearing self-citation or uniqueness theorem to force its conclusions. The derivation chain is therefore self-contained with respect to circularity, and the appropriate score is 0.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The analysis is empirical and built entirely on public survey data and published catalogs. The paper introduces no new entities. The central results depend on a set of sample-selection thresholds (ellipticity cut, Dfil cut, misalignment angle) and on unverified assumptions about the fidelity of the filament catalog, the position-angle measurements, and the independence of spectroscopic redshift selection. Of these, the redshift-selection independence is the most load-bearing because it directly affects the distance-to-filament distribution that defines the alignment signals.

free parameters (3)
  • Optical ellipticity threshold for the jet subsample = |epsilon_opt| > 0.1
    Applied in Section 3.2 to define the subsample used for the jet-filament distance analysis; the randomization signal is measured only for this hand-chosen subset.
  • Maximum distance to filament for sample inclusion = Dfil < 80 Mpc
    Used in both GMRG and EJ analyses to exclude galaxies far from cataloged filaments; all reported alignment results are within this range and could depend on the cutoff.
  • Misaligned jet angle threshold = 30 degrees from minor axis
    Used in Section 3.2 to compute the misaligned fraction (60.2% vs 56.2%); this arbitrary cutoff affects the quoted numbers, though not the KS test conclusions.
assumptions (5)
  • domain assumption Planck 2016 LCDM cosmology is assumed (Omega_m=0.309, Omega_Lambda=0.691, Omega_b=0.0486, H0=67.8 km/s/Mpc, sigma8=0.82)
    Used to convert redshifts to distances and radio luminosities; standard in the field.
  • domain assumption DESI Legacy optical ellipticities trace the true stellar major axis of the host galaxies
    All galaxy-filament and jet-galaxy angle measurements rely on this; the catalog applies model-based photometry (EXP/DEV/COMP) and the paper cuts on PA error < 1 deg, but systematic shape measurement biases could remain.
  • domain assumption The radio source position angle (pybdsf DC_PA or composite convex hull PA) traces the AGN jet axis
    Extended radio sources are assumed to be jets; this is standard but can be confused by projection and source morphology.
  • domain assumption The Malavasi et al. (2020) DisPerSE filament catalog, with 1 density smoothing cycle, 3-sigma persistence threshold, and 1 skeleton smoothing cycle, reliably represents the cosmic web at z < 0.6
    The environment measurement (Dfil and filament orientation) is entirely based on this catalog; its sampling-point spacing (~14 Mpc) sets the effective resolution and could smooth out true filament proximity.
  • domain assumption Spectroscopic redshift availability is independent of filament environment and of galaxy or jet orientation
    Stated in Section 2.4 without demonstration; if spectroscopic coverage correlates with density, the sample's Dfil distribution is biased and the central alignment results could be affected.

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Cite this review

Pith. "Pith review of On the relationship between the cosmic web and the alignment of galaxies and AGN jets." pith.science (2026). https://pith.science/paper/NZF22TQE

@misc{pith2026250203730,
  author       = {Pith},
  title        = {Pith review of: On the relationship between the cosmic web and the alignment of galaxies and AGN jets},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NZF22TQE}},
  note         = {Machine review of arXiv:2502.03730}
}
abstract

The impact of active galactic nuclei (AGN) on the evolution of galaxies explains the steep decrease in the number density of the most massive galaxies in the Universe. However, the fueling of the AGN and the efficiency of this feedback largely depend on their environment. We use data from the Low Frequency Array (LOFAR) Two-metre Sky Survey Data Release 2 (LoTSS DR2), the Dark Energy Spectroscopic Instrument (DESI) Legacy Imaging Surveys, and the Sloan Digital Sky Survey (SDSS) DR12 to make the first study of the orientations of radio jets and their optical counterpart in relation to the cosmic web environment. We find that close to filaments ($\lesssim 11 \,\rm Mpc$), galaxies tend to have their optical major axes aligned with the nearest filaments. On the other hand, radio jets, which are generally aligned perpendicularly to the optical major axis of the host galaxy, show more randomised orientations with respect to host galaxies within $\lesssim 8 \,\rm Mpc$ of filaments. These results support the scenario that massive galaxies in cosmic filaments grow by numerous mergers directed along the orientation of the filaments while experiencing chaotic accretion of gas onto the central black hole. The AGN-driven jets consequently have a strong impact preferentially along the minor axes of dark matter halos within filaments. We discuss the implications of these results for large-scale radio jet alignments, intrinsic alignments between galaxies, and the azimuthal anisotropy of the distribution of circumgalactic medium and anisotropic quenching.

Figures

Figures reproduced from arXiv: 2502.03730 by the authors.

Figure 1
Figure 1. Top panel: The sky coverage of different data used in this study. The grey lines are cosmic filaments below redshift 0.6 catalogued by Malavasi et al. (2020). The peach colour shade shows the RA-13 field of LoTSS DR2. The general massive radio galaxy (GMRG) and the extended jet (EJ) samples defined in Section 2.4 are shown with the blue and the green dots, respectively. Bottom panels: we randomly select a galaxy in … view at source ↗
Figure 2
Figure 2. An illustration showing the Cartesian coordinate (uˆ x, uˆ y, uˆ z ) and the local spherical coordinate (uˆr , uˆ 𝜃 , uˆ 𝜙 ) on the celestial sphere. The point 𝐴 and the vector vfil represent the location of a filament sampling point and the filament orientation vector, respectively. We measure the inclination and the position angle of the filament at point 𝐴 by transforming vfil from the Cartesian coordinate to the… view at source ↗
Figure 3
Figure 3. Histograms showing the stellar mass distribution (top panel) and the angular/physical distance from the closest filament distribution (mid￾dle/bottom panel) of the GMRG (blue dashed) and EJ (green) samples. Note that the EJ sample is a subset of the GMRG sample. 3.1.1 Parallel transport method As shown in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (6 more)
Figure 4
Figure 4. Figure 4: An illustration of parallel transport method. In this illustration, there are two blue-coloured great circles connecting the North celestial pole (𝑁) and the points 𝐴 and 𝐵, respectively. Angles 𝑃𝐴A and 𝑃𝐴B are the position angles of the two black bars at each point, m…
Figure 5
Figure 5. Figure 5: shows the absolute degree of parallel transport, i.e., |𝜉A − 𝜉B|, we apply when comparing the optical position angles of the GMRG sample (blue markers) to the position angle of the closest filament. The black line is the mean profile of the distribution. On average, pa…
Figure 6
Figure 6. Figure 6: The distribution of the angle between the galaxy optical major axis and the closest filament orientation as a function of the distance to the filament. The GMRG sample is used for this analysis. Top panel: the histogram between [0, 90] ◦ . The blue line represents the …
Figure 7
Figure 7. Figure 7: The skewness of the galaxy-filament angle distribution in different 𝐷fil bins. In both panels, the blue line shows the skewness calculated using all galaxies in the GMRG sample, i.e., the result shown in the bottom left panel of [PITH_FULL_IMAGE:figures/full_fig_p009_7.png]
Figure 8
Figure 8. Figure 8: The distribution of the angle between the galaxy optical major axis and the radio jet orientation as a function of the optical ellipticity. The EJ sample is used for this analysis. The panels are in the same format as [PITH_FULL_IMAGE:figures/full_fig_p010_8.png]
Figure 9
Figure 9. Figure 9: The distribution of the angle between the galaxy optical major axis and the radio jet orientation as a function of the distance to the filament. The EJ sample is used for this analysis. The panels are in the same format as [PITH_FULL_IMAGE:figures/full_fig_p011_9.png]

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Pith tools

Reviewed August 9, 2026 · model on record in the stance chip above.