pith. machine review for the scientific record. sign in

arxiv: 2605.05972 · v1 · submitted 2026-05-07 · 🌌 astro-ph.GA

Recognition: unknown

A statistical look on kinematic planes of satellite galaxies II: The physics behind their early formation in TNG50 MW/M31-like galaxies

Alexander Knebe, Diego Sotillo-Ramos, Isabel Santos-Santos, Mat\'ias G\'amez-Mar\'in, Rosa Dom\'inguez-Tenreiro

Pith reviewed 2026-05-08 07:48 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords kinematically persistent planessatellite galaxiescosmic webLagrangian volumesTNG50 simulationMilky Way analogsanisotropic collapsegalaxy formation
0
0 comments X

The pith

Early kinematically persistent planes of satellite galaxies are fossil remnants of high-redshift anisotropic collapse driven by the local Cosmic Web.

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

This paper traces the origin of kinematically persistent planes of satellites around 190 Milky Way and M31-like hosts in the TNG50 simulation. By following the deformation of Lagrangian Volumes around each system with a reduced tensor-of-inertia analysis, it finds that satellite orbital poles align preferentially with the direction of strongest collapse. Vertical and radial motions decay early, producing rotation-supported configurations. The timescales for plane settling, orbital-pole clustering, and volume-shape evolution all peak near a universe age of 4 Gyr during rapid host-halo growth. The results indicate that these planes preserve the imprint of anisotropic mass collapse set by the forming local Cosmic Web in Lambda-CDM.

Core claim

In the TNG50 sample, roughly 67 percent of early KPPs show satellite orbital poles aligned with the Lagrangian Volume's strongest-collapse axis e3 and about 20 percent with the intermediate axis e2. Kinematic analysis shows that motions perpendicular to these planes decay early, leaving rotation-dominated disks. The characteristic timescales for satellites to settle onto a common orbital plane, for orbital-pole clustering, and for LV shape evolution are quasi-coeval and peak at T_uni approximately 4 Gyr during the fast mass-assembly phase of the host halo.

What carries the argument

Lagrangian Volumes surrounding each host-satellite system, whose principal collapse directions are tracked via reduced tensor-of-inertia analysis and compared to the clustering of satellite orbital poles.

If this is right

  • Satellite orbital poles should remain aligned with the local Cosmic Web's collapse directions long after the initial formation epoch.
  • Early KPPs are expected to appear as thin, rotation-supported structures once vertical and radial velocities have decayed.
  • The same alignment and timescale patterns should appear in other Lambda-CDM simulations that resolve comparable host-satellite systems.
  • The planes form during the rapid mass-assembly phase and then persist as fossil features.

Where Pith is reading between the lines

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

  • Satellite-plane orientations observed around other galaxies today may serve as tracers of the early Cosmic Web geometry in their surroundings.
  • If the same alignment mechanism operates at higher resolution, it would tie small-scale satellite kinematics directly to large-scale structure formation.
  • This early imprint could help explain why some observed satellite planes remain coherent despite later mergers and accretion.

Load-bearing premise

The TNG50 simulation together with the chosen sample of 190 systems and the specific definition of early KPPs faithfully reproduces the relevant physics without numerical resolution effects or selection biases that could artificially generate the reported alignments and timescales.

What would settle it

Absence of the reported alignments between satellite orbital poles and Lagrangian Volume principal axes in either Local Group observations or in independent higher-resolution simulations.

Figures

Figures reproduced from arXiv: 2605.05972 by Alexander Knebe, Diego Sotillo-Ramos, Isabel Santos-Santos, Mat\'ias G\'amez-Mar\'in, Rosa Dom\'inguez-Tenreiro.

Figure 1
Figure 1. Figure 1: Upper Panels: Median values and percentiles for the satellite kinetic energy fractions in a cylindrical coordinate system for KPP satellites in two examples of KPP-HS systems. Blue, red and green curves stand for 𝜅rot, 𝜅rad and 𝜅𝑧 , respectively (see Sec. 4.1 for their definitions). The coordinate system is centred at the centre of mass and velocity of the host galaxy, with its 𝑍 axis aligned with the corr… view at source ↗
Figure 2
Figure 2. Figure 2: Left and middle panels: comoving distance curves to the 𝐽® stack-plane (𝑑Js(𝑡)) for satellites in two KPP-HS systems. Purple curves and shaded regions stand for the median and interquartile ranges of the individual distance values, 𝑑𝑖,Js, of KPP satellites at each timestep. Red curves and shades represent the same values for the non-KPP satellite sets. Blue, magenta and red dashed vertical lines mark the 𝑇… view at source ↗
Figure 3
Figure 3. Figure 3: Projections of the LV around the ID # 411449 KPP-HS, from 𝑧high (Tuni = 0.18 Gyr) onward. Two LV projections along fixed axes are shown for each snapshot, one along the 𝑒®3 (𝑧 = 0) principal direction onto the 𝑋𝑌 plane (first column), and the second one along the 𝑒®2 (𝑧 = 0) principal direction onto the 𝑋𝑍 plane (second column). The snapshot redshift 𝑧 and Universe age Tuni are given at the top left corner… view at source ↗
Figure 5
Figure 5. Figure 5: and panels (c) in Fig. A.2 show the a(t), b(t), and c(t) functions and their corresponding first and second time derivatives for the LVs associated with 33 KPP-HS systems. A general trend can be observed: during the early Gyrs of cosmic evolution, the slopes (i.e. the time derivatives) of 𝑎(𝑡), 𝑏(𝑡) and 𝑐(𝑡) remain relatively constant for many analyzed LVs. While the major axis 𝑎(𝑡) ex￾hibits rapid growth … view at source ↗
Figure 6
Figure 6. Figure 6: These changes in the 𝑐(𝑡)/𝑎(𝑡) and 𝑏(𝑡)/𝑎(𝑡) time derivatives are associated to the end of the rapidly decreasing (stretching) phase of the 𝑐(𝑡) (𝑎(𝑡)) axes leading to a more flattened structure nearly normal to the 𝑒®3 principal direction. This is one key ingredient for the establishment of satellite pole clustering, as we will see in the next sections for the P24 sample, see also Paper IV. The bottom panel of view at source ↗
Figure 7
Figure 7. Figure 7: Time evolution of the angles between the 𝐽® orb of satellites with respect to the principal directions of the LVs, 𝑒®𝑖 (𝑡), 𝑖 = 1, 2, 3, for one KPP-HS system. The cos(𝐽® orb, 𝑒®𝑖 (𝑡)) are shown for satellites belonging to KPPs, and outside these structures as well, see legends. Thin lines correspond to individual satellites, with subhalo IDs, colours and line-types as encoded on the right of the panels. T… view at source ↗
Figure 8
Figure 8. Figure 8: Projections along the 𝑒®3 (𝑡) (left panels) and 𝑒®2 (𝑡) (right panels) of the density field around the host galaxy formation site for 4 KPP-HS systems (with ID#s indicated in the bottom left corner in their left panels) for two different values of the Universe age given in the top left corner in each panel. KPP satellites are marked as red circles in each panel, at the location of their most gravitationall… view at source ↗
Figure 9
Figure 9. Figure 9: Alignment signals between the co-orbitation axis 𝐽® stack and the LV principal directions at each time, 𝑒®𝑖 (𝑡), for a KPP-HS system. Colour codes refer to the alignment signal with the 𝑒®3 (𝑡) (purple), 𝑒®2 (𝑡) (orange) and the 𝑒®1 (𝑡) (blue) principal directions. counterparts. Shaded bands indicate the interquartile ranges view at source ↗
Figure 10
Figure 10. Figure 10: Left and middle panels: comoving distance of satellites to the 𝑒®3-plane as a function of time. Purple curves and shaded regions stand for the median and interquartile ranges of the individual distance values of KPP satellites at each timestep. Red curves and shades represent the same values for the non-KPP satellite sets. As in view at source ↗
Figure 11
Figure 11. Figure 11: Median values 𝐴𝑖 of the normalized projections of KPP satellite velocity vectors onto the three principal directions 𝑒®𝑖 (𝑡). See legend for the representative colour codes. Shaded areas stand for the interquartile ranges. Black continuous lines and shades stand for the cos( ®𝑣𝑗 , 𝐽® stack ) median values and interquartile ranges. Blue and red dashed lines mark the 𝑇 0.5 Krot and 𝑇dJs timescales, respecti… view at source ↗
Figure 12
Figure 12. Figure 12: Cumulative distribution functions of the different timescales analyzed in this work. Black lines show the total distributions, and green and purple thin lines show results separating KPP-HS systems into different populations as decribed in Sec. 8. The median and interquartile ranges for each of the analyzed distributions are given in the lower right corner of each plot, as well as visually depicted as thi… view at source ↗
Figure 13
Figure 13. Figure 13: Representation of the distributions of the different timescales an￾alyzed in this paper. Median values and interquartile ranges are represented by filled points with horizontal error bars. For each timescale, three distribu￾tions are drawn, corresponding to the three KPP-HS populations considered in Sec. 8 as indicated by their colour. An important point to dilucidate is how well the results on the distri… view at source ↗
Figure 14
Figure 14. Figure 14: Examples of the alignment signal between the 𝐽® stack axial vector and the principal direction of the LV with which it aligns for 6 KPP-HS sys￾tems. Continuous (dashed) lines represent the alignment with the principal directions of the LVs defined assuming a scale of 𝐾 = 15 (𝐾 = 10). Colour codes stand for the LV principal direction around which the KPP satellite poles cluster. The KPP-HS ID# is shown on … view at source ↗
read the original abstract

We investigate the physical origin of kinematically persistent planes (KPPs) of satellite galaxies in a sample of 190 Milky Way (MW)/M31-like host-satellite systems drawn from the TNG50 simulation. Building on the identification of 46 early KPPs in a previous work, we analyse their formation in the context of the high-redshift evolution of the local Cosmic Web by tracking the deformation of the so-called Lagrangian Volumes (LVs) surrounding each system. Using a reduced tensor-of-inertia analysis, we characterise the time evolution of the principal directions of collapse and relate them to the clustering of satellite orbital poles. We find that in approximately 67\% of KPPs satellite orbital poles align with the LV direction of strongest collapse, $\vec{e}_3$, while a smaller fraction ($\sim20\%$) align with the intermediate axis, $\vec{e}_2$; alignments with the major axis are rare. These alignments are statistically distinct from random expectations and reflect the confinement of satellites to planar configurations normal to the corresponding LV principal directions. We perform a kinematic analysis of satellite motion within KPPs, finding that vertical and radial motions relative to these KPPs decay early, leading to rotation-dominated, ``disky'' configurations. The characteristic timescales for satellites to settle onto a common orbital plane, for satellite orbital pole clustering, and for LV shape evolution are found to be quasi-coeval, peaking at a Universe age T$_{\rm uni}\sim4$~Gyr, during the fast mass assembly phase of the host halo. These results support a scenario in which early KPPs are fossil remnants of high-redshift, anisotropic mass collapse driven by the local Cosmic Web formation process in $\Lambda$CDM.

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 a statistical analysis of the formation of early kinematically persistent planes (KPPs) in 190 Milky Way/M31-like galaxy systems from the TNG50 cosmological simulation. By tracking Lagrangian volumes (LVs) and using reduced tensor-of-inertia to identify principal collapse directions, the authors find that satellite orbital poles align preferentially with the strongest collapse axis e3 in 67% of cases and with e2 in 20%, significantly above random. Kinematic decomposition shows early decay of vertical and radial velocities, resulting in rotation-supported planes. The timescales for plane formation, pole clustering, and LV evolution are shown to be quasi-coeval, peaking around a universe age of 4 Gyr during the host's rapid assembly phase. The authors conclude that these KPPs are fossil records of anisotropic collapse influenced by the high-redshift Cosmic Web in the ΛCDM model.

Significance. This work is significant as it provides a physical mechanism for the origin of satellite planes in simulated galaxies, connecting them to the large-scale structure formation. The direct use of Lagrangian volume tracking and the statistical distinction from random alignments offer a concrete, simulation-grounded explanation that can be tested against observations. The quasi-coeval timescales add a temporal dimension that strengthens the fossil remnant interpretation. If robust, these findings contribute to resolving the 'planes of satellites' problem within standard cosmology without invoking new physics.

major comments (2)
  1. [§3.2] §3.2 (KPP sample and LV analysis): The central statistical claims (67% alignment with e3, ~20% with e2, distinct from random) rest on the subsample of 46 early KPPs identified in prior work; this manuscript must explicitly restate the KPP selection criteria, include error bars or bootstrap uncertainties on the alignment fractions, and test robustness to reasonable variations in host/satellite cuts, as these directly support the non-random and Cosmic Web interpretation.
  2. [§4.3] §4.3 (timescale evolution): The claim that plane settling, pole clustering, and LV deformation are quasi-coeval with peaks at T_uni ~4 Gyr is load-bearing for the fossil-remnant scenario, yet the text does not specify the peak-finding procedure (binning, smoothing, or derivative method), report uncertainties, or show that the result persists under alternative time binning or subsample choices.
minor comments (2)
  1. [Abstract] Abstract: The phrase 'statistically distinct from random expectations' should be accompanied by the exact random alignment fraction and a quantitative significance measure for immediate clarity.
  2. [Figure captions] Figure captions: Captions for alignment and time-evolution figures should explicitly define all symbols (e.g., e1, e2, e3 directions, vertical vs. radial velocity components) without requiring reference to the main text.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their positive assessment of our work and for the constructive major comments. We agree with the need to enhance the clarity and robustness of our statistical claims and timescale analysis. Below we address each point and outline the revisions we will make to the manuscript.

read point-by-point responses

  1. Referee: [§3.2] §3.2 (KPP sample and LV analysis): The central statistical claims (67% alignment with e3, ~20% with e2, distinct from random) rest on the subsample of 46 early KPPs identified in prior work; this manuscript must explicitly restate the KPP selection criteria, include error bars or bootstrap uncertainties on the alignment fractions, and test robustness to reasonable variations in host/satellite cuts, as these directly support the non-random and Cosmic Web interpretation.

    Authors: We fully agree that the KPP selection criteria from our prior work should be restated explicitly in this manuscript for the benefit of readers. In the revised version, we will add a concise summary of the KPP identification procedure (based on kinematic persistence over time) at the beginning of §3.2. Furthermore, we will calculate bootstrap uncertainties by resampling the 46 KPP systems and report 1σ errors on the alignment fractions. To address robustness, we will perform additional tests by varying the satellite number threshold (e.g., N_sat > 8 instead of >10) and host halo mass range, and include a new supplementary figure showing that the preference for alignment with e3 remains statistically significant across these variations. These additions will strengthen the support for the non-random alignment and its connection to the Cosmic Web. revision: yes

  2. Referee: [§4.3] §4.3 (timescale evolution): The claim that plane settling, pole clustering, and LV deformation are quasi-coeval with peaks at T_uni ~4 Gyr is load-bearing for the fossil-remnant scenario, yet the text does not specify the peak-finding procedure (binning, smoothing, or derivative method), report uncertainties, or show that the result persists under alternative time binning or subsample choices.

    Authors: We acknowledge that the description of how the peaks at T_uni ~4 Gyr were determined is insufficiently detailed. In the revision, we will explicitly state that the distributions were binned in 0.5 Gyr intervals and smoothed with a Gaussian kernel of width 1 Gyr, with peaks identified as the mode of the smoothed histogram. We will also report uncertainties on the peak positions using bootstrap resampling of the KPP sample. Additionally, we will demonstrate the robustness by presenting results for alternative bin widths (0.25 Gyr and 1 Gyr) and for subsamples split by host mass or environment, confirming that the quasi-coeval peaking around 4 Gyr persists in all cases. This will be added to §4.3 and supported by an updated figure. revision: yes

Circularity Check

0 steps flagged

Minor self-citation to prior KPP identification; central analysis independent

full rationale

The paper's load-bearing steps consist of direct measurements on TNG50 outputs: Lagrangian volume tracking, reduced tensor-of-inertia decomposition yielding principal axes e1/e2/e3, orbital-pole alignment statistics (67% with e3), and kinematic decay timescales for vertical/radial motions, all compared against random expectations. These quantities are computed from the simulation data without fitting parameters that are then re-used as predictions. The only self-citation is to the earlier identification of the 46 early KPPs, which functions solely as sample selection and does not supply the physical interpretation or the reported alignments/timescales. No self-definitional equations, fitted-input predictions, ansatzes imported via citation, or renaming of known results occur in the derivation chain.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on the fidelity of the TNG50 hydrodynamical simulation and the appropriateness of Lagrangian-volume plus tensor-of-inertia methods for characterizing collapse; no new free parameters or invented entities are introduced.

axioms (2)
  • domain assumption The TNG50 simulation accurately reproduces the baryonic and dark-matter physics relevant to satellite orbital dynamics and early halo assembly in a Lambda-CDM universe.
    All reported alignments and timescales are extracted from this specific simulation suite.
  • domain assumption The reduced tensor-of-inertia analysis on Lagrangian volumes correctly identifies the principal directions of anisotropic collapse that influence satellite orbits.
    The alignment statistics and fossil-remnant interpretation depend on this standard technique being applicable without major artifacts.

pith-pipeline@v0.9.0 · 5659 in / 1658 out tokens · 67509 ms · 2026-05-08T07:48:21.670852+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

295 extracted references · 262 canonical work pages · 2 internal anchors

  1. [1]

    doi:10.1093/mnras/stag193 , archiveprefix =

    Cosmic web dynamics: forces and strains. , keywords =. doi:10.1093/mnras/stag193 , archivePrefix =. 2407.16489 , primaryClass =

    work page doi:10.1093/mnras/stag193

  2. [2]

    , keywords =

    How cosmological merger histories shape the diversity of stellar haloes. , keywords =. doi:10.1093/mnras/stab3709 , archivePrefix =. 2106.09729 , primaryClass =

    work page doi:10.1093/mnras/stab3709

  3. [3]

    arXiv e-prints , keywords =

    VINTERGATAN-GM: long-lived satellite planes induced by a massive GSE-like merger. arXiv e-prints , keywords =. doi:10.48550/arXiv.2603.20171 , archivePrefix =. 2603.20171 , primaryClass =

    work page doi:10.48550/arxiv.2603.20171

  4. [4]

    , keywords =

    The imprint of galaxy mergers on satellite planes in a cosmological context. , keywords =. doi:10.1093/mnras/stad1861 , archivePrefix =. 2307.03218 , primaryClass =

    work page doi:10.1093/mnras/stad1861

  5. [5]

    , keywords =

    Mass density structuring around galaxy formation sites: impact on galaxy basic properties. , keywords =. doi:10.1093/mnras/stag147 , archivePrefix =. 2601.13431 , primaryClass =

    work page doi:10.1093/mnras/stag147

  6. [6]

    , keywords =

    High and low S \'e rsic index bulges in Milky Way- and M31-like galaxies: origin and connection to the bar with TNG50. , keywords =. doi:10.1093/mnras/stac629 , archivePrefix =. 2111.13712 , primaryClass =

    work page doi:10.1093/mnras/stac629

  7. [7]

    , keywords =

    The merger and assembly histories of Milky Way- and M31-like galaxies with TNG50: disc survival through mergers. , keywords =. doi:10.1093/mnras/stac2586 , archivePrefix =. 2211.00036 , primaryClass =

    work page doi:10.1093/mnras/stac2586

  8. [8]

    , keywords =

    Modeling multi-stream flow in collisionless matter: approximations for large-scale structure beyond shell-crossing. , keywords =. doi:10.48550/arXiv.astro-ph/9702139 , archivePrefix =. astro-ph/9702139 , primaryClass =

    work page doi:10.48550/arxiv.astro-ph/9702139

  9. [9]

    arXiv e-prints , keywords =

    Analysis of the plane of satellites around Milky Way-like galaxies in Λ CDM cosmology. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.02518 , archivePrefix =. 2510.02518 , primaryClass =

    work page doi:10.48550/arxiv.2510.02518

  10. [10]

    doi:10.1093/mnras/staf1610 , archiveprefix =

    Spinning masters: on the impact of tidal forces and protohalo size on early spin evolution. , keywords =. doi:10.1093/mnras/staf1610 , archivePrefix =. 2505.01298 , primaryClass =

    work page doi:10.1093/mnras/staf1610

  11. [11]

    arXiv e-prints , keywords =

    Planes of satellites, at once transient and persistent. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.01318 , archivePrefix =. 2510.01318 , primaryClass =

    work page doi:10.48550/arxiv.2510.01318

  12. [12]

    arXiv e-prints , keywords =

    A statistical look on kinematic planes of satellite galaxies I: frequency and properties in TNG50 MW/M31-like galaxies. arXiv e-prints , keywords =. doi:10.48550/arXiv.2509.13622 , archivePrefix =. 2509.13622 , primaryClass =

    work page doi:10.48550/arxiv.2509.13622

  13. [13]

    The large-scale structure of the universe

  14. [14]

    Robust Statistics: Theory and Methods , publisher =

  15. [15]

    Sparsity of similarly extreme analogs and a possible role of satellite pairs

    The satellite galaxy plane of NGC 4490 in light of CDM. Sparsity of similarly extreme analogs and a possible role of satellite pairs. , keywords =. doi:10.1051/0004-6361/202449954 , archivePrefix =. 2405.06016 , primaryClass =

    work page doi:10.1051/0004-6361/202449954

  16. [16]

    and Katz, N

    Keres, D. and Katz, N. and Weinberg, D. H. and Davé, R. , title =. , year =

  17. [17]

    1974 , publisher=

    The Nonlinear Diffusion Equation: Asymptotic Solutions and Statistical Problems , author=. 1974 , publisher=

    1974

  18. [18]

    , keywords =

    Structure of the universe in the two-dimensional model of adhesion. , keywords =. doi:10.1093/mnras/242.2.200 , adsurl =

    work page doi:10.1093/mnras/242.2.200

  19. [19]

    , keywords =

    On the environmental dependence of halo formation. , keywords =. doi:10.1111/j.1365-2966.2004.07733.x , archivePrefix =. astro-ph/0402237 , primaryClass =

    work page doi:10.1111/j.1365-2966.2004.07733.x 2004

  20. [20]

    Physics Reports , author =

    Vincent Desjacques and Donghui Jeong and Fabian Schmidt , keywords =. Large-scale galaxy bias , journal =. 2018 , note =. doi:https://doi.org/10.1016/j.physrep.2017.12.002 , url =

    work page doi:10.1016/j.physrep.2017.12.002 2018

  21. [21]

    and Hoffman, Yehuda and Crain, Robert A

    Galaxy properties and the cosmic web in simulations. , keywords =. doi:10.1093/mnras/stu2166 , archivePrefix =. 1405.0281 , primaryClass =

    work page doi:10.1093/mnras/stu2166

  22. [22]

    An excursion set model of the cosmic web: the abundance of sheets, filaments and halos

    An Excursion Set Model of the Cosmic Web: The Abundance of Sheets, Filaments, and Halos. , keywords =. doi:10.1086/504513 , archivePrefix =. astro-ph/0511365 , primaryClass =

    work page doi:10.1086/504513

  23. [23]

    A., Heckman, T

    Simulating the physical properties of dark matter and gas inside the cosmic web. , keywords =. doi:10.1111/j.1365-2966.2006.10511.x , archivePrefix =. astro-ph/0511357 , primaryClass =

    work page doi:10.1111/j.1365-2966.2006.10511.x 2006

  24. [24]

    Nature , author =

    Simulations of the formation, evolution and clustering of galaxies and quasars. , keywords =. doi:10.1038/nature03597 , archivePrefix =. astro-ph/0504097 , primaryClass =

    work page doi:10.1038/nature03597

  25. [25]

    D., Drew, J

    Intercluster filaments in a CDM Universe. , keywords =. doi:10.1111/j.1365-2966.2005.08897.x , archivePrefix =. astro-ph/0406665 , primaryClass =

    work page doi:10.1111/j.1365-2966.2005.08897.x 2005

  26. [26]

    , year = 1998, month = may, volume = 499, pages =

    Evolution of Structure in Cold Dark Matter Universes. , keywords =. doi:10.1086/305615 , archivePrefix =. astro-ph/9709010 , primaryClass =

    work page doi:10.1086/305615

  27. [27]

    , keywords =

    Origin and observables of the cosmic web. , keywords =

  28. [28]

    , keywords =

    A hierarchy of voids: much ado about nothing. , keywords =. doi:10.1111/j.1365-2966.2004.07661.x , archivePrefix =. astro-ph/0311260 , primaryClass =

    work page doi:10.1111/j.1365-2966.2004.07661.x 2004

  29. [29]

    Nature Astronomy , keywords =

    Baryonic solutions and challenges for cosmological models of dwarf galaxies. Nature Astronomy , keywords =. doi:10.1038/s41550-022-01689-w , archivePrefix =. 2206.05295 , primaryClass =

    work page doi:10.1038/s41550-022-01689-w

  30. [30]

    arXiv e-prints , keywords =

    Study of Satellite Plane Structure Characteristics Based on TNG50 Simulations: A Comparative Analysis from Plane to Non-Plane Structures. arXiv e-prints , keywords =. doi:10.48550/arXiv.2412.12474 , archivePrefix =. 2412.12474 , primaryClass =

    work page doi:10.48550/arxiv.2412.12474

  31. [31]

    2024, MNRAS, 535, 3775, doi: 10.1093/mnras/stae2632

    New tools for studying planarity in galaxy satellite systems: Milky Way satellite planes are consistent with CDM. , keywords =. doi:10.1093/mnras/stae2632 , archivePrefix =. 2411.17813 , primaryClass =

    work page doi:10.1093/mnras/stae2632

  32. [32]

    , keywords =

    A New Rarity Assessment of the ``Disk of Satellites'': The Milky Way System Is the Exception Rather Than the Rule in the CDM Cosmology. , keywords =. doi:10.3847/1538-4357/ad8634 , archivePrefix =. 2411.18040 , primaryClass =

    work page doi:10.3847/1538-4357/ad8634

  33. [33]

    arXiv e-prints , keywords =

    Subhalos are Distributed Anisotropically About Their Hosts. arXiv e-prints , keywords =. doi:10.48550/arXiv.2406.10150 , archivePrefix =. 2406.10150 , primaryClass =

    work page doi:10.48550/arxiv.2406.10150

  34. [34]

    , keywords =

    Anisotropies in the spatial distribution and kinematics of dwarf galaxies in the Local Group and beyond. , keywords =. doi:10.1093/mnras/stae1616 , archivePrefix =. 2310.02464 , primaryClass =

    work page doi:10.1093/mnras/stae1616

  35. [35]

    arXiv e-prints , keywords =

    Testing a proposed ``planarity'' tool for studying satellite systems: On the alleged consistency of Milky Way satellite galaxy planes with CDM. arXiv e-prints , keywords =. doi:10.48550/arXiv.2412.14330 , archivePrefix =. 2412.14330 , primaryClass =

    work page doi:10.48550/arxiv.2412.14330

  36. [36]

    , keywords =

    A co-rotating gas and satellite structure around the interacting galaxy pair NGC 4490/85. , keywords =. doi:10.1093/mnras/stae184 , archivePrefix =. 2401.09527 , primaryClass =

    work page doi:10.1093/mnras/stae184

  37. [37]

    , archivePrefix = "arXiv", eprint =

    A Two-phase Scenario for Bulge Assembly in CDM Cosmologies. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/763/1/26 , adsurl =

    work page doi:10.1088/0004-637x/763/1/26

  38. [38]

    B., Kawata, D., Gibson, B

    The Emergence of the Thick Disk in a Cold Dark Matter Universe. , eprint =. doi:10.1086/422709 , adsurl =

    work page doi:10.1086/422709

  39. [39]

    2010, ApJ, 725, 2312, doi: 10.1088/0004-637X/725/2/2312

    The Two Phases of Galaxy Formation. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/725/2/2312 , adsurl =

    work page doi:10.1088/0004-637x/725/2/2312

  40. [40]

    L., & Haiman, Z

    Two-phase galaxy formation. , archivePrefix = "arXiv", eprint =. doi:10.1111/j.1365-2966.2009.14962.x , adsurl =

    work page doi:10.1111/j.1365-2966.2009.14962.x 2009

  41. [41]

    , eprint =

    The Lack of Structural and Dynamical Evolution of Elliptical Galaxies since z\ 1.5: Clues from Self-Consistent Hydrodynamic Simulations. , eprint =. doi:10.1086/500044 , adsurl =

    work page doi:10.1086/500044

  42. [42]

    2012, MNRAS, 420, 1825, doi: 10.1111/j.1365-2966.2011.19805.x

    Large-scale gas dynamics in the adhesion model: implications for the two-phase massive galaxy formation scenario. , archivePrefix = "arXiv", eprint =. doi:10.1111/j.1365-2966.2011.18379.x , adsurl =

    work page doi:10.1111/j.1365-2966.2011.18379.x 2011

  43. [43]

    and Libeskind, N

    Identification of basins of attraction in the local Universe. Nature Astronomy , keywords =. doi:10.1038/s41550-024-02370-0 , archivePrefix =. 2409.17261 , primaryClass =

    work page doi:10.1038/s41550-024-02370-0

  44. [44]

    D., Drew, J

    Scale radii and aggregation histories of dark haloes. , eprint =. doi:10.1111/j.1365-2966.2005.08818.x , adsurl =

    work page doi:10.1111/j.1365-2966.2005.08818.x 2005

  45. [45]

    , keywords =

    The Caterpillar Project: A Large Suite of Milky Way Sized Halos. , archivePrefix = "arXiv", eprint =. doi:10.3847/0004-637X/818/1/10 , adsurl =

    work page doi:10.3847/0004-637x/818/1/10

  46. [46]

    The Emergence of the Thick Disk in a CDM Universe. II. Colors and Abundance Patterns. , eprint =. doi:10.1086/431924 , adsurl =

    work page doi:10.1086/431924

  47. [47]

    2003, MNRAS, 339, 937, doi: 10.1046/j.1365-8711.2003.06241.x G¨ otberg, Y., de Mink, S

    The growth and structure of dark matter haloes. , eprint =. doi:10.1046/j.1365-8711.2003.06135.x , adsurl =

    work page doi:10.1046/j.1365-8711.2003.06135.x 2003

  48. [48]

    H., Bullock , J

    Concentrations of Dark Halos from Their Assembly Histories. , eprint =. doi:10.1086/338765 , adsurl =

    work page doi:10.1086/338765

  49. [49]

    An Introduction to Celestial Mechanics

  50. [50]

    Solar System Formation and Evolution , year = 1998, editor =

    Orbital Resonances and Chaos in the Solar System. Solar System Formation and Evolution , year = 1998, editor =

    1998

  51. [51]

    Physica D Nonlinear Phenomena , keywords =

    Nonlinear resonances in the solar system. Physica D Nonlinear Phenomena , keywords =. doi:10.1016/0167-2789(94)90141-4 , archivePrefix =. chao-dyn/9406004 , primaryClass =

    work page doi:10.1016/0167-2789(94)90141-4

  52. [52]

    2016, ARA&A, 54, 441, doi: 10.1146/annurev-astro-081915-023315

    The Eccentric Kozai-Lidov Effect and Its Applications. , keywords =. doi:10.1146/annurev-astro-081915-023315 , archivePrefix =. 1601.07175 , primaryClass =

    work page doi:10.1146/annurev-astro-081915-023315

  53. [53]

    B., Erkal, D., & Li, T

    Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies. , keywords =. doi:10.3847/1538-4357/ac997b , archivePrefix =. 2205.05699 , primaryClass =

    work page doi:10.3847/1538-4357/ac997b

  54. [54]

    Gaia EDR3 Proper Motions of Milky Way Dwarfs. I. 3D Motions and Orbits. , keywords =. doi:10.3847/1538-4357/ac0436 , archivePrefix =. 2104.03974 , primaryClass =

    work page doi:10.3847/1538-4357/ac0436

  55. [55]

    , keywords =

    Gaia early DR3 systemic motions of Local Group dwarf galaxies and orbital properties with a massive Large Magellanic Cloud. , keywords =. doi:10.1051/0004-6361/202141528 , archivePrefix =. 2106.08819 , primaryClass =

    work page doi:10.1051/0004-6361/202141528

  56. [56]

    Planck 2015 results. XIII. Cosmological parameters. , keywords =. doi:10.1051/0004-6361/201525830 , archivePrefix =. 1502.01589 , primaryClass =

    work page doi:10.1051/0004-6361/201525830 2015

  57. [57]

    Summary of the contents and survey properties

    Gaia Early Data Release 3. Summary of the contents and survey properties. , keywords =. doi:10.1051/0004-6361/202039657 , archivePrefix =. 2012.01533 , primaryClass =

    work page doi:10.1051/0004-6361/202039657 2012

  58. [58]

    , keywords =

    A portrait of the vast polar structure as a young phenomenon: Hints from its member satellites. , keywords =. doi:10.1051/0004-6361/202347473 , archivePrefix =. 2310.13521 , primaryClass =

    work page doi:10.1051/0004-6361/202347473

  59. [59]

    2015, MNRAS, 449, 49, doi: 10.1093/mnras/stv264

    The merger rate of galaxies in the Illustris simulation: a comparison with observations and semi-empirical models. , keywords =. doi:10.1093/mnras/stv264 , archivePrefix =. 1502.01339 , primaryClass =

    work page doi:10.1093/mnras/stv264

  60. [60]

    V., Genel, S., et al

    The role of mergers and halo spin in shaping galaxy morphology. , keywords =. doi:10.1093/mnras/stx305 , archivePrefix =. 1609.09498 , primaryClass =

    work page doi:10.1093/mnras/stx305

  61. [61]

    , keywords =

    ERGO-ML I: inferring the assembly histories of IllustrisTNG galaxies from integral observable properties via invertible neural networks. , keywords =. doi:10.1093/mnras/stac3295 , archivePrefix =. 2202.06967 , primaryClass =

    work page doi:10.1093/mnras/stac3295

  62. [62]

    L., & Haiman, Z

    E pur si muove: Galilean-invariant cosmological hydrodynamical simulations on a moving mesh. , keywords =. doi:10.1111/j.1365-2966.2009.15715.x , archivePrefix =. 0901.4107 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15715.x 2009

  63. [63]

    2017, MNRAS, 465, 3291, doi: 10.1093/mnras/stw2944

    Simulating galaxy formation with black hole driven thermal and kinetic feedback. , keywords =. doi:10.1093/mnras/stw2944 , archivePrefix =. 1607.03486 , primaryClass =

    work page Pith review doi:10.1093/mnras/stw2944

  64. [64]

    Weinberger, V

    The AREPO Public Code Release. , keywords =. doi:10.3847/1538-4365/ab908c , archivePrefix =. 1909.04667 , primaryClass =

    work page doi:10.3847/1538-4365/ab908c 1909

  65. [65]

    First results from the IllustrisTNG simulations: the galaxy color bimodality

    First results from the IllustrisTNG simulations: the galaxy colour bimodality. , keywords =. doi:10.1093/mnras/stx3040 , archivePrefix =. 1707.03395 , primaryClass =

    work page internal anchor Pith review doi:10.1093/mnras/stx3040

  66. [66]

    2019, Computational Astrophysics and Cosmology, 6, 2, doi: 10.1186/s40668-019-0028-x

    The IllustrisTNG simulations: public data release. Computational Astrophysics and Cosmology , keywords =. doi:10.1186/s40668-019-0028-x , archivePrefix =. 1812.05609 , primaryClass =

    work page doi:10.1186/s40668-019-0028-x

  67. [67]

    , keywords =

    First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback. , keywords =. doi:10.1093/mnras/stz2306 , archivePrefix =. 1902.05554 , primaryClass =

    work page doi:10.1093/mnras/stz2306 1902

  68. [68]

    , keywords =

    The cold circumgalactic medium in emission: Mg II haloes in TNG50. , keywords =. doi:10.1093/mnras/stab2177 , archivePrefix =. 2106.09023 , primaryClass =

    work page doi:10.1093/mnras/stab2177

  69. [69]

    First results from the IllustrisTNG simulations: radio haloes and magnetic fields

    First results from the IllustrisTNG simulations: radio haloes and magnetic fields. , keywords =. doi:10.1093/mnras/sty2206 , archivePrefix =. 1707.03396 , primaryClass =

    work page Pith review doi:10.1093/mnras/sty2206

  70. [70]

    First results from the IllustrisTNG simulations: A tale of two elements -- chemical evolution of magnesium and europium

    First results from the IllustrisTNG simulations: a tale of two elements - chemical evolution of magnesium and europium. , keywords =. doi:10.1093/mnras/sty618 , archivePrefix =. 1707.03401 , primaryClass =

    work page Pith review doi:10.1093/mnras/sty618

  71. [71]

    2018, MNRAS, 475, 676, doi: 10.1093/mnras/stx3304

    First results from the IllustrisTNG simulations: matter and galaxy clustering. , keywords =. doi:10.1093/mnras/stx3304 , archivePrefix =. 1707.03397 , primaryClass =

    work page doi:10.1093/mnras/stx3304

  72. [72]

    2019, MNRAS, 490, 3196, doi: 10.1093/mnras/stz2338 Planck Collaboration, Ade, P

    First results from the TNG50 simulation: the evolution of stellar and gaseous discs across cosmic time. , keywords =. doi:10.1093/mnras/stz2338 , archivePrefix =. 1902.05553 , primaryClass =

    work page doi:10.1093/mnras/stz2338 1902

  73. [73]

    First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies

    First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies. , keywords =. doi:10.1093/mnras/stx3112 , archivePrefix =. 1707.03406 , primaryClass =

    work page Pith review doi:10.1093/mnras/stx3112

  74. [74]

    2018, MNRAS, 473, 4077, doi: 10.1093/mnras/stx2656 Planck Collaboration, Aghanim, N., Akrami, Y., et al

    Simulating galaxy formation with the IllustrisTNG model. , keywords =. doi:10.1093/mnras/stx2656 , archivePrefix =. 1703.02970 , primaryClass =

    work page Pith review doi:10.1093/mnras/stx2656

  75. [75]

    , keywords =

    The Origin of Kinematically Persistent Planes of Satellites as Driven by the Early Evolution of the Cosmic Web in CDM. , keywords =. doi:10.3847/1538-4357/ad27da , archivePrefix =. 2402.03288 , primaryClass =

    work page doi:10.3847/1538-4357/ad27da

  76. [76]

    , keywords =

    The abundance of satellites around Milky Way- and M31-like galaxies with the TNG50 simulation: a matter of diversity. , keywords =. doi:10.1093/mnras/stab2437 , archivePrefix =. 2101.12215 , primaryClass =

    work page doi:10.1093/mnras/stab2437

  77. [77]

    Milky Way and Andromeda analogues from the TNG50 simulation

    Milky Way and Andromeda analogs from the TNG50 simulation. , keywords =. doi:10.1093/mnras/stae2165 , archivePrefix =. 2303.16217 , primaryClass =

    work page doi:10.1093/mnras/stae2165

  78. [78]

    , year = 1967, month = jan, volume =

    Statistical mechanics of violent relaxation in stellar systems. , year = 1967, month = jan, volume =. doi:10.1093/mnras/136.1.101 , adsurl =

    work page doi:10.1093/mnras/136.1.101 1967

  79. [79]

    , year = 1968, month = jan, volume =

    The gravo-thermal catastrophe in isothermal spheres and the onset of red-giant structure for stellar systems. , year = 1968, month = jan, volume =. doi:10.1093/mnras/138.4.495 , adsurl =

    work page doi:10.1093/mnras/138.4.495 1968

  80. [80]

    doi:10.1093/mnras/sts416 , archiveprefix =

    NEXUS: tracing the cosmic web connection. , keywords =. doi:10.1093/mnras/sts416 , archivePrefix =. 1209.2043 , primaryClass =

    work page doi:10.1093/mnras/sts416 2043

Showing first 80 references.