The Magellanic Clouds are very rare in the IllustrisTNG simulations
arXiv:2409.17259 · doi:10.3390/universe10100385
Abstract
The Large and Small Magellanic Cloud (LMC and SMC) form the closest interacting galactic system to the Milky Way, therewith providing a laboratory to test cosmological models in the local Universe. We quantify the likelihood for the Magellanic Clouds (MCs) to be observed within the CDM model using hydrodynamical simulations of the IllustrisTNG project. The orbits of the MCs are constrained by proper motion measurements taken by the and . The MCs have a mutual separation of and a relative velocity of , implying a phase-space density of . We select analogues to the MCs based on their stellar masses and distances in MW-like halos. None of the selected LMC analogues have a higher total mass and lower Galactocentric distance than the LMC, resulting in tension. We also find that the distribution in the highest resolution TNG50 simulation is in tension with observations. Thus, a hierarchical clustering of two massive satellites like the MCs in a narrow phase-space volume is unlikely in CDM, presumably because of short merger timescales due to dynamical friction between the overlapping dark matter halos. We show that group infall led by an LMC analogue cannot populate the Galactic disc of satellites (DoS), implying that the DoS and the MCs formed in physically unrelated ways in CDM. Since the alignment of the LMC and DoS orbital poles has a likelihood of (), adding this to that of gives a combined likelihood of ().
arXiv comment25 pages, 11 figures, 5 tables. Accepted for publication in Universe in this form
References in corpus (98)
- The Sloan Digital Sky Survey: Technical Summary
- Populating a cluster of galaxies - I. Results at z=0
- Observational evidence for self-interacting cold dark matter
- Simulating Galaxy Formation with the IllustrisTNG Model
- The observed properties of dwarf galaxies in and around the Local Group
- First results from the IllustrisTNG simulations: matter and galaxy clustering
- First results from the IllustrisTNG simulations: the galaxy color bimodality
- Galactic star formation and accretion histories from matching galaxies to dark matter haloes
- Properties of galaxies reproduced by a hydrodynamic simulation
- First results from the IllustrisTNG simulations: A tale of two elements -- chemical evolution of magnesium and europium
- The mass distribution and gravitational potential of the Milky Way
- First results from the IllustrisTNG simulations: radio haloes and magnetic fields
- Substructures in hydrodynamical cluster simulations
- First Results from the TNG50 Simulation: Galactic outflows driven by supernovae and black hole feedback
- Halos and galaxies in the standard cosmological model: results from the Bolshoi simulation
- First Results from the TNG50 Simulation: The evolution of stellar and gaseous disks across cosmic time
- Resolving Cosmic Structure Formation with the Millennium-II Simulation
- Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions
- The merger rate of galaxies in the Illustris Simulation: a comparison with observations and semi-empirical models
- The APOSTLE simulations: solutions to the Local Group's cosmic puzzles
- Are the Magellanic Clouds on their First Passage about the Milky Way?
- The Illustris Simulation: Public Data Release
- Improved Estimates of the Milky Way's Stellar Mass and Star Formation Rate from Hierarchical Bayesian Meta-Analysis
- Third-Epoch Magellanic Cloud Proper Motions I: HST/WFC3 data and Orbit Implications
- The great disk of Milky-Way satellites and cosmological sub-structures
- The VPOS: a vast polar structure of satellite galaxies, globular clusters and streams around the Milky Way
- The Proper Motion of the Large Magellanic Cloud using HST
- Galaxies in LCDM with Halo Abundance Matching: luminosity-velocity relation, baryonic mass-velocity relation, velocity function and clustering
- Tango for three: Sagittarius, LMC, and the Milky Way
- Is the SMC Bound to the LMC? The HST Proper Motion of the SMC
- Theory of Dark Matter Superfluidity
- Mass and shape of the Milky Way's dark matter halo with globular clusters from Gaia and Hubble
- The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection
- Galaxies as simple dynamical systems: observational data disfavor dark matter and stochastic star formation
- The spatial distribution of the Milky Way and Andromeda satellite galaxies
- Small Dwarf Galaxies Within Larger Dwarfs: Why Some Are Luminous While Most Go Dark
- The 200 Degree-Long Magellanic Stream System
- The Magellanic Stream: Circumnavigating the Galaxy
- Co-orbiting satellite galaxy structures are still in conflict with the distribution of primordial dwarf galaxies
- Infall of substructures onto a Milky Way-like dark halo
- From galactic bars to the Hubble tension: weighing up the astrophysical evidence for Milgromian gravity
- Do dwarf galaxies form in tidal tails?
- Local Group Dwarf Spheroidals: Correlated Deviations from the Baryonic Tully-Fisher Relation
- The preferred direction of infalling satellite galaxies in the Local Group
- How Common are the Magellanic Clouds?
- Mismatch and Misalignment: Dark Haloes and Satellites of Disc Galaxies
- Measuring the Mass of the Large Magellanic Cloud with Stellar Streams Observed by
- Statistics of Satellite Galaxies Around Milky Way-Like Hosts
- The Milky Way's Disk of Classical Satellite Galaxies in Light of Gaia DR2
- Comparing the Ancient Star Formation Histories of the Magellanic Clouds
- Andromeda Dwarfs in Light of MOND. II. Testing Prior Predictions
- A thousand shadows of Andromeda: rotating planes of satellites in the Millennium-II cosmological simulation
- The Mass Distribution and Assembly of the Milky Way from the Properties of the Magellanic Clouds
- : Probing the Milky Way and Magellanic Clouds potentials with the 6-D map of the Orphan-Chenab stream
- Dynamical Friction in a Fuzzy Dark Matter Universe
- Dynamics of the Magellanic Clouds in a LCDM Universe
- Did the Milky Way dwarf satellites enter the halo as a group?
- The Link between Galactic Satellite Orbits and Subhalo Accretion
- The Magellanic Stream System: I. Ram-pressure tails and the relics of the collision between the Magellanic Clouds
- Fast galaxy bars continue to challenge standard cosmology
- Andromeda Dwarfs in Light of MOND
- A massive blow for CDM the high redshift, mass, and collision velocity of the interacting galaxy cluster El Gordo contradicts concordance cosmology
- The predicted luminous satellite populations around SMC and LMC-mass galaxies - A missing satellite problem around the LMC?
- Planes of satellites around Milky Way/M31-mass galaxies in the FIRE simulations and comparisons with the Local Group
- MOND simulation suggests the origin of some peculiarities in the Local Group
- The multiplicity and anisotropy of galactic satellite accretion
- The grouping, merging and survival of subhaloes in the simulated Local Group
- Gas depletion in Local Group dwarfs on ~250 kpc scales: Ram pressure stripping assisted by internal heating at early times
- The synchronised dance of the Magellanic Clouds' star formation history
- Phenomenological consequences of superfluid dark matter with baryon-phonon coupling
- Tidal dwarf galaxies in cosmological simulations
- The VMC survey -- XLIII. The spatially resolved star formation history across the Large Magellanic Cloud
- The distribution and morphologies of Fornax Cluster dwarf galaxies suggest they lack dark matter
- The Magellanic Corona and the formation of the Magellanic Stream
- HST Proper Motions of NGC 147 and NGC 185: Orbital Histories and Test of Dynamically Coherent Andromeda Satellite Plane
- Asymmetrical tidal tails of open star clusters: stars crossing their cluster's prah challenge Newtonian gravitation
- Origin of the Local Group satellite planes
- Galaxies lacking dark matter in the Illustris simulation
- Using dwarf satellite proper motions to determine their origin
- Dynamical Friction in Superfluids
- Magellanic satellites in CDM cosmological hydrodynamical simulations of the Local Group
- The Clustering of Orbital Poles Induced by the LMC: Hints for the Origin of Planes of Satellites
- Evolution of LMC/M33-mass dwarf galaxies in the EAGLE simulation
- 3D hydrodynamic simulations for the formation of the Local Group satellite planes
- The High Fraction of Thin Disk Galaxies Continues to Challenge ΛCDM Cosmology
- Dynamical Friction in fuzzy dark matter: circular orbits
- Constraints on the dynamical evolution of the galaxy group M81
- Stellar and dark matter density in the Local Universe
- Barred spiral galaxies in modified gravity theories
- The Escape Velocity Curve of the Milky Way in Modified Newtonian Dynamics
- The Magellanic Edges Survey III. Kinematics of the disturbed LMC outskirts
- On the Effect of the Large Magellanic Cloud on the Orbital Poles of Milky Way Satellite Galaxies
- The Relevance of Dynamical Friction for the MW/LMC/SMC Triple System
- The satellite galaxy plane of NGC 4490 in light of ΛCDM - Sparsity of similarly extreme analogs and a possible role of satellite pairs
- On the absence of backsplash analogues to NGC 3109 in the CDM framework
- Effect of the Large Magellanic Cloud on the kinematics of Milky Way satellites and virial mass estimate
- Dynamical Friction due to fuzzy dark matter on satellites described by axisymmetric logarithmic potentials
- Hermeian haloes: extreme objects with two interactions in the past
Cited by in corpus (6)
- Testing the local void hypothesis using baryon acoustic oscillation measurements over the last twenty years
- Comparing measures of the Hubble and BAO tensions in CDM and possible solutions in gravity
- NGC 3521 as the Milky Way near twin: spectral energy distribution from UV to radio decameter ranges
- NGC3521 as the Milky Way analogue: spectral energy distributon from UV to Radio and photometric variability
- Bulgeless Evolution And the Rise of Discs (BEARD) III. A numerical simulation view of satellites around Milky-Way analogues
- The orbital dynamics of the LMC and SMC about the Milky Way