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The 61 pages that link to Dark matter halo, each with the reason it gives.

• Dark matterRelated: Its detailed density profile and small-scale structure remain under investigation.

• Galaxy mergerRelated: Merging halos bring galaxies together and influence their orbits before the visible systems combine.

• Dynamical frictionRelated: A satellite moving through a halo experiences friction from the gravitational response of its dark matter.

• Cosmic webRelated: Halos host galaxies and gather along the web’s dense regions.

• Andromeda GalaxyRelated: Andromeda’s halo governs satellite orbits and extends far beyond its visible disk.

• Local GroupRelated: The group’s gravitational mass is dominated by the dark matter halos around its largest galaxies.

• Galaxy evolutionRelated: Halo growth provides the evolving gravitational framework in which galaxies form.

• Galaxy rotation curveRelated: A halo’s gravity can sustain high orbital speeds at large radii.

• ReionizationRelated: The halos hosting early galaxies set where ionizing sources formed and how they clustered.

• Virgo ClusterRelated: The cluster’s dark matter halo supplies most of its gravitational mass.

• Tidal strippingRelated: Satellite disruption and its debris constrain the shape and mass of the host halo.

• Galaxy groupRelated: Its gravity supplies most of the mass binding a group.

• Galaxy interactionRelated: Halo gravity influences encounter orbits and helps bind galaxies before their visible parts collide.

• Dwarf galaxyRelated: Its gravity can dominate a dwarf galaxy’s mass despite the galaxy’s few visible stars.

• Sagittarius Dwarf Spheroidal GalaxyRelated: The shape of Sagittarius’s debris reflects the Milky Way’s unseen halo potential.

• Tidal tailRelated: Tail shapes and motions respond to the gravitational potential of the halo.

• Irregular galaxyRelated: The halo shapes the gravitational environment in which an irregular galaxy evolves.

• Magellanic CloudsRelated: The Milky Way’s halo affects the Clouds’ trajectories and tidal disruption.

• Galaxy filamentRelated: Filaments connect halos and feed them with matter.

• Galactic tideRelated: The halo’s mass profile determines much of the galactic tide experienced by orbiting systems.

• Gravitationally bound systemRelated: Its gravity helps hold galaxies and clusters together beyond the mass of visible matter.

• Tidal dwarf galaxyRelated: Tidal dwarfs are expected to contain little of the dark matter that dominates typical dwarf halos.

• Triangulum GalaxyRelated: M33’s gravity and rotation indicate mass beyond its visible stars and gas.

• Vera RubinRelated: A massive halo offers an explanation for the persistent outer speeds Rubin’s team measured.

• Flocculent spiral galaxyRelated: Its gravitational potential affects disk stability and the evolution of spiral structure.

• Fornax ClusterRelated: The cluster’s unseen halo supplies most of its gravitating mass.

• Magellanic BridgeRelated: Its mass shapes the Clouds’ orbits and therefore models of the Bridge’s origin.

• Sombrero GalaxyRelated: The galaxy’s outer motions and halo studies connect its visible structure to unseen mass.

• Abell 1689Related: Most of the cluster’s inferred lensing mass resides in its dark matter halo.

• Brightest cluster galaxyRelated: The galaxy occupies the dense central region of the cluster’s much larger halo.

• H I regionRelated: Outer H I rotation measurements help constrain the Milky Way's halo mass.

• Hoag's ObjectRelated: Its mass distribution may affect the dynamics and long-term stability of the ring.

• Low surface brightness galaxyRelated: Its mass can dominate even when the galaxy's visible stellar component is faint.

• IC 1101Related: The halo’s extent is distinct from the visible size often attributed to IC 1101.

• Andromeda–Milky Way collisionRelated: The galaxies’ overlapping halos exert gravity before their visible stars approach.

• Centaurus A/M83 GroupRelated: Invisible mass helps explain how galaxies remain bound within groups.

• Field galaxyRelated: Halo mass and history can affect field galaxies independently of cluster membership.

• Intergalactic starRelated: The cluster's halo governs the motions and distribution of many intergalactic stars.

• Jeans equationsRelated: Stellar velocity data analyzed with Jeans equations can constrain its mass profile.

• Messier 49Related: The motions of stars and globular clusters help constrain Messier 49’s halo.

• Unbarred spiral galaxyRelated: Its gravitational influence affects disk rotation and the growth of structure.

• Galaxy groups and clustersRelated: Most of a cluster’s mass lies in its extended dark matter halo.

• IC 342/Maffei GroupRelated: The group’s halo mass and extent are difficult to establish from its obscured galaxy census.

• Satellite galaxies of the Milky WayRelated: The Milky Way's halo supplies much of the gravity binding its satellites.