Galactic halo

A galactic halo is an extended, roughly spherical component of a galaxy which extends beyond the main, visible component.^[1] Several distinct components of a galaxy comprise its halo:^[2][3]

• the stellar halo
• the galactic corona (hot gas, i.e. a plasma)
• the dark matter halo

The distinction between the halo and the main body of the galaxy is clearest in

, there is no sharp transition between the other components of the galaxy and the halo.

A halo can be studied by observing its effect on the passage of light from distant bright objects like quasars that are in line of sight beyond the galaxy in question.^[4]

The stellar halo is a nearly spherical population of field stars and globular clusters. It surrounds most disk galaxies as well as some elliptical galaxies of type cD. A low amount (about one percent) of a galaxy's stellar mass resides in the stellar halo, meaning its luminosity is much lower than other components of the galaxy.

The

Galactic corona

A galactic corona is a distribution of gas extending far away from the center of the galaxy. It can be detected by the distinct emission spectrum it gives off, showing the presence of atomic neutral hydrogen (the H I region, pronounced "H-one") and other features detectable by X-ray spectroscopy.^[7]

The

The Navarro–Frenk–White profile is a widely accepted density profile of the dark matter halo determined through numerical simulations.^[9] It represents the mass density of the dark matter halo as a function of ${\displaystyle r}$, the distance from the galactic center:

$${\displaystyle \rho (r)={\frac {\rho _{\text{crit}}\delta _{c}}{(r/r_{s})(1+r/r_{s})^{2}}}}$$

where ${\displaystyle r_{s}}$ is a characteristic radius for the model, ${\displaystyle \rho _{\text{crit}}=3H^{2}/8\pi G}$ is the critical density (with ${\displaystyle H}$ being the

), and ${\displaystyle \delta _{c}}$ is a dimensionless constant. The invisible halo component cannot extend with this density profile indefinitely, however; this would lead to a diverging integral when calculating mass. It does, however, provide a finite gravitational potential for all ${\displaystyle r}$. Most measurements that can be made are relatively insensitive to the outer halo's mass distribution. This is a consequence of Newton's laws, which state that if the shape of the halo is spheroidal or elliptical there will be no net gravitational effect from halo mass a distance ${\displaystyle r}$ from the galactic center on an object that is closer to the galactic center than ${\displaystyle r}$. The only dynamical variable related to the extent of the halo that can be constrained is the escape velocity: the fastest-moving stellar objects still gravitationally bound to the Galaxy can give a lower bound on the mass profile of the outer edges of the dark halo.^[10]

The formation of stellar halos occurs naturally in a cold dark matter model of the universe in which the evolution of systems such as halos occurs from the bottom-up, meaning the large scale structure of galaxies is formed starting with small objects. Halos, which are composed of both baryonic and dark matter, form by merging with each other. Evidence suggests that the formation of galactic halos may also be due to the effects of increased gravity and the presence of primordial black holes.^[11] The gas from halo mergers goes toward the formation of the central galactic components, while stars and dark matter remain in the galactic halo.^[12]

On the other hand, the halo of the Milky Way Galaxy is thought to derive from the Gaia Sausage.

• Disc galaxy – Type of galactic form
• Galactic bulge – Tightly packed group of stars within a larger formation
• Galactic corona – Hot, ionised, gaseous component of a galactic halo
• Galactic coordinate system – Celestial coordinate system in spherical coordinates, with the Sun as its center
• Galaxy formation and evolution – Subfield of cosmology
• Spiral arm – Spiral-shaped regions of enhanced brightness within the galactic disc in spiral galaxies

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