The Role of Dark Matter in Galaxy Formation and Evolution

Tianyu Zhang

Dalian Mapleleaf International High School, Maqiaozi street, Dalian, China

Keywords: Dark Matter, Cosmology, Galaxy Formation.

Abstract: At the forefront of contemporary astrophysics, it is widely accepted that galaxy formation is directly attributed

to the gravitational pull of dark matter halos. As the universe ages, dark matter not only observes the inception

and growth of galaxies but also significantly impacts their evolutionary paths and morphological

transformations. This paper seeks to explore how these enigmatic substances act as cosmic architects, shaping

and propelling the galaxy formation process. Additionally, we will explore how dark matter orchestrates the

large-scale structural network of the universe, including the formation and evolution of galaxy clusters and

superclusters, highlighting its pivotal role in the grand scheme of the cosmos. Additionally, the article will

delve into the various approaches currently employed by the scientific community to detect dark matter and

develop its theoretical models. This ranges from direct detection experiments conducted in precise

laboratories to indirect detection utilizing astronomical observation techniques, including the gravitational

lensing effect.

1 INTRODUCTION

Dark matter is a mysterious form of matter in the

universe, whose existence and properties are essential

for understanding the structure, evolution, and

composition of the cosmos. It refers to a form of

matter that cannot be directly observed via

electromagnetic radiation, but its presence can be

inferred indirectly from its gravitational effects. In

long-term observations of celestial motions,

astronomers have discovered that the motion and

gravitational structures of many celestial bodies do

not adhere to existing gravitational models. Hence,

they postulate the existence of an invisible substance

pervasively distributed across numerous galaxies, star

clusters, and the broader universe, contributing to

gravitational forces and influencing the evolution of

cosmic structures across various scales. Its mass

significantly exceeds the total of all visible celestial

bodies in the universe. By integrating anisotropic

observations of cosmic microwave background

radiation with standard cosmological models, it is

determined that dark matter comprises 85% of the

universe's total mass and 26.8% of its total energy

(Ade, 2016). Currently, scientists continue to

investigate dark matter and its properties using

https://orcid.org/0009-0001-6353-2704

methods such as gravitational lensing and computer

simulations.

2 FUNDAMENTAL AND

PROPERTIES OF DARK

MATTER

Although the properties of dark matter remain poorly

understood, scientists continue to explore and study it

using various methods. Regarding the properties of

dark matter, since it cannot be directly observed, we

generally agree that it neither emits nor reflects light

and therefore cannot be observed through optical

means. This explains why there are no effective

methods to detect dark matter. Among the current

methods used to observe the universe, only

gravitational wave detection involves capturing

electromagnetic radiation. Fortunately, dark matter

possesses gravity, being one of the primary sources of

gravitational force in the universe, significantly

influencing the structure and dynamical behavior of

celestial systems like galaxies and galaxy clusters.

Additionally, dark matter has mass and therefore

inertia. Consequently, its presence can be indirectly

Zhang, T.

The Role of Dark Matter in Galaxy Formation and Evolution.

DOI: 10.5220/0013077700004601

Paper published under CC license (CC BY-NC-ND 4.0)

In Proceedings of the 1st International Conference on Innovations in Applied Mathematics, Physics and Astronomy (IAMPA 2024), pages 335-342

ISBN: 978-989-758-722-1

335

inferred through the observation of gravitational

lensing effects. Although the mass of individual dark

matter particles remains undetermined, this is due to

the uncertain particle properties of dark matter itself.

Dark matter is exceedingly stable and rarely

transforms into other forms, changing only under

extreme conditions such as during the universe's early

formation or its eventual contraction. Notably, in

addition to gravity, particle-type dark matter may

engage in weak interactions, but it largely lacks

participation in electromagnetic or strong

interactions. This restricts the interactions between

dark matter and visible matter, which may contribute

to the remarkable stability of dark matter itself.

Furthermore, the prevailing view within the scientific

community is that the velocity of dark matter

significantly exceeds the speed of light.

2.1 Evidence for Dark Matter from

Observational Studies

In 1922, astronomer Jacobs Kaptin first proposed the

concept of the possible existence of "dark matter",

who suggested that the motion of celestial systems

could indirectly infer the presence of unseen matter

surrounding the celestial bodies. Although dark

matter has not yet been directly detected, substantial

evidence indicates its widespread presence in the

universe, including from galaxy rotation curves and

dispersion velocity distributions. In 1933,

astrophysicist Fritz Zwicky employed spectral

redshifts to measure the velocities of galaxies within

the Coma Cluster relative to the cluster itself

(Zwicky, 1933). Observations of visible matter mass

distributions in spiral galaxies and calculations based

on the law of universal gravitation suggest that outer

celestial bodies should orbit the galaxy's center more

slowly than those near the center. However,

measurements of the rotation curves of numerous

spiral galaxies reveal that outer celestial bodies orbit

at velocities nearly equal to those of inner celestial

bodies, significantly higher than expected. This

implies the existence of massive unseen matter within

these galaxies. Using the potential force theorem, the

distribution of matter within a galaxy can be deduced

from the dispersion velocity distribution of its visible

celestial bodies.

There are currently three mainstream methods for

determining the mass distribution of galaxies or

galaxy clusters. (1) Analysis the motions of galaxies

or clusters using gravitational theory. In 1939,

astronomer Horace W. Babcock examined the spectra

of the Andromeda Nebula, revealing that the

rotational speeds of celestial bodies in the outermost

regions were significantly greater than those

predicted by Kepler's law, indicating a higher mass-

to-light ratio (Babcock, 1939). This implies the

presence of substantial dark matter within the galaxy.

(2) Observing the X-rays emitted by galaxy clusters.

Galaxy clusters commonly contain hot gases that emit

X-rays. Once these gases achieve hydrodynamic

equilibrium within the cluster's gravitational field,

they will emit different temperatures due to uneven

distribution of mass (3) The gravitational lensing

effect, a subtle prediction of general relativity,

demonstrates that the light from the back of a galaxy

cluster is bent as it passes through massive clusters.

By examining the extent and pattern of this light

bending, scientists can infer the distribution of matter

within the galaxy cluster, even though much of this

matter does not emit visible light.

At the cosmic scale, the total amount of dark

matter in the universe can be determined by precisely

measuring the anisotropy of cosmic microwave

background radiation. Observations reveal that

26.8% of the universe's total energy is attributed to

dark matter, compared to only 4.9% from traditional

matter comprising celestial bodies and interstellar

gases(Ade, 2016). Large-scale computer simulations

of cosmic evolution using n-body gravity modeling

highlight the critical importance of dark matter

particle properties for their aggregation behavior

(Melott, 1983). The simulations reveal that slow-

moving dark matter particles tend to clump together

more readily under gravity, thereby facilitating the

formation of large-scale structures (White, 1983).

Conversely, particles moving at high speeds, such as

neutrinos, tend to disrupt or smooth out these

structures due to their rapid motion (White, 1987),

and thus are not considered the primary candidates for

dark matter.

2.2 Theoretical Models of Dark Matter

Dark matter has been proposed since 1933, and

astrophysicists and particle physicists have raised

considerable possibilities for having models about

dark matter, such as the weakly interacting massive

particles, the Axion model, Graitino model, the

neutrino model, the sterile neutrino model and so on.

For the convenience of organization, based on their

inherent velocity dispersion and temperature

differences, different types of particle models are

classified into (1) cold dark matter, namely WIMPs

model, Axion model. (2) warm dark matter,

represented with sterile neutrino and Graitino models.

(3) hot dark matter, such as the neutrino which have

own mass.

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3 THE IMPACT OF DARK

MATTER ON GALAXY

FORMATION

In the modern physics cosmological model, dark

matter is crucial for galaxy formation and evolution.

Following decades of meticulous observations and

simulations, the dark matter model has been solidly

established. During the first second of the inflationary

epoch, fluctuations in matter distribution began to

influence gravity, leading to a gradual decrease in its

stability. Over time, the originally well-mixed dark

matter and gas separate due to the fluctuating gravity,

with the gas gradually descending toward the center

of the dark matter halo. Some dark matter halos are

so large that the gas can cool significantly at their

core, enabling the formation of stars and eventually a

proto-galaxy. As dark matter halos merge, the energy

dynamics within the galaxy influence the formation

of future stars.

3.1 Dark Matter Halos

Figure 1: Composite image (of the full TNG100-1 box) All

the gravitationally collapsed structures (in orange/white)

are surrounded by successive shock surfaces (blue) which

encode their formation histories.

Due to the fact that dark matter only participates in

interactions with gravity, it collapses and aggregates

to form large-scale structures resembling fibers

compared to other baryonic matter. We will transform

these elliptical spherical dark matter structures with

deep potential wells into dark matter halos.

3.2 Halo Mass Function and Its

Implications for Galaxy Formation

The halo mass function plays a pivotal role in

astrophysics and cosmology. Given a halo's redshift

and known mass, its density distribution can be

derived from its mass function (Jeremy, 2008).

Press-Schechter Formalism (PS theory) is one of

the earliest models used to describe the halo mass

function. Based on Gaussian random field theory, this

model considers the smoothed density perturbation

field as a Gaussian random field with a mean of 0 and

a variance of σ²(M), predicting the formation of dark

matter halos by identifying regions where the

perturbation exceeds the critical density δc.

Extended Press-Schechter Formalism (EPS

theory): An extension of the PS theory that

incorporates the merging history of halos, allowing

for a more precise description of the evolution of the

halo mass function.

Sheth-Tormen Formalism (TS theory): A

refinement of the PS theory that incorporates

additional parameters to more accurately align with

numerical simulation results.

As the seed of galaxy formation, the mass

distribution and abundance of dark matter halos

directly determine the rate and quantity of galaxy

formation. In the early universe, small mass dark

matter halos first formed and gradually merged to

form larger mass halos as the universe expanded and

evolved, triggering the formation of galaxies.

The halo mass function also regulates the

properties of galaxies by influencing internal physical

processes such as star formation, gas cooling,

feedback mechanisms, etc. For example, high mass

halos typically retain more gas for star formation,

while low mass halos may lose most of their gas due

to feedback, leading to a decrease in star formation

efficiency. By studying the halo mass function under

different redshifts, we can understand the evolution

of galaxies in different cosmic periods. For example,

as the universe expands and cools, the merging

activity of dark matter halos becomes more frequent,

and galaxies also undergo complex processes such as

mergers, interactions, and evolution.

3.3 Hierarchical Structure Formation

In the standard cold dark matter (Λ CDM)

cosmological model, the complex structures in the

universe are evolved from tiny quantum fluctuations

that gradually grow and evolve due to gravitational

forces during the period of cosmic inflation. This

The Role of Dark Matter in Galaxy Formation and Evolution

337

theoretical framework provides a theoretical basis for

the hierarchical growth of dark matter halos.

In the standard cold dark matter (ΛCDM)

cosmological model, the complex structures in the

universe are derived from tiny quantum fluctuations

that progressively grow and evolve through

gravitational forces during cosmic inflation. This

theoretical framework underpins the hierarchical

growth of dark matter halos. After the Big Bang, dark

matter was nearly evenly distributed throughout the

universe, albeit with minor density variations. These

slight density variations gradually coalesce under

gravitational influence, forming small dark matter

clumps known as the initial dark matter halos. As the

universe expands and cools, the density fluctuations

of dark matter halos intensify, transitioning into a

nonlinear growth phase.

During this phase, gravity predominates, leading

to the further collapse of less dense dark matter halos

into denser ones in response to fluctuations in density.

Small dark matter halos evolve into larger ones

through the merging and accretion of other halos or

dark matter particles, following a bottom-up

evolutionary model where lower-mass dark halos

form first and then coalesce into higher-mass ones.

Typically, smaller halos form and nest within larger

ones. This structure resembles the growth of trees,

with small branches evolving into larger ones. Within

this hierarchical structure, dark matter halos of

varying masses have distinct formation epochs and

evolutionary histories. Generally, lower-mass halos

form earlier while higher-mass ones form later.

This is attributed to the smaller density

fluctuations required for lower-mass halos, which

facilitate their formation in the early universe,

whereas higher-mass halos necessitate greater density

fluctuations and longer evolutionary periods.

3.3.1 Hierarchical Structure Formation’s

Impact on Galaxy Formation

As previously mentioned, dark matter halos create

gravitational potential wells for normal matter, such

as gas and dust, enabling their aggregation and

cooling, which in turn leads to the formation of stars

and galaxies. Without the gravitational influence of

dark matter halos, stable structures of normal matter

would be difficult to form in the universe.

The shape and distribution of dark matter halos

influence the morphology of galaxies. For instance,

an irregular or asymmetrically structured dark matter

halo could potentially stretch the galactic disk,

resulting in the distortion or deformation of the

galaxy's shape. Moreover, mergers of dark matter

halos can trigger interactions and collisions between

galaxies, thereby further impacting their morphology

and dynamical properties.

The hierarchical merging process of dark matter

halos significantly drives galaxy evolution. Through

merging and accretion, dark matter halos grow and

accumulate mass, thereby influencing star formation

rates, gas distribution, and the dynamical states within

galaxies. Additionally, the evolution of dark matter

halos interacts with feedback processes, such as

stellar winds and supernova explosions in galaxies,

collectively shaping the course of galaxy evolution.

On larger scales, the hierarchical merging of dark

matter halos also facilitates the formation of galaxy

clusters and supermassive galaxies. The merging and

interaction of multiple dark matter halos can create

large galaxy clusters comprising hundreds or even

thousands of galaxies. Within these clusters, galaxies

gravitationally interact and merge, further enhancing

galaxy formation and evolution.

3.4 The Formation of Clusters and

Super Clusters

As described in section 3.3.1, the existence of dark

matter allows star clusters to retain a stable structure.

While significant, the gravitational interactions

between visible matter, such as stars and gas, within

star clusters, are insufficient to fully maintain their

stability. The gravitational pull of dark matter

compensates for this deficiency, enabling star clusters

to preserve their shape and structure over extended

periods. Dark matter facilitates star formation through

gravitational dynamics. During the formation of star

clusters, dark matter accumulates in the central

regions, creating dense dark matter halos. The

gravitational pull of these halos accelerates the

collapse and cooling of nearby gas, which in turn

initiates the star formation process.

Just as in star clusters, the stability of super

clusters also relies on the gravitational pull of dark

matter. The gravitational interactions between

galaxies and galaxy clusters in super clusters, while

crucial, are insufficient to fully sustain their stability.

The gravitational influence of dark matter fills this

role, allowing super clusters to maintain their overall

shape and structure over long periods. Dark matter

further influences the evolutionary process of super

clusters. Using observational methods such as

gravitational lensing, scientists can deduce the

distribution and evolution of dark matter within super

clusters. These observational findings enhance our

understanding of the evolutionary history and future

trends of super clusters.

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4 DARK MATTER AND

GALACTIC EVOLUTION

Before the discovery of dark matter, it was commonly

assumed that all visible matter constituted the entire

mass of the universe; this misconception resulted in

substantial discrepancies between observed and

theoretical estimates of cosmic mass. Dark matter

constitutes an invisible yet massive component of

galaxies, with a mass significantly exceeding that of

visible matter like stars and gas. Consequently, a

higher proportion of dark matter directly increases the

total mass of the galaxy. The gravitational pull of dark

matter is one of the primary gravitational forces in

galaxies. As the proportion of dark matter rises, the

gravitational pull of galaxies intensifies significantly,

which in turn influences the motion and distribution

of matter within them.

As discussed in section 3.3.1, dark matter halos

serve as the structural framework for galaxy

formation and morphology. Thus, dark matter

stabilizes stars and gas within galaxies via its

gravitational pull, ensuring their sustained orbital

motion. In other words, a higher proportion of dark

matter leads to increased galaxy rotation speeds,

further enhancing their stability. Dark matter is more

uniformly distributed than ordinary matter, and a

greater proportion of it causes the galaxy's center of

gravity to be more aligned with the center of dark

matter distribution. This leads to alterations in the

galaxy's shape, resulting in a flatter and more

extended configuration. The growing proportion of

dark matter influences the distribution and movement

of gas and dust within galaxies. For instance, the

gravitational influence of dark matter may

concentrate gas and dust closer to the galaxy's center,

which in turn impacts the formation and evolution of

stars within these galaxies.

The galaxy rotation curve illustrates the

relationship between the velocities of stars and their

orbital distances within the galaxy. Normally, as one

moves farther from the galaxy's center, the velocity of

stars should decrease as the gravitational pull from

the center diminishes. However, observations reveal

that many galaxies' rotation curves do not conform to

this expectation, particularly in the outer regions

where the stellar rotational velocities do not

significantly decrease and even show an upward trend

in some cases. This phenomenon is referred to as

"rotation curve anomaly" or "high-velocity rotating

galaxies". The presence of dark matter offers a

plausible explanation for this phenomenon (Rubin,

1980). Since dark matter does not emit

electromagnetic radiation, it cannot be directly

observed, but it influences the stars and gas in

galaxies through gravitational forces. In the outer

regions of galaxies, where the mass of visible matter

is minimal, the mass of dark matter remains

substantial, exerting sufficient gravitational force to

sustain high stellar velocities, resulting in a flat or

even rising rotation curve, it is generally believed that

baryonic matter, which is difficult to detect, does

contribute to some of the dark matter effects, but

evidence suggests that it comprises only a small

fraction (Graff, 1996, Najita, 2000).

In galaxy clusters, the gravitational pull of dark

matter acts to counterbalance the centrifugal forces,

thereby maintaining their stability. Likewise, within

galaxies, the gravitational force of dark matter

supports their stability, preventing their disintegration

from the centrifugal motion of internal components.

Uneven distribution of dark matter creates

imbalances in the tidal force fields within galaxies.

However, it is this uneven tidal force field that, to

some extent, helps stabilize galaxy structures. It helps

prevent massive tidal disruption of galaxies when

disturbed by external forces, such as the gravitational

pull from neighboring galaxies.

4.1 Feedback Mechanisms

Two primary and frequently employed feedback

mechanisms in simulation analysis are supernova

feedback and ANG feedback Supernova feedback

primarily harnesses the immense energy and

materials expelled during supernova explosions.

These energies and materials heat and disperse the

adjacent baryonic gas, creating supernova winds.

These winds can subsequently influence the gas

distribution and star formation rate within the galaxy.

Additionally, supernova explosions can trigger

intergalactic gas flows and the formation of galaxy-

wide winds, thereby impacting the distribution of

baryonic matter on a larger scale. Active galactic

nuclei (AGNs), powered by supermassive black holes

at the centers of galaxies, are intense radiation

sources. AGNs heat, disperse, or expel the baryonic

matter within galaxies by emitting massive amounts

of energy in the form of jets and radiation (Risa,

2018) Similar to supernova feedback, this mechanism

profoundly influences the gas dynamics, star

formation rate, and morphology of galaxies. For

instance, the energy emitted by AGNs can inhibit star

formation in the central regions of galaxies while

promoting gas cooling and star formation in the outer

regions.

The Role of Dark Matter in Galaxy Formation and Evolution

339

5 OBSERVATIONS OF DARK

MATTER IN GALAXIES

Observations of dark matter within galaxies represent

a pivotal area of research in contemporary astronomy

and physics. Since dark matter neither emits

electromagnetic waves nor interacts strongly with

ordinary matter electromagnetically, it cannot be

directly observed using optical or electromagnetic

methods. Nevertheless, scientists have devised

multiple indirect methods for observing and detecting

dark matter, which are especially critical for

observations at the galaxy scale.

Scientists infer the presence of dark matter in

galaxies by observing how the rotational speed of

stars, gas, and other substances varies with distance

from the galaxy's center. Based on Newton's law of

gravity and dynamical theory, if a galaxy contained

only the mass of its visible matter, the rotational

speed of material distant from the center should

decrease. However, empirical observations reveal

that the rotation curves of many galaxies in the

universe remain flat beyond the central region,

suggesting the presence of additional mass,

specifically dark matter, as noted in section 4.

Another notable example is the gravitational

lensing effect. This phenomenon was predicted by

Albert Einstein's theory of general relativity and

independently confirmed by Arthur Eddington in

1919 through the observation of star displacements

during a total solar eclipse. As light from distant

galaxies passes through foreground galaxies or

clusters, it is bent by the gravity of the dark matter,

creating the gravitational lensing effect. Scientists

deduce the distribution and mass of dark matter in

galaxies or clusters by analyzing the bent light.

5.1 Simulations and Modeling

The numerical simulation of galaxy formation using

dark matter is an important field in cosmology, which

relies on complex computer simulations to

understand and predict the formation and evolution of

large-scale structures in the universe, such as

galaxies, galaxy clusters, etc.

Firstly, a theoretical framework for simulation

must be established based on general relativity and

cosmological principles. The standard cosmological

model (ΛCDM model) is typically employed as it

encompasses dark matter, dark energy, ordinary

matter, and radiation, enabling comprehensive

simulation across all scales. Simulations often begin

with observational data from cosmic microwave

background radiation shortly after the Big Bang,

which offer insights into the early state of the

universe.

Similarly, the initial amplitude and distribution of

density fluctuations, as described in section 3.3, are

among the key initial parameters for simulations. N-

body simulation is the most prevalent method among

scientists, where dark matter particles interact and

evolve into large-scale structures under the influence

of gravity. Besides N-body simulations, grid methods

are also utilized to simulate the dynamics of dark

matter and gases.

The simulation process involves extensive gravity

calculations, commonly employing the Fast Fourier

Transform (FFT) or tree-based algorithms, such as

the Barnes-Hut algorithm, to compute gravitational

interactions among particles. Another significant

factor influencing simulation outcomes is the

feedback among celestial bodies. Although dark

matter does not engage in interactions other than

gravity, the feedback effects of gas, stars, and black

holes in simulations, such as supernova explosions,

galaxy winds, and active galactic nuclei, can impact

the structure and evolution of dark matter halos.

After the simulation is completed, it is also

important to extract data from the simulation and

analyze information such as the formation time, mass,

morphology, and kinematic characteristics of the

galaxy. This work primarily facilitates the

comparison between simulation results and

observational data, such as galaxy redshift surveys

and cosmic microwave background radiation

observations, and verifies the model's accuracy. Some

individuals employ visualization tools to render

simulation results as images or animations, aiming to

provide a more intuitive understanding of galaxy

formation and evolution.

6 CHALLENGES AND OPEN

QUESTION

An an important concept in cosmology, dark matter is

currently facing a lot of problems and challenges in

many aspects.

6.1 Small-Scale Structure Problems and

the Missing Satellites Problem

After extensive numerical simulations, it was found

that dark matter forms numerous halos and

substructures in the universe. However, the number

of galaxies observed by scientists today is

significantly lower than that predicted by simulation

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results, a phenomenon known as the 'small-scale

problem'. Similarly, the Milky Way is expected to be

surrounded by a multitude of satellite galaxies.

However, the actual number of observed satellite

galaxies is markedly lower than theoretical

predictions, a discrepancy known as the 'missing

satellite problem'.

6.2 The Impact of Baryonic Physics on

Dark Matter Distribution

At scales less than 1h-1Mpc (million parsecs),

baryonic processes significantly influence the

clustering of dark matter. This influence is especially

pronounced at smaller scales, like 0.1h-1Mpc, where

gas adiabatic processes can substantially boost dark

matter clustering. Moreover, baryonic processes

including radiative cooling, star formation, and

dynamical supernova feedback in the universe can

modify the mass distribution of dark matter halos,

particularly under the influence of active galactic

nucleus feedback mechanisms, which amplify this

effect. For instance, the feedback from active galactic

nuclei discussed in 4.1 might inhibit the formation of

massive dark matter halos. Theoretically, baryonic

matter also influences the morphology of dark matter

halos. As the universe evolves, the spatial

morphology of dark matter halos transitions gradually

from flat to rounded. The presence of baryonic matter

hastens this transformation, further rounding the

shapes of dark matter halos. However, feedback from

active galactic nuclei can mitigate this acceleration.

7 PLANNED TASKS AND

EXPECTATIONS FOR THE

FUTURE

The Large Synoptic Survey Telescope (LSST) is a

planned ground-based telescope designed for deep

and wide-field continuous observations of the sky,

aimed at unveiling the large-scale structure of the

universe, the nature of dark matter and dark energy,

and the behavior of transient celestial objects. LSST

will feature an unprecedented wide field of view,

enabling it to cover extensive regions of the sky.

Additionally, by utilizing its high sensitivity to

observe extremely faint celestial objects, LSST will

reveal deeper mysteries of the universe. In terms of

its mission, LSST is designed to perform long-term

continuous observations to capture the dynamic

changes in celestial bodies. (2) The James Webb

Space Telescope (JWST), a next-generation

spacecraft developed by NASA and space agencies in

other countries, was successfully launched in 2021. It

has now superseded the Hubble Telescope as a

pivotal tool for exploring the universe's depths. JWST

is outfitted with state-of-the-art instruments like

NIRCam and MIRI, which facilitate advanced

spectral and imaging analyses.

In the future, it is necessary to continue to

improve the sensitivity and accuracy of direct and

indirect detection techniques for dark matter particles,

in order to obtain more direct evidence about dark

matter.

Based on new observational data and

experimental results, continuously improve and

revise existing dark matter theoretical models to

better explain dark matter phenomena in the universe.

8 CONCLUSIONS

In general, dark matter plays an indispensable role in

the formation and evolution of galaxies. Dark matter,

in its high-density form, generates substantial

gravitational forces that attract adjacent matter,

including visible substances like gas and dust. These

gravitational forces cause surrounding matter to

gradually accumulate, forming primitive nebulae that

evolve into celestial entities such as stars and

galaxies. Additionally, because dark matter does not

interact with electromagnetic radiation, its

distribution is uniformly spread across vast spatial

scales. This distribution pattern ensures that galaxies

experience consistent gravitational forces during their

formation, leading to relatively regular and

symmetrical structures. The gravitational influence of

dark matter not only fosters the formation of galaxies

but also sustains their stability. Its presence allows the

internal matter within galaxies to maintain a relatively

stable state of motion, preventing excessive

contraction or disintegration due to internal

gravitational forces. In larger-scale systems such as

galaxy clusters, the gravitational influence of dark

matter also facilitates interactions and mergers among

galaxies. These processes profoundly influence the

formation and evolution of galaxy clusters.

Through the study of dark matter, we can deepen

our understanding of the universe's structure and

evolution. This avenue of research also advances the

fields of fundamental and particle physics, unveiling

novel physical phenomena and laws. In summary, the

exploration of dark matter and its halos represents a

pivotal area of development in astrophysics.

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341

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